text:
A preliminary exploration of the influence of Greek philosophy on early childhood education: An application In Hong Kong
Grace LAU, Kwok Keung HO
Department of Early Childhood Education (ECE)
The twentieth century saw great hopes but also great failures. Philosophy, however, by its timeless truth, might confront the ever changing fashion by giving people a pointer through its philosophical application in the realm of education. In this paper, the authors argue that many philosophical teachings from the famous Greek philosophers are indeed influential when their teachings are applied to the early childhood classrooms in Hong Kong. Their sphere of influence has extended from the British colonial period to the present era in Hong Kong as far as early childhood education is concerned. For Plato, his theory of Forms and his emphasis on the search of Truth will be compared with Aristotle empiricist views in his study of nature. While analyzing the theory of Forms and the idea of the Good, the authors found that Plato's approach could be traced back to Xenophanes who proposed a monotheistic theory of God and is religiously related to Christianity. Their applications in the top-down teacher-directed play-based curriculum were valid in the early childhood educational mode during the early colonial period to the 1980s in Hong Kong. Since Aristotle was found to have a different approach to Forms as compared to those of Plato, Aristotle's argument for Forms was mentioned and its relevancy to the prevalent hybrid mode of the play-work-based curriculum in early childhood education is explored. Following the most recent reform in early childhood education in Hong Kong, free play is recommended in the reform document. Heraclitus's doctrine of 'flux' could apply most suitably in the free play condition as 'flux' signifies an ever changing condition just as the nature of free play does. A final touch of this paper is on exploring the divergent views of Plato and Aristotle and their impacts on education today so as to provoke further thoughts of the readers in the areas explored. Copyright © 2017, Grace LAU & Kwok Keung HO.
Hellenic Journal of Research in Education
https://doi.org/10.12681/hjre.10886
Lau, G., & Ho, K. K. (2017). A preliminary exploration of the influence of Greek philosophy on early childhood education: An application In Hong Kong. Hellenic Journal of Research in Education, 6(1), 73-94.
10.12681/hjre.10886
Fingerprint Dive into the research topics of 'A preliminary exploration of the influence of Greek philosophy on early childhood education: An application In Hong Kong'. Together they form a unique fingerprint.
Early childhood Education Arts & Humanities
Greek philosophy Arts & Humanities
Hong Kong Arts & Humanities
Aristotle Arts & Humanities
Plato Arts & Humanities
Early childhood Arts & Humanities
Colonial Period Arts & Humanities
Curriculum Arts & Humanities


Yes, uniGUI Voyager is here. Actually, it has been here for a while!
Voyager is the nickname for uniGUI version 1.50. It contains exciting new features which were announced in uniGUI roadmap back in 2017. One of those features is uniGUI HyperServer which primarily targets to radically improve availability, stability, and scalability of uniGUI applications. It also introduces other important features such as allowing to update applications remotely without a need to stop the application server. Another exciting improvement is porting to uniGUI to the latest Ext JS version 6.x.
uniGUI HyperServer is a new server archirecture designed to highly improve uniGUI applications' availability, stability and specifically scalability. This goal is achieved by applying industry's known and widely used techniques such as load balancing and process recycling.
A traditional uniGUI application server consists of one single process and multiple threads. The single process can be a uniGUI executable or an ISAPI or Apache worker process. In all cases all sessions reside inside a single process and several threads in same process are used to handle incoming requests.
uniGUI HyperServer changes above model and turns into a multi-process multi-threaded model. In this new model several worker processes are spawned to serve same web application. Sessions will be divided among worker processes and based on the configuration you may have multiple worker processes for same uniGUI application. Worker processes are managed and orchestrated by another process which is actually the HyperServer itself. The HyperServer will be the main entry point for all incoming requests. HyperServer will take all requests and distribute them among worker processes. HyperServer has also the responsibility to spawn new worker processes when needed and recycle them as soon as they are purged. Since uniGUI sessions are stateful, another important duty of HyperServer is to direct incoming session requests to the correct worker process which has created that particular session. In HyperServer terminology each worker process is called a Node.
uniGUI Voyager integrates the latest version of Ext JS 6.x. It was another revolutionary change for uniGUI. The previous version of Ext JS used in uniGUI was Ext JS 4.4.2 which was quite outdated. With upgrading Ext JS to 6.x now uniGUI can take benefit from all new enhancements and features of Ext JS 6. Here you can read a blog published in Sencha's web site which explains our journey of upgrading Ext JS in uniGUI Voyager.
It was almost seven years ago since my first blog posted in this site. Yes, uniGUI has been in beta stage for seven years. It may look like a long time. Indeed, it is a long time for a beta period. We can mention several reasons for this.
The most important reason is that uniGUI initially started as a product for both VCL and web platforms. Many of you may still remember this feature. It allowed developers to create both VCL and web applications using a single source base. However, after a while, we realized that it is too hard to keep the same level of quality and richness for VCL. The Ext JS framework was growing steadily, adding new features with each new edition, and many of those features were difficult to implement for VCL. In time, the VCL part of the framework turned into an outdated and incomplete version of the web interface. This fact was unacceptable, and we decided to drop support for VCL and continue with a web-only framework. Our decision was supported by the majority of our community, and after that, we left the VCL mode behind and accelerated web only development. This was the first major architectural change in uniGUI framework.
Another major architectural change happened because we were not happy with the component hierarchy built in the initial versions of uniGUI. It was complicated and difficult to maintain. In the new architecture, the design-time code and the run-time code are fully separated. Also, the run-time code was divided into two libraries named Core and Components. The component hierarchy was also recreated and reorganized. This architecture of uniGUI is still used today. Obviously, we were not in a rush to release version 1.00. uniGUI was developed in the form of a community project, with quality and stability as the highest priority. Of course, uniGUI could not be free because from the first day it was intended to become a commercial product. The included Ext JS library is also a commercial product which can not be deployed without an OEM license. In the year 2014, we started selling uniGUI Beta licenses. The main reason for this was that uniGUI could not continue distributing fully functional beta builds without including an OEM Ext JS license, so it became inevitable to make an OEM agreement with Sencha Inc. After that date, all uniGUI beta builds could only be obtained by purchasing a beta license from us.
According to our community our beta builds were stable enough to be used in production. Indeed many developers are using uniGUI in production for many years. Again, we decided to continue in beta mode until we are fully confident that uniGUI can be labeled as version 1.00. Fortunately we are happy to announce that uniGUI has finally came out of beta mode. Yes, eventually we have removed the phrase beta and build 1404 is our first official non-beta build. From our point of view build 1404 is just yet another build in or long chain of builds. We are aware of all imperfections and lackings. Documentation is still not complete and component reference manual must be finished. Our highest priority is documents for now and with each new build we will continue improving uniGUI documents.
By ending the beta phase, we can say that a new era started for uniGUI. There is still much to do. Among the high priority tasks, we can count porting uniGUI to Ext JS 6.5, implementing our load balancing server and adding support for the Linux operating system. We will be busy with these tasks and continue improving uniGUI. At this point, let me express my sincere gratitude to all developers who have supported us during the beta stage by buying beta licenses. uniGUI could not thrive without your support.
We are glad to announce that version 0.99.95 is available for all uniGUI editions. Trial edition can be downloaded from download section.
This version includes many fixes and new features. Most probably it is the last version right before version 1.00RC which will be announced soon. Thanks to all developers around the world by supporting us especially those who have ordered a license.
Starting from this edition we have renamed project group file names to avoid confusion. In previous versions project groups were named with a number representing Delphi version. For example, uniGUI2011Group was name of project group for Delphi XE. In this new version we have renamed it to uniGUI_XE_StdGroup, so respected project group can be easily spotted.
[UNG-1777] - CoInitialize is not called properly.
[UNG-1765] - JS error when uniDBGrid LoadMask is not enabled.
- 0002325: In Combo controls EmptyText is not published.
- 0002324: Bug when UniDataTimePicker is editor in DBGrid.
- 0002323: UniDBGrid: Filter doesn't work correctly after clear button.
- 0002322: UniDBLookupCombo: Component is not reset when filter is cleared.
- 0002321: UniImageList/UniNativeImageList: New UseGlobalCache property.
- 0002320: UniImageList/UniNativeImageList: Draw method implemented.
- 0002319: Issue when CoInitialize is called after ServerModule is inited.
- 0002078: Use global cache for ImageLists and other objects where possible.
- 0002313: Bug in uniNativeImage list GetPng and GetBitmap methods.
- 0002312: Recent issue in uniDBGrid which prevents mobile grids from working properly.
- 0002311: Delphi 10.1 Berlin support.
- 0002310: ShowMessage issue when active form is a LoginForm.
- 0002307: DateTimePicker: Can't set time @runtime when Kind = tUniTime.
- 0002302: OnColumnFilter event must return KeyValue when Filter is a DBLookupCombo.
- 0002301: Columns[n].Filtering.VarValue must return KeyValue when filter is a DBLookupCombo.
- 0002300: UniDBLookupCombo: Style property is published.
- 0002298: UniComboBox: New AnyMatch property.
- 0002295: Grid column Filter doesn't resize with the column.
- 0002294: Bug when UniContainerPanel is Mask target.
- 0002293: Issue when UniDBLookupCombo is a grid editor and field is a Lookup field.
Finally our new site is online! It adopts a modern responsive design which makes it compatible will all desktop and mobile browsers. We will continue improving the layout and adding more content to uniGUI website.


text:
Q: blending composites..some explanation please I am trying to figure out what Romain Guy did in his blend composite BlendingComposite--Romain Guy. This is what I know at least I think.

*

*Image holds its information in an array of colors (info for each pixel)

*Blending takes those pixels and combines them using algorithm to create a final pixel.

I am confused how to get the pixels arrays of those images and then work with them?
How is the blending composite then created?
Thank you for your help and time.

A: Here is the specification describing how to implement the PDF blend modes, which is what are described on the linked page.

redpajama_set_name: RedPajamaStackExchange


text:
September 12, 2018 / 1:35 AM / 10 months ago
Tennis: Serena 'out of line' but both sides share blame says King
(Reuters) - Former world number one Billie Jean King has softened her initial stance on the controversy over Serena Williams, who was "totally out of line" when she vehemently disputed calls by chair umpire Carlos Ramos during Saturday's U.S. Open final.
FILE PHOTO: Serena Williams of the USA argues with chair umpire Carlos Ramos (not pictured) while playing Naomi Osaka of Japan in the womenís final on day thirteen of the 2018 U.S. Open tennis tournament at USTA Billie Jean King National Tennis Center in New York, NY, U.S., September 8, 2018. Mandatory Credit: Robert Deutsch-USA TODAY Sports/File Photo
Ramos, however, could have prevented the affair had he communicated better and given Williams a 'soft warning' instead of a code violation when he saw her coach Patrick Mouratoglou giving signals during the match, King said.
Williams was issued a warning, point and then game penalty after she argued with Ramos during the final, which was won 6-2 6-4 by Japan's Naomi Osaka.
"Serena was out of line. There's no question," King told CNN on Tuesday. "No one is saying she was a good sport. If they are they are crazy.
"She was totally out of line. She knows it."
King's remarks to CNN were something of a walk back of her earlier comments when she said in a Washington Post editorial that Williams had faced down sexism with her protests.
She also did not criticise Williams' on-court behaviour.
King, however, said Williams was not aware she had been handed a first violation and was surprised to have a point taken from her when she received a second for later smashing her racquet.
The loss of the point prompted Williams to call Ramos a "thief", which led to a third violation for verbal abuse that resulted in the umpire issuing a game penalty, although he could have prevented the incident from escalating, King said.
"The point is he (aggravated) the situation. 'I'm not attacking your character,' is the most important thing he could have said," King told CNN.
"I think everything would have been different."
King said she hoped the incident would bring about needed changes to the sport, including allowing for direct communication between the umpire and the fans over a loudspeaker and ending the ban on coaching during Grand Slam matches.
"Crisis creates an opportunity to get it right," she said.
Reporting by Rory Carroll; Editing by Greg Stutchbury

redpajama_set_name: RedPajamaCommonCrawl


text:
Election petition: NDC will continue to protest against EC
Date: Dec - 30 - 2020 , 12:04
BY: www.graphic.com
The National Democratic Congress (NDC), says it will not stop organising protests against the Electoral Commission (EC) despite petitioning the Supreme Court.
According to presidential candidate for the party in the just ended polls, John Dramani Mahama the party will use protests to "demand the enforcement of the rule of law and protection of life and property of the good people of Ghana.".
Mr Mahama made is known via his social media handles on Wednesday 30, 2020.
He stressed that going to the court does not prohibit the party from organising protests against the declared results.
"The National Democratic Congress has decided to proceed to the Supreme Court to contest the results of the rigged elections of December 7. The decision follows a meeting of the National Executive Committee (NEC) of our party on Tuesday in Accra."
"While in court, the NDC will continue all legitimate actions, including protests, to demand the enforcement of the rule of law and protection of life and property of the good people of Ghana.", he said.
National Democratic Congress (NDC) , topstory, Electoral Commission (EC) , #Election2020


The Sony CyberShot DSC-L1 packs a 4.1-megapixel imager, 3X-optical zoom lens into a stylish little package just smaller than a candy bar. Measuring just 3.7" x 1.7" x 1.1" (95 x 44.3 x 25.7mm), the L1 is powered by a InfoLithium battery pack, and features Sony's Real Imaging Processor circuitry, delivering outstanding shot-to-shot speed, stamina and quick start-up time for catching the action when it happens.
Its Carl Zeiss Vario-Tessar 3X optical zoom lens, sets the stage for picture quality typically delivered by larger, more expensive digital cameras. For the first time in Sony's ultra-compact class of digital cameras, the Cyber-shot L1 employs a 1.5-inch transflective LCD, making it easier to see what's on the LCD even in bright sunlight.
When used with Memory Stick PRO Duo media, the L1's high-quality MPEG Movie VX Fine mode captures and plays back high-resolution full-motion videos with 640x480 pixel resolution at 30 frames per second. The length is limited only by the capacity of the memory card being used.
Like most of Sony's Cyber-shot cameras, the DSC-L1 model has speedy auto-focus and auto-exposure options to snap the best picture the first time. You can quickly select the best setting based on the shooting conditions by choosing from one of seven preset modes, including twilight, snow, beach and candle.
The DSC-L1 also features four newly developed technologies - including a linear focus drive and a compact high-resolution optical system - that combine to produce its ultra-small 3x optical lens. This lets you zoom in for crisp images of a flower or zoom out for a far-away shot of the game-winning goal, all the while staying in sharp focus.
The included InfoLithium battery provides for approximately 240 shots per charge with a to-the-minute, on-screen display of remaining battery life.
The silver DSC-L1 will be available in mid-October (2004), and the blue, black and red models will follow in January (2005), each for about $300.
The Cyber-shot L1 and a CD for size comparison.
The playing card deck-size Canon S410 Digital Elph and the diminutive DSC-L1.
The credit card-size Casio EX-Z40 and the diminutive DSC-L1.


I have just completed moving JBlog to a new host. After my last post my old host kept going down and the MySQL server didn't get much better. So I packed up and moved here to a new host at www.profusehost.net which offers 1gb of storage… w00t and all that for the small price of putting some ad code on your site. And since I had some adsense on my site which I decided wasn't worth it in the end. Hosting for the price of having the ads is worth it so there you go.
Hopefully from now on I can blog more and not worry about the database being down less. For those syndicating or coming from bookmarks you might want to update them since I have no idea how long it will be till my old host shuts down the service.


Canon EOS M10 X Rilakkuma | Do more with your #ToyTravel!
Are you part of the Nui-Dori trend? I do see some of my friends who travel alone, accompanied with their toy! ToyTravel is a trending way to travel, and Canon is partnering with the much-loved Rilakkuma! It inspire creativity among social media users and avid, big fans of travelers and photographers alike. Interestingly, you can now have Rilakkuma as your next travelling companion with Canon's special edition EOS M10 box set, bundled with a limited edition 24cm Rilakkuma plush toy! Like the one I have (ok, maybe mine is slightly bigger! Took it at event...)!
The Canon EOS M10 X Rilakkuma is your next big travel buddy!
So if you might be interested to know what exactly is ToyTravel, it is the art of photography where toys imitate life. It's common for social media users to inject creativity and fun into their everyday adventures with a preferred animated object – from a figurine in a bowl of cereal, to a stuffed toy strapped into an airline seat; the possibilities are endless. Now with the Canon EOS M10, they are empowered to share stories of their travels and adventures through high quality photos.
Combining Rilakkuma, a popular character, with Canon EOS M10, the lightest camera in the compact series, we hope to bring ToyTravel to every fun-loving social media user and photographer out there and make their next travel adventure a more memorable one. With the sleek and chic EOS M10, users will be able to capture superior quality photos and videos for sharing on social media platforms.
The all-new Canon EOS M10 X Rilakkuma!
Credit to Anis for taking this shot for me!
The EOS M10 is the newest addition to Canon's EOS M range of high performance mirrorless interchangeable-lens cameras. As the most compact and lightweight in the series, EOS M10 is the perfect camera to bring along on all types of adventures! With its large 18.0-megapixel APS-C sensor and fast Hybrid CMOS AF II system, users can now capture excellent quality photos of spontaneous moments with no more missed opportunities.
Macam jumpa kawan lama! LOL!
Designed for perfect selfies, the Self Portrait mode features a one-touch beautification shortcut that offers a skin smoothing effect. Its Wi-Fi feature also allows seamless sharing on multiple social media platforms. With optional jackets (sold separately) in a range of striking colours such as classic Navy, a sweet hue of Pink, whimsical Aqua and monochrome Border, you can now style and customise the camera according to your personalities.
Oh well, you can see we are such a FUN bunch of bloggers!
Rilakkuma appeared at the launch! So cute!
One final shot with Rilakkuma!
Jom pergi holiday and lepak dengan Rilakkuma! Need to get more shots with the new Canon EOS M10!
And here's some TVC for you to see how cute is Rilakkuma and why you should get it as your travel buddy!
So yes, if you are keen, better get the limited version box set FAST!
There will be a total of three themes for this contest and you will have one month to capture the perfect ToyTravel photo for each theme.
Deadline extended to 8th July!
#ToyTravel Challenge 2 theme released! Chillout Activity is the theme!
The first theme was announced on 6th of June and the first winner will be revealed at the end of the month. For more details, please visit this site. *Promo valid for a limited time only. Availability differs according to your country so check out your local retail outlet for more information! T&C here.


The Leet World (forum) needs you!
As we've been saying, the release of our site and first episode approaches, and as such, we are attempting to to put together something of a community for the people that stumble into our path. For those of you who are checking up on the process of the show, feel free to head on over to The Leet World Forum, and help us test everything as we get ready. Register, start some topics, interact with us, and that way we'll have the board somewhat populated in anticipation of the release.
Also, stay tuned, since tomorrow we'll be announcing the date that our first episode launches.
This entry was posted in Maintenance, News and tagged forum, the leet world, TheLeetWorld on August 2, 2007 by Eddy.


text:
Artie Lange new interview
Q. What is your gut feeling on whether Howard will re-sign with Sirius/XM?
A. You know, honestly, everybody thinks that we all have inside information. I really don't. I don't think Howard even knows now. I'm pretty positive negotiations haven't started. My gut feeling is, if he does come back, there will be an amendment in the schedule, in some way, shape or form. But I don't know anything at all about that.
Q. Does your second book have a title, or a tentative release date yet?
A. The tentative title is "College Is For Losers," which is a quote my father said to me. No release date: We're hopin' for the Fall.
Categories Stern Tags Artie Lange, Enough Money, Gig, Gut Feeling, Howard Stern, Howard Stern Show, Longshoreman, Losers, Mad Tv, Negotiations, Radio, Release Date, Resume, Shape, Show Business, Sirius, Tentative Release, Tentative Title, Waiter 1 Comment
Eric The Midget ready to sue Gary Baba Booey
Howard said he had Eric on the line and said that he must be retarded. Howard said that he has figured it out because Eric called Gary up in the office yesterday and he was threatening him. He said Eric wants to sue Gary. He said he got an email from Robert Mills and another guy from the head of TNA Wrestling. Eric said he's not the head of TNA. Howard said it's obvious that they're letters from fans and they're not the real people.
Categories News & Politics Tags Address Email, Baba Booey, Different Companies, Elf, Email Address, Eric, Ingrate, Lawyer, Lot, Midget, Money, Plays, Real People, Shape, Shit, Tna, Wrestling Leave a comment
Howard Stern – Medicated Pete Dating Game video
September 19, 2016 December 1, 2009 by Admin
Howard got to the Medicated Pete dating game. He said that they have Medicated Pete coming in to meet 3 girls who were already set up in the studio. Howard had Pete come in after that. He was looking down at the floor and not at the girls. Pete eventually looked at them and asked what was up. Howard said that Pete has Tourettes and he was having a hard time today.
Categories Stern Tags 3 Girls, Ataxia, Balance Problems, Bar Howard, Cool Guy, Dating Game, Dependant, Fringe, Girls, Happy Hour, Hard Time, howard, Howard Stern, Jeans, Lila, medicated, Meet Girls, pete, Shape, Shell, Stern Howard, Time Today, Vegan, Wheelchair Leave a comment


text:
Long on Color
In 1871, Samuel P. Long penned "Essay VII, Color" in his book Art: Its Laws and the Reason for Them, Collected, Considered, and Arranged for General and Educational Purposes. Granted, it is a very long title, but an important book on art for the general public that time. Interestingly, Mr. Long, who was a Counsellor at Law in the United States, had been a student of Gilbert Stuart Newton at the British Royal Academy in the early 1800s. Stuart's mother, in turn, was the daughter of American portrait artist, Gilbert Stuart. Our distinguished Counsellor, himself, was a landscape painter and exhibited at The Pennsylvania Academy of the Fine Arts and the Boston Athenaeum. During this time and into the last quarter of the 19th century, the academies taught only representational art, no Impressionism (although it is representational) or Abstract art (nonrepresentational). An artist's hope of success lay almost entirely on acceptance at the salons. Strictly regimented, with a lengthy course of study combined with rules on linear perspective, the handling of light, colors to be employed, the subject matter, and how the paint was to be applied and with what brushes, strict academic training fell out of favor by the end of the 19th century. This manner of painting was considered to be not only a creative endeavor, but an intellectual one, in sharp contrast to the emotionalism of much of the 20th century "modern art", the primary basis of which is deconstruction of form and the use of unrealistic distorted compositions and colors. Long wrote his book near the tail end of the long reign of the academies and his essays insight to the thinking of 19th century artists in flux.
Long refers to the "mysteries" of color and the mysterious effects of light and dark (chiaroscuro) in a painting. Chiaroscuro creates space and body and the proper application of light and dark in a painting allows subject to be detached from the background to advance and recede—in other words it provides dimension. Regarding color, Long states that "although most enchanting, it is for the general purposes of imitation, the least essential of the component parts of painting". In his mind, the most important foundation elements of a fine studio painting were invention, composition, design/drawing, chiaroscuro and lastly, color. Invention was that process by which the artist composed a "story" or theme from his mind, not from an actual scene or subject. The source could be from poetry, history, mythology, religion or simply the mental invention of the artist. Composition is another "mental operation" that consisted of the artist making "picturesque arrangements to please the eye" and most importantly "preserving a correspondence between the material employed and the sentiment of the subject". To preserve or capture the sentiment of the subject one would think that color would be very important; however, Long forges ahead with what he considers the foundation of a painting—the drawing, stating that "color apart from outline is only an unmeaning glare". The technique of chiaroscuro was used to "render the surface of a picture "agreeable" to the eye by dividing it into masses of light and dark and "to assist sentiment and give expression". The lights and darks of a painting, in his words, "should be so arranged as to assist sentiment and be an echo to the sense". Tenebrism, a related painting technique, which Long may have lumped in with chiaroscuro, is a more dramatic version using a stream of light to cut through the darkness and emphasize the subject.
Color, is important in both chiaroscuro and tenebrism because of the application of high- and low-key colors used to create the effects. Long did recognize this and the other attributes of color in his Essay VII. He states that color gives reality to a subject and that the "beauty of the atmosphere, the morning dawn, evening splendor; the tender freshness of spring, the fervid vivacity of summer and the mellow abundance of autumn" is almost entirely dependent on color. He recognized that color heightens joy, inflames anger, and deepens sadness--important expressive concepts to modern nonrepresentational artists. Color was important to the early- to mid-nineteenth century artists in a different way than to the late 19th century and early 20th century artists. As artists began breaking rules of academic art to explore new dimensions in painting techniques, visualization, and color theory, the expression/emotion of the artist and the process and action of applying paint became more important than the realistic portrayal of subjects in their proper form, perspective and color. Just as now, color to Long and other artists of his time, was "used to characterize the various qualities, textures, and surfaces of bodies in all their various situations of light, shadow and reflection". To varying degrees, shadow and reflection have been significantly reduced in importance in nonrepresentational art where the perspective of depth is often absent, and color is used more for texture and visual impact.
Long was not an advocate of the academic "high finish" of the generation of painters that preceded him. Too much blending of the colors, a hallmark of this manner of painting, resulted in a highly polished finish that was passé at the time Long wrote his essays. He was an advocate of impasto (thick paint application with visible strokes) because it provided "brilliancy" and also texture, which were very important to the Impressionists and later artists, but also to some of the earlier Renaissance painters. He made the association between color and detail, essentially saying to apply only the colors necessary to provide the overall appearance and avoid the minutia of exacting detail; it is the eye that processes juxtaposed colors that "echo the sense" of the subject. We cannot say whether Long approved of the Impressionist style of painting; however, I think expressionism might have offended his "senses". It would be quite instructive to us if we could examine paintings by Long in order to assess his command of the "mysteries of color."
Back to Highlights


Welcome Guest. Please register or log in now. There are 11 people online (0 Friends).
The Cooler Master Choiix Power Fort Advanced combines a few unique features into the standard portable power source for electronic devices.
It seems that diversity is the name of the game in these times. Cooler Master was always a brand that made enthusiast computer parts. Everything from cases to cooling was Cooler Master's domain. Choiix is Cooler Master's chic mobile brand name and with that comes all new types of products including general consumer electronic ones. The Choiix Power Fort Advanced promises to keep your portable electronic devices charged up while you're on the go away from AC power.
The Choiix brand of packaging is clear with orange and white coloring. Having a clear package allows you to see what the product looks like on the shelf. The Power Fort itself sits neatly in the center. The sticker is interesting. It is promoting "world class safety" as one of the buying points. We guess that if you are stuck in your car without power in your phone, this can help you out of a bind.
The back of the box contains the various recharge amounts you should get using the Power Fort. It also mentions that the Power Fort has a built-in flashlight.


It may be possible to teach machines how to pick out features in neurons and other cells that have not been stained or undergone other damaging treatments, according to a new study.
said Margaret Sutherland, Ph.D., program director at the National Institute of Neurological Disorders and Stroke (NINDS), which partially funded the work.
A dish, or culture, of neuronal cells appears uniform to the naked eye and the different, individual cells in it cannot be seen. Ever since the late nineteenth century when pioneering neuroscientists, Santiago Ramon y Cajal and Camillo Golgi, drew the earliest maps of the nervous system, scientists have been developing dyes and staining methods to help distinguish the structures in the brain, including different types of cells and their state of health.
However, many of these methods involve harsh chemicals that fix, or freeze, cells in an unnatural state or damage living cells after multiple stains have been applied. The traditional techniques also limit the details scientists can observe.
A team led by Steven Finkbeiner, M.D., Ph.D., director and senior investigator at the Gladstone Institutes in San Francisco, and professor of neurology and physiology at the University of California, San Francisco, explored whether computers could be trained to identify structures in unstained cells.
said Dr. Finkbeiner, the senior author of the study.
The researchers used a method called Deep Learning, which relies on principles of machine learning, a type of artificial intelligence in which machines can learn from data and make decisions. Facial recognition software is an example of machine learning.
Using Deep Learning, Dr. Finkbeiner's team trained a computer program to analyze brain cells by showing it stained and unstained images. Then, to test whether the program had learned anything, the researchers challenged it with new unlabeled images.
After the first round of training, the program identified where cells were located in the culture dish by learning to spot a cell's nucleus, a round structure that contains genetic information and serves as the cell's command center.
During additional experiments, Dr. Finkbeiner's group increased the complexity of the features the program was looking for and successfully trained it to distinguish dead cells from living cells, as well as to identify specific types of brain cells.
In addition, the program learned to differentiate between axons and dendrites, which are two specific types of extensions on neurons. According to the results, the program was successful in predicting structures in unlabeled tissue.
The researchers call this computational machine-learning approach "in silico labeling".
Dr. Finkbeiner and his team noted that the main drawback to using this technology is that the training datasets need to be very large, ideally around 15,000 images. In addition, there may be a risk to overtraining the programs, that they become so specialized they can only identify structures in a particular set of images or in images generated in a particular way, and not make predictions about more general images, which could limit the use of this technology.
Dr. Finkbeiner and his colleagues plan to apply these methods to disease-focused research.
More research is needed to refine the technology and make it more widely available.
Christiansen, Eric M. et al.


Named for his father, the venture is actually Stulman's second food-store foray; he considers the first, Market Table, "a failure in execution." For round two, he's recruited his manager from D'Artagnan, sourced produce from friends' farms and Brooklyn Grange, installed a granola-parfait station, and will sell Stumptown coffee to go for a very neighborly buck a cup. In back, an all-day menu features raw-bar selections, American cheeses and craft beers, meal-size salads, and such iconic sandwiches as the lobster roll and a roast pork with broccoli rabe and provolone. And in a month or so, Stulman plans to launch online delivery tailored to everything from game-day feasts to spontaneous Sunday brunch. Check out the menus below, and take a peek inside the space in our slideshow.


text:
Označení USS John Paul Jones nesla v historii amerického námořnictva dvě plavidla:

 USS John Paul Jones (DD-932) – torpédoborec třídy Forrest Sherman (1956 – 1982)
 USS John Paul Jones (DDG-53) – torpédoborec třídy Arleigh Burke (1993 – aktivní)

redpajama_set_name: RedPajamaWikipedia


"State-sponsored health insurance for all Marylanders such as the single-payer plan proposed by Democratic gubernatorial nominee Ben Jealous could cost $24 billion a year, forcing lawmakers to significantly raise taxes, according to a nonpartisan analysis.
"Such a cost would increase the state's $44 billion operating budget by more than half.
"The analysis, drafted by the state's Department of Legislative Services and released to The Baltimore Sun, said Maryland would have to levy a 10 percent payroll tax against every business and charge a $2,800 fee for every man, woman and child to pay for a new health care system in which doctors bill the state instead of private insurance companies.
"Dan Johnston, assistant director of research for National Nurses United, said Jealous could use a number of options to pay for the system: sales tax increases, payroll tax increases and income tax increases.
"The $24 billion estimate for the cost of a single-payer system did not include existing spending on Medicare, by the Veterans Administration and the military healthcare system, the analysts said.
"The spending could grow if the federal government withdrew Medicaid coverage or the state's administration of health care billing proved costly, the analysis noted.
"A single-payer system would disrupt Maryland's unique approach to paying for health care.
"The state and federal government have entered into an 'all-payer' contract in which the federal government provides about $1.8 billion more in funds than it would otherwise for Medicare, the government health system for older Americans.
"That contract would be voided if the state moves to a single-payer system, said Gene M. Ransom III, CEO of the Maryland State Medical Society. Ransom, who represents doctors across the state, said he worries about the disruption caused by a shift toward a single-payer system. He thinks it will cost much more than the state analysts say.
"If the current deal with the federal government is tossed out, Maryland could lose funding for the new Prince George's County hospital, Ransom said.
"Mizeur called the waiver 'the backbone of our state's health care system' that could be put at risk with the change Jealous is proposing.


With San Diego Comic Con looming, roving Radio Free Skaro reporter Warren Frey took it upon himself to interview Andrew James, the editor of the new Doctor Who range at Titan Comics. James spilled the beans on SDCC plans, a Doctor Who Day promotion across the U.S. and the U.K. and much more, but first…a massive (one could even say Titan-ic) amount of news. From the leak of Deep Breath (or a somewhat unfinished version of it, anyway) to action dolly news, Big Finish updates and more, the Three Who Rule were overwhelmed by an avalanche of information. And all this without an official Doctor Who panel at Comic Con! Madness. Pure madness.
Radio Free Skaro #431 – Click here to listen!
– Series 8 Trailer…1974 Style!
– Sanjeev Bhaskar…In Series 8!
– SPACE…Confirms Deep Breath Start Time!
– BFI…Sci Fi: Days Of Fear And Wonder!
– The Radiophonic Workshop…Plays The BFI!
– Doctor Who World Tour…Sydney Details!
– Doctor Who World Tour…Seoul Details!
– Big Finish…Adapts Missing Adventures!
– TARDIS And Eleventh Doctor…LEGO!
– 50th Anniversary Tribute…In LEGO!
– Classic Doctor Who DVD Compendium…Details!
– Walgreens…To Stock Action Dollies!
– Chicago TARDIS…Big Finish Guests!
– Chicago TARDIS…Announces Mat Irvine!
– Chicago TARDIS…Announces Dominic Glynn!
– Titan Comics…SDCC Comic Pack!
– Andrew James…Of Titan Comics!
Sadly, a trio of recent deaths in the Doctor Who world lead off this week's episode, as we remember the contributions of writer/actor Glyn Jones, director Derek Martinus, and the Rani herself, Kate O'Mara. But with new Doctor Who still months away, trickles of information are beginning to emerge as to the shape of Series Eight, including returning writers (Gareth Roberts), new actors (Tom Riley) and…well, that's about it. It's only April! One thing you won't have to wait for is the return of Fluid Links, where the Three Who Rule once again take your questions about the show and use their tiny mind-computers to formulate opinions. Next week, it's another classic series commentary with "The Curse of Peladon"! Whee!
Radio Free Skaro #416 – Click here to listen!
– Gareth Roberts…writing for Series 8!
– BBC iPlayer…available of 30 days!
– Monster Day Out at…the Doctor Who Experience!
– Radio Free Skaro on…Blue Box Podcast!
– Chris talks about "The Ark" on…TARDIS Tavern!
It's the beginning of the next 400 episodes of Radio Free Skaro, and what better way to start off this new era than with talk of Star Wars, weather in Florida, hockey, Tim Hortons and other irrelevant meanderings! The Three Who Rule eventually focused their energies and relayed what little Doctor Who news eked out this week, including such gems as new guests for Gallifrey 2014 (and the lineup for our own live show on Friday, February 14th), the return of friend of the show Phil Ford to Doctor Who, and other assorted newsy morsels.
All mere preamble to a commentary recorded this summer at Westercon for "Silver Nemesis". We're not saying our commentary is good, but rest assured it is better than the story itself, so have a listen to it, won't you?
Radio Free Skaro #401 – Click here to listen!
– Radio Free Skaro…Gallifrey Stands!
– Doctor Who…Series 8 Begins Filming!
– Phil Ford…Writes for Series 8!
– BFI Matt Smith Celebration…Video!
– City of Death…Novelization in Hardcover!
– Doctor Who Console Video Games…Are No More!
– National Television Awards…Fictitious Nominations!
From its origins on a humble Skype connection in 2006 to the quasi-shabby status it endures today, Radio Free Skaro has tried to entertain, inform and educate its listeners about the wonderful world of Doctor Who. And in this, its 400th episode, it may have finally succeeded. Joining us for a retrospective roundtable on the Matt Smith era were Chris and Laura Mead of the Oodcast, Luke Harrison of TMDWP, Kyle Anderson of the Doctor Who: The Writer's Room (and Nerdist fame) and Chip, the Two Minute Time Lord. What did these luminaries, and to a much lesser extent, Steven, Warren, and Chris think of Matt Smith's run as the Doctor? You'll just have to listen to find out. You'll also have to endure some blather about stats beforehand. Vegetables before you get your dessert!
Radio Free Skaro #400 – Click here to listen!
– The Time of the Doctor…Appreciated!
– The Time of the Doctor…Final Viewing Figures!
– The Time of the Doctor…Sets Another BBC America Record!
– Tom Baker's New Year's…Message!
– The Best of The Doctor…On Region 4 DVD!
– Babelcolour's…50th Anniversary Tribute Video!
– Chris and Laura Sigma…from The Oodcast!
As we turn the corner into October in this 50th anniversary year of Doctor Who, the Three Who Rule reach the halfway point in their odyssey of covering the eras of each producer of the classic series in the Miniscope. This week, the Barry Letts epoch is the focus, a five year stretch of classic episodes that vaulted Doctor Who from a Saturday tea-time tradition to a British television institution. A lifelong fan of the era, Gary Russell, who has been involved with the show in many ways since the early 1980s, joins us to discuss the many strengths of Letts's time on the show. Steven, Warren, and Chris also reunite to discuss the news of the week, including details of a worldwide simulcast of The Day of the Doctor, which were announced earlier this week. Fun and exciting!
Radio Free Skaro #387 – Click here to listen!
– Doctor Who simulcast…in 75 countries!
– Doctor Who Revisited…coming to Space!
– Sherlock, The Doctor, and Me…with Steven Moffat!
– Pup Ltd Doctor Who…show reel!
– Doctor Who loses…at the Welshies!
– Gareth Roberts is novelizing…City of Death!
– Tenth Doctor ebook…by Derek Landy!
– Edmonton Doctor Who themed…election signs!
Gally is over for another year. While the Three Who Rule briefly reminisce about the glory that was Gallifrey One's Network 23 in this episode of Radio Free Skaro, it's back to normal for podcaster and listener alike for the next few months – at least until next year's The 24 Hours of Gallifrey One, or y'know, until the new series of Doctor Who starts in the autumn. To help us get back into the swing of things, we present to you a commentary on the 2011 Doctor Who Christmas special, The Doctor, The Widow and The Wardrobe, as well as a smattering of news and views of what was missed while we were all living it up at Gally.
Radio Free Skaro #299 – Click here to listen!
– Michael Troughton Records…Ice Warriors Commentary!
– Torchwood: Miracle Day…On North American DVD/Blu-ray!
– Doctor Who: The Eternity Clock to use…Unreal Engine 3!
– Doctor Who: The Adventure Games…Cancelled!
– Karen Gillan to attend…the official Doctor Who Convention!
– The Doctor, The Widow…and The Wardrobe!
SPACE Podcast – September 30, 2011. Click here to listen!
The Three Who Rule chime in with a capsule review of Gareth Roberts' Closing Time, and Cynthia Loyst, the new InnerSPACE host, makes her first appearance, all on the latest InnerSPACE podcast!
For the uninitiated, the InnerSPACE Podcast is the official podcast from SPACE Channel, the Canadian home of Doctor Who. Hosted by Mark Askwith, this weekly podcast features chatter about various news and events in the sci-fi world, as well as banter about the various shows that air on SPACE including Doctor Who.
Listen to the episode in the media player above, or check out the podcast on the SPACE website here.
Continuing in the new tradition of stealing the BBC's thunder, a BBC America press release today revealed the title of Gareth Roberts' episode 12 as Closing Time.
The BBC had thus far kept the titles for Episodes 12 and 13 under wraps, but with this announcement, all titles are now known for the latter half of Series 6 with the exception of Steven Moffat's Episode 13 finale. Of course nobody outside of the production office knows when that last title will be revealed, but it wouldn't be surprising if the BBC kept it hidden for a while yet, despite the imminent return of the series.
The BBC America press release can be found here.
– The Minute…Doctor Who Podcast!
– Series 6…Episode 1 and 2 Titles!
– Series 6…Episode 3-7 Titles!
– Michael Sheen…in Doctor Who!
– Lords…Of The Red Planet!
– Spearhead From Space…Revisitations DVD Extras!
– Terror Of The Autons…DVD Extras!
– Tom Baker…Joins Big Finish!
– Sarah Jane Adventures…Fictitious RTS Award!
– Steven Moffat…Fictitious RTS Award #1! And Fictitious RTS Award #2!
– Colin Baker And Nicola Bryant…Join Twitter!
The world of Doctor Who lost one of its icons this past week, and all fans are mourning the passing of our beloved Brigadier, Nicholas Courtney. The highs from Gallifrey came crashing down as the news of Courtney's death hit earlier in the week, and it was only fitting that a Courtney tribute episode be recorded. We welcomed Doctor Who script editor, New Adventures author and Doctor Who Magazine editor, Big Finish producer and life-long Doctor Who fan Gary Russell on the show to reminisce about his experiences with the wonderful Mr. Courtney. Please join us as we remember Sir Alastair Gordon Lethbridge-Stewart, the man who portrayed him as well as cover the news of the week.
– Gareth Roberts…Writes For Series 6!
– Planet Of The Spiders…DVD Extras!
– Doctor Who Radio Plays…Box Set!
– Doctor Who…Ranked By IGN!
– Vincent And The Doctor…Nominated For A Nebula!
– A Christmas Carol…Nominated For A Saturn!
– Revelation of the Daleks…Action Figures!
Episodes	A Christmas Carol, David Walliams, DVD, Exploration Earth - The Time Machine, Fictitious Awards, Frontios, Gareth Roberts, gary russell, James Corden, Nebula Awards, Nicholas Courtney, Planet of the Spiders, Radio Plays, Revelation of the Daleks, Saturn Awards, Series 6, Slipback, The Ghosts of N-Space, The Paradise of Death, The Pescatons, Toby Whithouse, video games, Vincent and the Doctor, Whatever Happened To... Susan?


It's not all that often that you meet a Football League chairman who is also a successful racing driver and ice cream entrepreneur, but then Andrew Howard is not most people.
Autonomous Motor Racing – What Do The Humans Think?
Set to launch next year, RoboRace will be motorsport's first foray into driverless competition. But what do the real drivers think of the concept? We asked three for their views.
It is 10 years since Richard Burns, Britain's last World Rally Champion, succumbed to a brain tumour. We remember rallying's gentleman superstar.
Last season Sebastien Buemi narrowly missed out on the Formula E title. This time around he'll be hungrier than ever to go all the way.
Formula E enjoyed a great first year despite initial scepticism. But it's next task is arguably a tougher one: continuing with that momentum.
How does Nicolas Prost live up to one of the most famous fathers in motorsport? How does Alain cope with seeing his son on track? We looked into France's great racing dynasty.
They are the unsung heroes of motorsport. At every level, from club racing to Formula 1, marshals are as vital as the cars themselves.
Can Formula E Profit From F1's Latest Crisis?


Would you say it changed for the better?
Alex-Segre/ShutterstockSince its initial inception in 1975, the Zara brand has rapidly burgeoned into an ubiquitous icon in the fashion industry. The world of fast fashion doesn't seem complete without its monochrome interior and fluorescent Helvetica logo. Their brilliant business tactic lay in selling affordable clothing in a store that exuded a high-fashion vibe. By establishing a healthy compromise between pricey designer stores and bargain basements, the company has rightly earned its title of one of fashion's biggest retailers through letting people wear the latest runway trends without breaking the bank. Who said you can't be fashionable and economical? (Here are 11 fashion tips that will make you look more expensive).
In an article by the New York Times, Zara communications director, Jesus Echevarría, divulged their inspiring success story. According to the story, Inditex, the parent company of its flagship Zara and several other smaller chains, collectively makes around 840 million garments a year and has about 5,900 stores in 85 countries—as of 2012. That number is apparently always changing because Inditex has opened more than a store a day in recent years, which equates to a whopping total of about 500 stores a year. Believe it or not, it can take a new garment as little as 15 days to go from design production to store shelves.
So where did the sartorial story really begin?
In 1975, Amancio Ortega Gaona, the brand's original founder, decided to open up a small store in La Coruña (a town in northwestern Spain) that specialized in housecoats and robes. As a fan of the critically acclaimed 1974 film Zorba the Greek that had recently been released, he decided to name his creation after it.
The store was initially deemed as Zorba at its inception, but it turned out that Zorba the Greek was quite the popular concept. Gaona was soon approached by the owner of a bar two blocks away that had donned the same exact name. Understandably, the owner complained that it would be way too confusing to have two Zorbas in town (one that sold beer and another that sold clothes), so Gaona was forced to change his label.
To make matters more complicated, Gaona had actually already made the molds for the letters in his sign, so the resourceful mogul decided to be cost-effective and work with what he had. By rearranging some of the mold letters in his possession, he settled on the shorter and snappier Zara. The holding company Inditex was fashioned in 1985 after the company's international expansion, eventually spiraling into the distinguished sartorial legend responsible for saturating our paychecks on a periodic basis.


The intersection of nature and sensuality pays homage to the tradition of Venus depicted in the wilderness. The representation of human as animal and the comparison of feminine beauty to the natural terrain are both themes. The timeless aspect of the landscape contrasts with the short-lived primetime of a human lifespan.
The old masters of painting, such as Raphael and Botticelli during the renaissance, and later artists such as impressionist Renoir, paired the figures of women with picturesque terrains. Photographers such as Edward Weston and Alfred Stieglitz followed suit. Surrealist photographer Jerry Uelsmann furthered the pairing, montaging figures to appear integral with their wilderness habitats.
To the uninitiated, the context of the landscape adds legitimacy to the otherwise taboo subject of the undraped form in art. For others, the parallels between the body and the land are an observable banquet of organic texture, sweeping lines, and visual power of the sky.


Sure, it's the off-season for America's national pastime, but there's no such thing as too much baseball. To get you in the mood for some long extra innings of winter training, this DVD of the week shows how tough it is to make it to the Big Leagues.
Miguel "Sugar" Santos (Soto) is a 19-year-old Dominican who's in love with baseball. He doesn't feel at home unless he's on the mound throwing devastating curveballs. Sugar's talent earns him a ticket out of the DR and a life of poverty. After proving his worth in a tryout with the fictional major league Kansas City Knights, he is sent to the Knights' minor league affiliate in Bridgeport, Iowa, where he lives with a farm family that takes in ball players every year.
At first, Sugar is unable to communicate in English, and his new environment makes him feel isolated. His only friend, Jorge (Rufino), a veteran Dominican minor leaguer, tries to guide him on a path to greatness, teaching him that there's more to the game than striking batters out. Eventually, Sugar's struggles on the mound and off the field begin to take a toll. Following an injury, he is demoted to the bull pen, and Sugar must decide if he wants to chase his Big League dream or give it up.
STACK's Take: A realistic portrayal of the difficulties faced by foreign players trying to make it to the Majors. But athletes from anywhere, who are trying to make a name for themselves in any sport, can learn a lot from this film.


text:
Urbanist on Twitter
Cold Is Cool For Retai
In certain cities, winter has made its presence known. From the wild winds whipping down the city streets to the snow and sleet pounding the pavement. While summer and spring weather pushes people out of the big cities, winter keeps them in. City dwellers tend to stay close to home and spend quite a bit of time indoors, which has helped the delivery industry thrive. From meals to groceries to fashions to even flat screen TVs—practically anything can be delivered right to your apartment. Technology has also stepped in making it easier than ever to order via text, online, or with the swipe of an app. As more and more companies dive into this delivery realm, the consumers are the ones that will ultimately benefit from the competition. And the Urbanist, will bring these stories right to your doorstep all winter long (with no delivery fee).
Dig in, discover. @_The_Urbanist
Dressing Up The Future Of Fashion
Rebecca Minkoff is now trying out ebay proprietary technology in dressing rooms in select stores. Essentially, the innovation uses kinetic sensors to facilitate the shopper experience. For example, if a shopper doesn't find an outfit in her size, the sensors will record that data. The store can then email the customer at a later date when the dress size is made available online or in-store. The benefit of this new technology is strengthening the relationship with the consumer by offering her the convenience of not having to keep checking back to see if the outfit is available—a benefit that goes a long way in transforming shoppers into brand loyalists.
Virtual Disruption Hits The Streets
Big brand advertisers are lured to cities basically because of their massive crowds in a confined space—the perfect 24/7 captive audience. The hurdle for these brands? Competition. Ad billboards galore litter the streets and sky. Posters are plastered underground. Technology, too, has started to play a role in recent years, offering video ads. And now instant commerce has entered the city scene to play more of an upfront role.
2(X)IST men's fashion is one brand taking advantage of this on-the-spot commerce. In manhattan, the brand currently features scantily clad male models on telephone kiosks. Aside from stopping traffic, these ads also have the ability to transform city dwellers into instant consumers with their QR codes. Shoppers simply scan the code with their phones and can immediately buy the fashion for themselves or their loved ones.
Interaction has also made a leap forward, popping up in the most unexpected places, like a crosswalk in Hildesheim, Germany. Students have installed video screens on street corners that literally transform the crosswalk into a virtual game of pong. Aside from entertainment value, this also opens the doors for brands to further bridge the virtual and real world gap in the hopes of incentivizing a purchase. Both types of technology further prove that you don't have to stay online to make digital work for your brand.
How Brands Take Flight
Walking through the airport now, and you'll see a zillion different brands. To stand out, you need to understand the environment and target. Three brands that have broken through the sea of sameness are:
Butterfly Twists: This foldable-footwear brand has succeeded by crafting a product that's perfect for business travelers. A comfy corporate footwear replacement that's also one size fits all, which cuts down on product-selection time.
Al nassma: This Dubai chocolate company has added a twist to the typical candy offerings—rich chocolate made from camel's milk. To further cut through the confectionary clutter, Al nassma created unique displays that bring this attribute to life.
Wonderful Pistachios: Name recognition and its iconic green color have helped set the brand apart at shelf. Plus, the fact that it's a healthy alternative to candy and pizza, and has resealable package. Both of which have resonated well with busy travelers.
At the end of the day, these brands have succeeded where others haven't because of their deep understanding of the travel retail atmosphere at shelf and the different mindset of the business traveler.
Brands have succeeded because of their deep understanding of the travel atmosphere.
For more urban trends & insights, check out next month's issue.
Got questions? Email us at urbanist@integer.com or tweet @_The_Urbanist
Categories:2015
©2020 The Integer Group®


text:
//-----------------------------------------------------------------------
// <copyright file="FollowersIdsCommand.cs" company="Patrick 'Ricky' Smith">
//  This file is part of the Twitterizer library (http://www.twitterizer.net)
//
//  Copyright (c) 2010, Patrick "Ricky" Smith (ricky@digitally-born.com)
//  All rights reserved.
//
//  Redistribution and use in source and binary forms, with or without modification, are
//  permitted provided that the following conditions are met:
//
//  - Redistributions of source code must retain the above copyright notice, this list
//    of conditions and the following disclaimer.
//  - Redistributions in binary form must reproduce the above copyright notice, this list
//    of conditions and the following disclaimer in the documentation and/or other
//    materials provided with the distribution.
//  - Neither the name of the Twitterizer nor the names of its contributors may be
//    used to endorse or promote products derived from this software without specific
//    prior written permission.
//
//  THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS "AS IS" AND
//  ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT LIMITED TO, THE IMPLIED
//  WARRANTIES OF MERCHANTABILITY AND FITNESS FOR A PARTICULAR PURPOSE ARE DISCLAIMED.
//  IN NO EVENT SHALL THE COPYRIGHT OWNER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT,
//  INDIRECT, INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, BUT
//  NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; LOSS OF USE, DATA, OR
//  PROFITS; OR BUSINESS INTERRUPTION) HOWEVER CAUSED AND ON ANY THEORY OF LIABILITY,
//  WHETHER IN CONTRACT, STRICT LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE)
//  ARISING IN ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE
//  POSSIBILITY OF SUCH DAMAGE.
// </copyright>
// <author>Edgardo Vega</author>
// <summary>The Friendship Resources members command class.</summary>
//-----------------------------------------------------------------------

namespace Twitterizer.Commands
{
    using System;
    using System.Globalization;
    using System.Net.Http;
    using Twitterizer.Core;
    using Twitterizer.Models;

    /// <summary>
    /// Returns the members of the specified list.
    /// </summary>
    [AuthorizedCommand]
    internal class FollowersIdsCommand : TwitterCommand<UserIdCollection>
    {
        /// <summary>
        /// Initializes a new instance of the <see cref="GetListsCommand"/> class.
        /// </summary>
        /// <param name="requestTokens">The request tokens.</param>
        /// <param name="options">The options.</param>
        public FollowersIdsCommand(OAuthTokens requestTokens, UsersIdsOptions options)
            : base(HttpMethod.Get, string.Format(CultureInfo.CurrentCulture, "followers/ids.json"), requestTokens, options)
        {

            if (requestTokens == null)
            {
                throw new ArgumentNullException("requestTokens");
            }

            this.DeserializationHandler = UserIdCollection.DeserializeWrapper;
        }

        /// <summary>
        /// Initializes the command.
        /// </summary>
        public override void Init()
        {
            UsersIdsOptions options = this.OptionalProperties as UsersIdsOptions;

            if (options == null)
            {
                this.RequestParameters.Add("cursor", "-1");
                return;
            }

            if (options.UserId > 0)
                this.RequestParameters.Add("user_id", options.UserId.ToString(CultureInfo.InvariantCulture.NumberFormat));

            if (!string.IsNullOrEmpty(options.ScreenName))
                this.RequestParameters.Add("screen_name", options.ScreenName);

            this.RequestParameters.Add("cursor", options.Cursor > 0 ? options.Cursor.ToString(CultureInfo.InvariantCulture) : "-1");
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
\section{Introduction}

The basic physical scenario of active galactic nuclei and quasars is
generally believed to be a supermassive black hole surrounded by accretion disk
which releases the observed huge body of energy (Rees 1984). However
in this model one prominent problem is the fuel. Syer, Clark, \& Rees (1991)
investigate the possibility of accretion disk capturing stars in dense
star cluster of nucleus (within 1pc) in order to remove the accretion
fuel problem. This interesting interaction has been employed to explain
the high metallicity phenomena in active galactic nuclei and quasars by
Artymowicz, Lin \& Wampler (1993), Zurek et al (1994), especially for
broad absorption line (BAL) quasars with extremely high metallicity
(sometimes several hundred times that of solar abundance, Shields 1996).
It is interesting to note that this process also result in the formation
and coalescence of compact objects in the central
energy house of active galactic nuclei and quasars which may be
sources of frequent $\gamma$-ray and gravitational wave bursts.

Gravitational wave could soon be detected directly even emitted from a
source located at a cosmological distance because several
ground-based gravitational wave experiments including
the Laser Interferometer Gravitational-Wave Observatory
(LIGO) (Abramovici et al. 1992), VIRGO, TAMA300 and GEO600 are
under construction. The best understood of all gravitational-wave
sources are coalescing, compact binaries composed of neutron stars
and black holes. These NS/NS, NS/BH and BH/BH binaries may
give information about the equation of state (EOS) of nuclear
matter at high densities (Shibata, Nakamura \& Oohara 1992, 1993;
Rasio \& Shapiro 1994; Zhuge, Centrella \& McMillan 1994; Davies et al.
1994; Ruffert, Janka \& Sch\"afer 1996; Cheng \& Dai 1998).

In addition the observations of afterglow of Gamma-ray Burst (GRB)
lend strong supports to the
cosmological origin of GRB (Paczy\'nski 1986, Mao \& Paczy\'nski 1992,
Meegan et al 1992, Piran 1992) (see a concise review by Greiner
1998 for the afterglow, and Piran 1998).
Despite the effort of searching more than 20 years to look for the
counterparts of GRB at
other wave bands, no known population of objects in the Universe
have been identified with any GRB sources (e.g.
Fenimore et al. 1993, Fishman \& Meegan 1995, Band \& Hartmann 1998).
Two main reasons to cause this situation. First, the position accuracy
of GRB detected by BASTE is so low that a large number of known objects
are  located in its error box. Secondly, the burst duration is so short
that it is very difficult to use other means to reduce the error box.
Although the BeppoSAX has observed a dozen of GRBs' afterglows, one of
these sources can reduce its error box down to $\sim$
one arc second. But still no confirmed counterparts are identified,
even for the well-observed, GBR970228 and GRB970508. On the
other hand, the observed isotropic and inhomogeneous distribution of
GRBs detected by the BASTE instrument on board the Compton Gamma-Ray
Observatory (CGRO) is best explained by a source population at
cosmological distances.

Most cosmological GRB models involve compact objects. For examples,
(1) neutron star - neutron star/black hole merger
(e.g. Paczy\'nski 1986; Eichler et al 1989;
Dermer 1992; Narayan, Piran \& Shemi 1991; Mao \& Paczy\'nski 1992);
(2) collision between black hole and Helium core or white dwarf by
Fryer \& Woosley (1998), Fryer et al (1998);
(3)the phase transition from neutron star to strange star (Cheng \& Dai
1996); (4) the transition of normal nuclear matter to matter with pion
condensation in neutron star (e.g. Haensel et al 1990,
Muto et al 1993); (5) rapidly rotating neutron star with extremely large
magnetic field (Usov 1992, Duncan \& Thompson 1992);
(6) a failed supernova type Ib (Woosley 1993), or microquasar (Paczy\'nski
1998) etc. Therefore, if we want
to find the hosts of GRB sources, it is logical to look for cosmological
sources with a lot of compact objects. From the stellar evolution point of
view, the progenitors of compact objects, e.g. neutron stars, are massive
stars (approximately $5\sim 20 M_{\odot}$).
>From the observations of afterglows of GRBs it has been deduced by
Paczy\'nski (1998) that GRB may associate with the star formation region.
We note that most of the masses of the massive stars, consisting of
a lot of heavy elements, will be ejected during the
supernova explosion and a metal-rich region will be formed.
Naturally, galaxies with high abundance of
compact object should be metal-rich. Therefore it is logical to look for
cosmological sources with high metal abundance. In order to observe the
sources located at cosmological distance, these sources must be luminous.
It should be noted that most AGNs/QSOs are metal-rich (Artymowicz, Lin \&
Wampler 1993,
Hamann et al 1997). This may be the real reason why GRBs may be related
to AGNs and QSOs as reported by Schartel, Andernach \& Greiner (1996),
and Burenin et al (1998) who claim
there are possible association of $\gamma$-ray burst with radio quiet
quasar, and with active galactic nuclei, respectively. However
the physical scenario of this association remains open if it is true,
at least, some of GRB are related with AGNs/QSOs.
It has been suggested that
GRB may be produced in a star formation region which leads to
expectation of the burst rate of GRB proportional to the formation
rate of star in the cosmological galaxies (Paczy\'nski 1998). Because
the lifetime of AGN/QSO is rather short
(generally less than $10^8$ yr), the possible host objects of GRB are
mostly ones related with galaxies. Alternatively here we suggest that
the interaction between accretion disk and stars in dense cluster may lead
to the formation of a large number compact objects in the central
engine of active galactic
nuclei. The formation and interactions among the compact objects in the
nuclei might associate with GRB. Therefore active galactic nuclei are
one kind of its host objects if GRBs are indeed associated with compact
objects.

\section{The Model}

The mechanism for the enhancement of
metal-rich elements has been suggested by a way of evolution of
main sequence stars, which are captured by the accretion disk
surrounding the supermassive black hole in the center of quasar
(for a review cf. Lin \& Papaloizou 1996). The captured stars would accrete
material from the disk and increase their masses up to 50 solar masses in
less than $10^4$ years. These massive stars evolve rapidly toward the
supernova stage
and the ejecta of the supernovae provide enough heavy element to produce
the features suggested by observations.
The metal abundance expressed in terms of the ratio
between NV and CIV is related to the total number of
captured main sequence stars $N_{\rm MS}$ during the active phase of quasar
as follows (Artymowicz, Lin \& Wampler 1993; Zurek et al 1994)
\begin{equation}
\frac{{\rm NV}}{{\rm CIV}}\approx 0.01
		       \left(\frac{N_{\rm MS}}{1.0\times 10^5}\right).
\end{equation}
However this mechanism
results in other implications, such as formation of neutron stars/black holes
in the vicinity of the accretion disk.
As we will argue in the subsequent section,
it exists an efficient way to form compact object - compact object
(i.e. NS/BH, NS/BH) binaries via the formation of
compact object - red giant star (NS/BH, RG) binaries.
The (NS/BH, NS/BH) binary will be formed after the explosion of the red
giant star. In such a scheme the merger rate of (NS/BH, NS/BH) binary
approximately equals to the capture rate of main sequence star, therefore
it is proportional to the metal abundance. If the merger of (NS/BH, NS/BH)
binary or Helium core of RG and black hole is one of the possible mechanisms
of GRBs, then active galactic nuclei and quasars should associate with GRBs.
In fact the coalescence of two compact objects also produces intense
transient gravitational waves which should be detected by LIGO/VIRGO in
1Gpc radius.

\subsection{Evolution of the captured stars in the accretion disk}

We assume that the nucleus of the quasar consists of a massive black hole
surrounded by an accretion disk, which are enclosed by a star cluster.
The structure of disk is described by the standard model in which
the local height and the surface density of the accretion disk are given by
(e.g. Frank, et al 1992)
\begin{equation}
\left(\frac{h}{R}\right)=1.6\times 10^{-3}
      \alpha^{-1/10}\dot{m}^{3/20}M_8^{-1/10}r_{\rm d}^{1/8},
\end{equation}
and
\begin{equation}
\Sigma=1.7\times 10^7 \alpha^{-4/5} \dot{m}^{7/10} M_8^{1/5}r_{\rm d}^{-3/4}
       ({\rm g~cm^{-2}}),
\end{equation}
respectively, and the inward drift velocity due to the outward
transportation of the angular momentum in disk reads
\begin{equation}
v_{\rm r}=4.1 \times 10^4 \alpha^{4/5}\dot{m}^{3/10}M_8^{-1/5}r_{\rm d}^{-1/4}
	  ({\rm cm~s^{-1}}),
\end{equation}
or the time scale of inward drift is
\begin{equation}
\tau_{\rm r}=4.0\times 10^7 \alpha^{-4/5}\dot{m}^{-3/10}M_8^{6/5}
	     \left(\frac{r_{\rm d}}{10^5}\right)^{5/4}({\rm yrs}),
\end{equation}
where $\dot{m}$ is dimensionless accretion rate scaled with the Eddington limit,
$\alpha$ is the
viscosity coefficient, $r_{\rm d}$ = $\frac{R}{R_s}$ is the radius of disk
normalized by Schwartzchild radius
$R_s=\frac{GM_{\rm BH}}{c^2}$, and $M_8$ denotes
the mass of central black hole ($M_{\rm BH}$) in units of $10^8M_{\odot}$.

The main sequence stars in the star cluster will be captured by the disk and
the number of the captured main sequence stars in the annular $R-R+dR$ is
estimated as (Artymowicz, Lin \& Wampler 1993),
\begin{eqnarray}
dN&=&m_*G^2(\Sigma RdR)\frac{32\pi^{1/2} C_d \nu_0 \Delta T}
                            {\sigma_0^3} \nonumber\\
  &            \approx& 0.45\left(\frac{m_*}{M_{\odot}}\right)
               \left(\frac{\nu_0}{10^7{\rm pc^{-3}}}\right)
	       \left(\frac{\Delta T}{10^8{\rm yr}}\right)
	       \left(\frac{\sigma_0}{300{\rm kms^{-1}}}\right)^{-3}\nonumber\\
  &        &\alpha^{-4/5}\dot{m}^{7/10}M_8^{11/5}r_{\rm d}^{1/4} dr_{\rm d}
\end{eqnarray}
where $\Delta T$ is the active period of quasar, $\nu_0$ is the number
density of star cluster at 1 pc in the range of about $10^7$/pc$^3$
(Blandford 1991), $\sigma_0$ is the dispersion velocity of star in
the cluster, and $C_d\approx 6$. Integrating over the disk, there are
$\sim 10^5$ main sequence stars captured by disk in the active phase of
quasar or the captured rate is $\sim 10^{-3} yr^{-1}$.
The captured stars will
coorotate with the medium in the disk (Syer et al 1991), and
accrete gas from the disk with Bondi
rate until a gap appears in disk with condition that the star's Roche
radius exceeds the disk scale-height $h$ (Lin \& Papaloizou, 1996). The
timescale of Bondi accretion is
\begin{equation}
\tau_a=1.40\times 10^3\alpha^{2/5}\dot{m}^{-1/10}M_8^{2/5}
       \left(\frac{r_{\rm d}}{10^5}\right)^{3/4}
       \left(\frac{m}{M_{\odot}}\right)^{-1} ({\rm yrs}),
\end{equation}
and the maxium accreted mass of the captured star is limited by
\begin{equation}
\left(\frac{m}{M_{\odot}}\right)=17.7 \alpha^{-3/10}
		    \dot{m}^{9/20} M_8^{7/10}
		    \left(\frac{r_{\rm d}}{10^5}\right)^{3/8}.
\end{equation}
This condition is also
coincided with that the Bondi radius ($r_{\rm B}=Gm_*/c_{\rm s}^2$)
does not exceed the local height $h$. With the typical parameters
of the quasars and $\alpha$ = 1, the maximum accreted mass of the
captured stars is in the range of 10 $\sim$ 20 $M_{\odot}$ (but the
maximum mass of the captured stars could be much higher than 20
$M_{\odot}$ if $\alpha$ is much less than unity).
The star in this mass range will evolve off their
main sequence quickly and likely become  neutron stars plus small
fraction of black holes (see e.g. Shapiro \& Teukolsky 1983). For more
massive stars (m $\ge$ 20 $M_{\odot}$) they could become neutron stars
or black holes (Timmes, Woosley \& Weaver 1996).
The simple formula of the evolution time scale for the main
sequence star is (Meurs \& van den Heuvel 1989)
\begin{equation}
\tau_{\rm e}=10^{a_1}\left(\frac{m}{M_{\odot}}\right)^{a_2},
\end{equation}
where the index $a_1$ and $a_2$ are tabulated in their table 3.
For interested cases, we have $a_1=9.3$, $a_2=-2$ for
$3.8\le m/M_{\odot}\le 12$, and $a_1=8.2$, $a_2=-1$ for star
larger than $12M_{\odot}$.
Substituting parameters for lower mass case into Eq.9, we obtain:
\begin{equation}
\tau_{\rm e}=9.0\times 10^6 \alpha^{3/10}\dot{m}^{-9/20}M_8^{-7/10}
	     \left(\frac{r_{\rm d}}{10^5}\right)^{-3/8}~~({\rm yrs}).
\end{equation}
The higher mass case will evolve faster than that given in Eq.(10). It has been estimated that the main sequence stars start to be
captured by the disk at the disk radius $\sim$1 pc
(Artymowicz, Lin \&  Wampler 1993)
but the exact value of this radius is not crucial in our model.
The more important radius $R_c$ is before which the captured stars
finish the evolution of supernova stage. This radius must be larger
than that of the tidal radius $R_{\rm t}$ =
$\left(\frac{M_{\rm BH}}{m_*}\right)^{1/3}r_*$, otherwise the captured
stars will disrupted by the central massive black hole.
This radius can be estimated by equating the radial inward drifting
time scale Eq.(5) and the evolution time scale
Eq.(11) and is given by
\begin{equation}
r_{\rm c}=\frac{R_{\rm c}}{R_{\rm s}}
	 =4.0\times 10^4 \alpha^{44/65}\dot{m}^{-6/65}M_8^{-76/65}.
\end{equation}
It appears that this radius is always larger than that of $R_t$ for typical
quasar parameters.

\subsection{Formation of binaries}

In the early stage, almost all of the captured stars can evolve to
neutron stars/black holes with mass $m_{\rm ns}$
which will be ejected from the disk after supernova
explosion. But these neutron stars/black holes can only shoot up to a
scale height
\begin{equation}
h_{\rm ns}=\frac{v_{\infty}^2 R_{\rm c}^2}{G M_{\rm BH}},
\end{equation}
where $v_{\infty}\sim$ 300 km/s is the neutron star kick velocity produced by
supernova explosion. Taking the typical parameters, $h_{\rm ns}\sim$
$10^{16}$ cm. The compact stars will be oscillating up and down
crossing  the disk. Artymowicz, Lin \& Wampler (1993) also note the
possibility of retrapping of compact stars by disk, but the following
case is more interesting.
Before evolving to compact star, the captured star will go through
the red giant phase with radius ($R_{\rm RG}$) and mass $M_{\rm RG}$.
During the close encounter with a neutron star, the
red giant star would undergo substantial tidal deformation
at the cost of a part of the relative kinetic energy of the orbit.
Such a tidal process can eventually dissipate
the total positive energy of the initial unbound orbit via oscillations
and heating, and a (NS/BH, RG) binary system will be created. One might argue
that the velocity dispersion of NS/BH is much larger than the escape velocity
of RG at its surface (about 70km/s). However, it is interesting to note
the following situation.  The surface density of RG
$\Sigma_{\rm RG}\sim M_{\rm RG}/R_{\rm RG}^2\sim 10^7$ g/cm$^2$ is
much larger than that of disk $\sim 10^3$ g/cm$^2$ at 0.1pc.
This leads to an efficient
dissipation of NS/BH kinetic energy in the process of encountering RG's
envelope. The probability
of NS/BH encountering the dense envelope of RG can be easily estimated
\begin{equation}
f=\frac{S_{\rm RG}}{S_{\rm disk}}\sim 10^{-2},
\end{equation}
where $S_{\rm RG}$ is the total surface area of all RG, and $S_{\rm disk}$
is the area of disk capturing main sequence star. The drag force acting on
NS/BH by the dense envelope of RG reads (Artymowicz et al 1993)
\begin{equation}
F_d=\frac{4\pi G^2m_{\rm ns}^2\rho C_d}{v_{\infty}^2}.
\end{equation}
After $N$ times of encountering the disk, the kinetic energy of NS/BH will
be reduced
significantly so that NS/BH can be captured by RG through tidal process,
\begin{eqnarray}
N&=&\frac{v_{\infty}^4}{8\pi fG^2 m_{\rm ns}C_d \Sigma_{\rm RG}}\nonumber\\
 &\sim & 10^4\left(\frac{f}{0.01}\right)^{-1}
	 \left(\frac{\Sigma_{\rm RG}}{10^7{\rm g/cm^2}}\right)^{-1}
	 \left(\frac{v_{\infty}}{300{\rm km/s}}\right)^4,
\end{eqnarray}
and the capture time scale of NS/BH by the RG envelope is about
\begin{equation}
\tau_{\rm ns, RG}=N\frac{h_{\rm ns}}{v_{\infty}}\sim 10^5{\rm yr},
\end{equation}
which is slightly shorter than the life time of RG, therefore a large
fraction of RG can be captured by the compact objects in the vicinity
of the disk to form (NS/BH, RG) binaries if we take into account the
interaction between NS/BH and the envelope of RG. Let us consider the
tidal capture rate in more detail. The distance $D$ for the tidal capture to
form a (NS/BH, RG) binary can be estimated as
(Bhattacharya \& van den Heuvel 1991)
\begin{equation}
D \approx 1.75R_{\rm RG} \left(\frac{m_{\rm ns}}{M_{\rm RG}}\frac{m_{\rm ns}+M_{\rm RG}}{M_{\odot}}
	  \frac{R_{\odot}}{R_{\rm RG}}\right)^{\frac{1}{6}}
	  \left(\frac{50{\rm Km/s}}{v_{\rm ns}}\right)^{\frac{1}{3}},
\end{equation}
where $v_{\rm ns}$ is the reduced velocity of the compact star. The cross section of this
capture process is given by
\begin{equation}
\sigma \approx \pi D^2\left[1+\frac{2G(m_{\rm ns}+M_{\rm RG})}{v^2_{\rm ns}}\right],
\end{equation}
and is $\sim 3 \times 10^{28} cm^2$ for typical parameters.
The formation rate of (NS/BH, RG) binary
thus can be written as
\begin{equation}
\frac{dN_{{\rm NR}}}{dt}=
       \left(\frac{N_{\rm ns}}{V_{\rm ns}}\right)
       \left(\frac{N_{\rm RG}}{V_{\rm RG}}\right)v_{\rm ns}\sigma V_{\rm RG}
       =k N_{\rm ns}N_{\rm RG},
\end{equation}
where $N_{\rm ns}$ and $V_{\rm ns}\sim h_{ns} R_c^2$
($N_{\rm RG}$ and $V_{\rm RG}$ )
are the number and occupied volume of compact stars (red giant stars)
respectively, and constant
$k=v_{\rm ns}\sigma/V_{\rm ns}$.
It should be noted that $N_{\rm ns}$ and $N_{\rm RG}$ are
time-dependent because the presence of (NS/BH, RG) binary formation results
from the tidal interaction between compact stars and red giant stars.
The time-dependent numbers of compact
stars and red giant stars obey the following equations
\begin{equation}
\frac{dN_{\rm RG}}{dt}=\Gamma-kN_{\rm ns}N_{\rm RG},
\end{equation}
\begin{equation}
\frac{dN_{\rm ns}}{dt}=\frac{N_{\rm RG}}{\tau_{\rm RG}}
		       -kN_{\rm ns}N_{\rm RG},
\end{equation}
where $\Gamma$ is the capture rate of main sequence stars by disk, and
$\tau_{\rm RG}$ represents the evolution time scale from red giant star to
NS/BH (about a few times of $10^5$ years).
These non-linear equations can be analytically resolved
in some interesting stages.

(1) When $t\le \frac{1}{\Gamma}$, the production of red giant stars
dominates, we have
\begin{equation}
N_{\rm RG} \approx \Gamma t,~~~ {\rm and}~~~
N_{\rm ns} \approx \left(\frac{\Gamma}{\tau_{\rm RG}}\right)t^2.
\end{equation}

2) In steady state, the numbers of compact stars and red giant stars
reach constants, i.e.
\begin{equation}
N_{\rm RG}(\infty)=\tau_{\rm RG}\Gamma,~~~~ {\rm and}~~~
N_{\rm ns}(\infty)=\frac{1}{k\tau_{\rm RG}}.
\end{equation}
It is clear that the (NS, RG) binary formation rate is a constant, i.e.
$\frac{dN_{{\rm NR}}}{dt}=\Gamma$.

\subsection{Coalescence of (NS/BH, NS/BH) and (BH, Hc) binaries}

The evolution of massive binaries leads to two possibilities: (1) Merging
of Helium core of RG and black hole, (2) (NS/BH, NS/BH) binary formations
and merging.  The first case occurs for very close binaries in which the
black hole companion  encounters with the Helium core before the secondary
evolves into compact object. This process is recently suggested as a GRB
mechanism by Fryer \& Woosley (1998).  The second corresponds to the case
which the secondary evolves into compact star faster than that of spiral-in
process. Then the (NS/BH, NS/BH) binaries are formed and eventually merge to
emit intense transient gamma-rays and graviational waves. The estimations
of above processes are given below.

The captured compact star may spiral-in the red giant star with the
core mass $M_{\rm core}$ and envelope mass $M_{\rm en}$. Many detail
calculations have been done (e.g. Bodenheimer \& Taam 1984;
Taam \& Bodenheimer 1989, Taamr  et al 1997).
A rough estimation of final separation of the binary after
spiral-in can be made by comparing the binding energy of envelope
with the difference in total energy of the binary before and after spiral-in
(Webbink et al 1983, Verbunt 1993)
\begin{equation}
\frac{D_f}{D_i}=\frac{M_{\rm core}}{M_{\rm RG}}
		\left(1+\frac{2D_i}{\alpha_{*} \lambda R_L}
		\frac{M_{\rm en}}{m_{\rm ns}}\right)^{-1},
\end{equation}
where $D_i$, and $D_f$ are the initial and final separation
respectively, $R_L$ is the Roche radius, which is given by
(Eggleton 1983)
\begin{equation}
\frac{R_L}{D_i}=\frac{0.49}{0.6+q^{-2/3}\ln (1+q^{1/3})},
\end{equation}
where $q$ is the mass ratio of (NS/BH, RG) binary system,
$\alpha_*$ is the efficiency with wich released binary energy is
used to lift the envelope; $\lambda$  a factor depending on the mass
distribution in the envelope of RG. Their product is often taken to be 0.20.
The core mass of red giant star for $M_{\rm RG} \ge 7M_{\odot}$ is given by (Iben 1993),
\begin{equation}
\frac{M_{\rm core}}{M_{\odot}}=0.058 \left(\frac{M_{\rm RG}}{M_{\odot}}\right)^{1.57}.
\end{equation}
And the radius of core is
given by (Paczy\'nski \& Kozlowski 1972; Pols \& Marinus 1994; Wijers 1998)
\begin{equation}
\frac{R_{\rm core}}{R_{\odot}}=
	     0.22\left(\frac{M_{\rm core}}{M_{\odot}}\right)^{0.6}.
\end{equation}
If $D_f$ is smaller than the sum
$R_{\rm core}+R_{\rm ns}\approx R_{\rm core}$, after spiral-in the compact
star merges with the core of the red giant star. We have calculated
some typical cases listed in Table 1. It can be found that the RG
massive than 18$M_{\odot}$ will merger with the Helium core before
they form a (NS/BH, NS/BH) binary. Even the companion star is a neutron
star, it may accrete efficiently material from the red giant to become
a black hole during the spiral-in process(Chevalier 1996;
Fryer \& Woosley 1998). Therefore the merger of (NS/BH, Hc) binary can
become $\gamma$-ray burst as described by Fryer \& Woosley (1998).

   There are two possible ways to destroy the formed (NS/RG, RG) binaries:
   1) the combining gravitation of central black hole and the dense
   star cluster, 2) the third encounter from the cluster. It has been
   shown by Saslaw (1985) that the chance of the later way is rather
   small. We can now estimate the action of the first way. If the
   tidal force from the gravitation of central massive black hole and
   dense star cluster exceeds the interacting force between the two
   components, then the (NS/BH, RG) will be disrupted by the tidal
   force. The tidal force reads
   \begin{equation}
   F_{\rm tid}=\frac{G(M_{\rm BH}+M_{\rm SC})(m_{\rm c}+M_{\rm RG})}{R^2}
               \frac{D_i}{R},
   \end{equation}
   where $M_{\rm SC}$ is the mass of dense star cluster, and $m_{\rm c}$
   is the mass of the compact object. Then the ratio between the tidal
   force and the gravitational force ($F_B$)
   between the two components is
   \begin{equation}
   \frac{F_{\rm tid}}{F_{\rm B}}=\frac{M_{\rm BH}+M_{\rm SC}}{M_{\rm RG}}
        \frac{M_{\rm RG}+m_{\rm c}}{m_{\rm c}}\left(\frac{D_i}{R}\right)^3
        \approx 10^{-4},
   \end{equation}
   which means that the formed binaries can survive in its surroundings.
   On the other hand, consequently the spiral-in process takes place in
   the binary very fast. The timescale
   of this process can be roughly estimated under the assumption that
   the formed (NS/BH, RG) binary keeps the total angular momentum constant.
   According to Verbunt (1993), this timescale reads
   \begin{equation}
   \tau_{\rm sp}=\frac{1}{2(1-m_{\rm c}/M_{\rm RG})}\frac{M_{\rm RG}}{\dot{M}}
                 \approx \frac{1}{2} \frac{M_{\rm RG}}{\dot{M}},
   \end{equation}
   where $\dot{M}$ is the rate of mass transfer onto the compact object.
   For the case of the RG as a donor in (NS/BH, RG)
   binary system, $\dot{M}$ can be
   estimated from Bhattacharya \& van den Heuvel (1991),
   \begin{equation}
   \dot{M}=1.4\times 10^{-2} M_1^{2.25}R_1^{0.75}~(M_{\odot}~{\rm yr^{-1}}),
   \end{equation}
   where $M_1=M_{\rm RG}/M_{\odot}$, and $R_1=R_{\rm RG}/R_{\odot}$.
   We thus obtain
   \begin{equation}
   \tau_{\rm sp}\approx 35.7 M_1^{-1.25}R_1^{-0.75}~({\rm yr}).
   \end{equation}
   From the above two equations we have the typical timescale for the
   case of RG with
   mass $10M_{\odot}$, $\tau_{\rm sp}\sim$ 2 yr. This simply means
   that the new formed (NS/BH, RG) binary will reach the final stable
   configuration $D_f$ (listed in the Table 1) within 2 years, and
   become hard from the soft state very rapidly. It is thus viable
   to form hard binary in accretion disk. Furthermore, it has been
   shown in more detail by Magorrian \& Tremaine (1999) that the highest
   tidal disruption rate $10^{-4}$yr$^{-1}$ only take place in faint
   galaxies ($L<10^{10}L_{\odot}$). The tidal disruption of giant star
   could produce flare as often as every $10^5$yr. Therefore it is robust
   to believe that the present model of star-disk interaction works dominately
   over tidal capture by supermassive black hole hosting in the center of
   AGN/QSO in the active phase of AGN/QSO.

The detailed study of orbital changes due to the explosion of
supernovae can be found in Pols \& Marinus (1994), and Portegies Zwart
\& Verbunt (1996). On the other hand, Verbunt(1993)
argued that this effect can be estimated by assuming that the
explosion is instantaneous, and the
positions and velocities of the stars are the same after the explosion as
before the explosion (Dewey \& Cordes 1987).
This implies that the distance $D_f$ between the compact star and the
core star before the explosion is the periastron distance after the
explosion and that the periastron velocity of the new orbit is the same
as the orbital velocity in the pre-supernova orbit. Therefore
the eccentricity is given by (Verbunt 1993)
\begin{equation}
e_{\rm ns} = {M_{\rm core} - m_{\rm ns} \over 2m_{\rm ns}}.
\end{equation}
The mass center of binary has obtained a speed $v_{\rm cm}$ because of the
mass loss and is given by
\begin{equation}
v_{\rm cm}=e_{\rm ns}v_1,
\end{equation}
where $v_1 = \sqrt{\frac{GM_{\rm core}}{D_f}} \sim 10^8
\left(\frac{M_{\rm core}}{4M\odot}\right)^{1/2}
\left(\frac{D_f}{1R_{\odot}}\right)^{1/2}$ cm s$^{-1}$
is the orbital velocity of the exploding component before explosion.
This velocity will make the (NS/BH, NS/BH) binary shooting up to a scale
height about $\sim 10h_{\rm ns}$. Furthermore, the orbit of the binary
is sufficiently small so it should be circularized by tidal interaction
and the radius $D_{\rm ns}$ of the circular orbit is given by
\begin{equation}
D_{\rm ns} = (1+e_{\rm ns})D_f.
\end{equation}
In table I, we list some possible values of $e_{\rm ns}$ and $D_{\rm ns}$ by
assuming $m_{\rm ns}=1.4M_{\odot}$. We can see that $e$ is larger than unity
when $M_{\rm RG}$ is larger than $15M_{\odot}$. This means that
after explosion the binary will be broken. For $m_{\rm ns}=3M_{\odot}$,
we find that $e$ is always less than unity and D$_f$ is larger than R$_c$
even when $M_{\rm RG}$ equals 20$M_{\odot}$, in other words, there is no
merger of massive black hole and helium core.

There are two interesting
consequences of the new born (NS/BH, NS/BH) binary. First, the kick velocity
will carry the binary to leave the disk up to the
distance about $10h_{\rm ns}\sim10^{17}cm$. Second, since
the separation of two compact stars in the (NS/BH, NS/BH) binary is
$\sim D_{\rm ns}$,
the gravitational radiation of the binary will make these two compact
stars merge in the time scale of (Peter 1964)
\begin{equation}
t_{\rm m}(D_{\rm ns},e)
  =\frac{12}{19}\left(\frac{D_{\rm ns}^4}{\beta c_1^4}\right) {\rm Int}(e),
\end{equation}
with
\begin{equation}
c_1=\frac{e^{\frac{12}{19}}}{(1-e^2)}
    \left(1+\frac{121}{304}e^2\right)^{\frac{870}{2299}},
\end{equation}
and
\begin{equation}
\beta=\frac{64}{5}\frac{G^3M_1M_2(M_1+M_2)}{c^5},
\end{equation}
and Int$(e)$ is the integral (see eq. 5.14 in Peter 1964). Therefore
the compact star merger rate should be about $\Gamma$. One should not
be surprised by the short time scale of merger since $t_m$
is proportional to $D_{\rm ns}^4$ while most of $D_{\rm ns}$ are less
than solar radius, and $t_{\rm m}\propto (1-e^2)^{7/2}$ for larger
eccentricity.

\section{Discussions}

In this paper we suggest that if the metallicity of the metal-rich quasars
result from the capture of
the main sequence stars by the accretion disk surrounding the central
massive black hole of quasars and the captured stars
can increase their masses by accretion
so they can evolve off their main sequence branch and move toward the
supernova stage which provide the observed metal abundance. Then the remnant
stars are likely compact stars, i.e. neutron stars or black holes.  We have
shown that the neutron star/black hole density in the vicinity of the disk
will be high enough to a population of (NS/BH, RG) bnaries
whic can eventually evolve to become either (i) (NS/BH, NS) binaries if
the mass of RG is less than $15M_{\odot}$ and  merge in a time scale of
a few million years or (ii) (NS/BH, Hc) binary.

In a wide range of cosmological GRB models the compact star merger plays
an essential role. Since the main sequence star capture rate
$\Gamma$ = 10$^{-3}$ yr$^{-1} \left(\frac{\rm NV/CIV}{0.01}\right)$
is proportional to
the metal abundance ${\rm \frac{NV}{CIV}}$ and the compact object
binary formation rate equals the
main sequence star capture rate in our simple model. Therefore, the
GBR burst rate $R_{\rm GRB}$ in AGNs or QSO can be estimated as
\begin{equation}
R_{\rm GRB} \sim 10^{-3}\eta {\rm \frac{NV/CIV}{0.01} yr^{-1} QSO^{-1}},
\end{equation}
where $\eta$ is the beaming factor of the $\gamma$-rays which reduces the
observed probability of GRBs resulting from the compact star mergers
(e.g. $\eta$ is 0.1-0.01 for NS/NS merger, Ruffert, Janka, Schafer 1996;
Ruffert et al. 1997; Ruffert \& Janka 1998). Such estimated GRB
rate in metal-rich quasars is much high than  that of ordinary
galaxies, e.g. the merger rate  due to the mass exchange
and gravitational radiation losses giving a conservative rate
$\sim 10^{-6} yr^{-1}$ (Phinney 1991, Narayan et al 1992),
or at a higher rate $10^{-(4\sim 5)}$ per year
(Tutukov \& Yungelson 1993, Portegies \& Verbunt 1996)
in light of the calculations of binary evolution.
Of course, the population of AGN/QSO is only 1\% of normal galaxies
which makes the total burst rate for these two classes of object comparable.
However the burst rate for individual AGN/QSO which has exceptional
high metal abundant could be very large. It has much higher possibility
that the not-yet-identified host of GRB may an AGN/QSO with very high
metallicity.

   Recently, Dokuchaev, Eroshenko \& Ozernoy (1998) propose the possibility of
   GRBs origin from the evolved galactic nuclei. In their model,
   GRBs result from  the coalescence of the compact object binary which
   are formed due to the dynamical evolution of cluster and dissipation
   of gravitational radiation. Carter (1992) proposed that
   GRBs are produced by the tidal disruption by the central supermassive
   black hole. Rees (1988) even pointed out that the rate of tidal
   disruption could be $10^{-4}$yr$^{-1}$ which is significantly
   lower than the capture rate [see eq.(6)] and formation rate of
   (NS/BH, NS/BH) binaries, particularly the whole star (unless
   giant star) will be swallowed
   by the supermassive black hole with mass $>10^8M_{\odot}$ since the Roche
   radius $R_t$ will lie within the horizon radius of the black hole.
   Therefore it is believed in an ANG/QSO GRB rate due to the presently
   proposed process may dominate the tidal capture of star by the
   central black hole.
One might argue that there is no AGN/QSO
at the locations of GRB970228 and GRB970508 which are detected by BeppoSAX
therefore it is unlikely that GRBs are related to this class of object.
However, in order to locate the accurate position
the BeppoSAX is restricted to long duration GRBs. Popham, Woosley \&
Fryer (1998) show that only (BH, Hc) merger can produce long duration burst,
other mergers [e.g. (NS/BH, NS/BH)] will not produce long duration burst.
   It is important to
   note that the lifetime of AGN is typically of $10^8$ years,
   alternatively, the present paper proposed that at least some of
   GRBs may origin from the active nuclei due to the interaction between
   the star in cluster and accretion disk, roughly one percent of the
   observed GRBs.
In our model, only very low mass compact star and high mass RG binaries
can form (BH, Hc) mergers.
For a power law mass function, such binaries will be a very small fraction.
It is not too surprised not to identify any AGN/QSO with GRB970228 and
GRB970508 which are long duration bursts.
Interestingly there are two GRBs with small error box, in which AGN were found.
It was reported by Drinkwater et al (1997) that the possible X-ray
counterpart of GRB920501 is related with a Seyfert 1 galaxy at $z=0.315$.
Piro et al (1998) report that the first X-ray location of a $\gamma$-ray
burst by BeppoSAX (within $3^{\prime}$ radius) contains the
quasar 4C 49 with $z=1.038$. Finally, we want to point out that the basic
energy mechanism of gamma-ray bursts in our model are the same as those
proposed by other authors, namely GRBs are resulting from the mergers of
compact binaries, except the formation rate of the binaries and the location
of Gamma-ray bursts. Since our model burst rate is proportional to the metal
abundance (cf. eq. 39), we shall predict that if the GRBs can be identified
with AGNs/QSOs, these AGNs/QSOs must have high metal abundance.

\acknowledgements
The authors are grateful to the anonymous referee for his/her useful
comments on the surviving of formed binary in the dense star cluster
and other suggestions to improve the paper.
We thank Dr. R.Wijers for his useful comments and suggestions.
We are grateful to Prof. M.Veron for providing some information
of quasars, Prof. D.N.C. Lin for discussion about the interaction
between the main sequence stars and the accretion disk, Prof. R.E.
Taam for useful suggestions on the problems of spiral-in and the
capture of red giant stars, Prof. Z.W.Han for suggestions of the
stellar evolution, Prof. Z.G.Dai for the discussion of
gamma-ray bursts and Prof. M.A.Ruderman for suggestions and encouragement.
This work is initiated in a Neutron Star Workshop in Aspen Center
for Physics in 1995 and part of this work is supported by a RGC grant
of Hong Kong Government. JMW thanks the supports from the Climbing Plan of
the Ministry of Science and Technology of China and the National
Natural Science Foundation of China under grant No. 19803002.

redpajama_set_name: RedPajamaArXiv