"…Thank you for helping us design this project and for building it in such a way as to exceed our expectations. Throughout the project you and Mark were very considerate of the difference in opinions we had on design and materials, and diplomatically helped us reach decisions which led to a beautiful room. The gas fireplace and stone hearth turned out very well."
PINE CREEK ASSOCIATES: BUILDING AND REMODELING HOMES IN FAIRFIELD COUNTY AND BEYOND FOR OVER 25 YEARS.


Green House, Good Life: You Know That Feeling That You Left the Door Unlocked?
You Know That Feeling That You Left the Door Unlocked?
I have that feeling, except that instead of coming home to find out that I left the door unlocked for the day, today I came home to realize that I've basically left it unlocked for the last year and a half.
It's always been on our to-do list to check the screws in our exterior door hinges and strike plates. They come with puny 1"-ish screws that only attach the hardware to the door frames (which tend to be made of relatively soft wood), and it's wise to swap them out for 3" screws that go all the way into the studs. (Back in our condo, we had a neighbor whose door was kicked in. Fortunately, only a small stereo was stolen, but the door frame and trim were destroyed by the force of the kick, and they had to replace everything...not to mention the inconvenience of having a door that wouldn't lock for a day or two until they could replace the door, frame, and trim.) Since all of the force of a swift kick is concentrated on the strike plate, and the strike plate is only held in place by two screws, it's important that those screws are held in place by as much wood as possible. 3" screws are just the thing to go all the way through the studs.
I sort of hoped that the guys who installed our doors had swapped the screws out for longer ones, and we've been a little busy since we moved in, so checking on it just wasn't a priority. Today I finally got my hands on some 3" screws and finally got to work. When I took the first screw out of the first strike plate, it was about 3/4" long. Which is pretty much like going without locks altogether. Eek! (For people with relatively little worth stealing, we're really, really security-conscious, and this was a huge violation of our own policies....although we do have a pretty sophisticated alarm system.) Longer screws are way more secure.
As I'm sure you can imagine, swapping out the screws was really easy (why did we put it off so long?!).
It can be helpful to have a drill on hand to pre-drill the holes for the longer screws. Otherwise you might get screwdriver-hand (which, if you're not familiar, is similar to exam-hand and various other claw-hand maladies). It's most important to have 3" screws on the strike plate side, but we like to cover all of our bases and also use them on the hinge side, too.
You never cease to amaze me with your attention to detail. I NEVER would have thought about that. Would you please come inspect my house?
Never would have thought of that--good to know. I've always relied on living in a safe place, but in the end that will only get you so far. We're moving into a (sort of temporary) new-to-us house in the next week and will be replacing at least one of the doors before long--have to pay attention to that, and do so again when we build our own house in the next year or so.


Relationships sometimes overwhelm me. Of the many mysteries of life, lifelong bonds of friendship and love are to me the most mysterious of all.
When you form a special bond with someone – a friend who sticks with you through the ages, who's always there for you and you for him – that is special beyond words.
When you're separated by time or distance – not seeing or hearing from each other for years – and the stars align to bring you together again, it's as if nothing changed. Time and distance disappear in the magic of the moment.
And if there are friends for life, what of lovers?
There is nothing logical about the concept of love at first sight, or the notion that there is one true love out there for each of us. It makes no sense at all. There was a time when I would have laughed at such a ludicrous notion.
Until I laid eyes on a woman who made my heart soar. If you'd asked me that day if she could be the one – that we'd still be together nearly 30 years later – I would have said I don't believe in such things. But deep inside, I knew. And I wondered if she knew it too.
How does that sort of thing even happen? Is it just attraction? Hormones? Procreation?
If so, how could someone who rails against the very idea of one true love know in his heart that he has found her? And how could that same person – still disbelieving that silly idea – look back through the years and know in his heart that she was the one?
Though time and space have sometimes separated us, and joyous and tragic events have changed us, she remains the one. The only one. After all these years my heart still soars for that woman. And after all these years I still don't know what she sees in me. Of the many mysteries of life, that remains a mystery to me.
She is still a mystery to me.
Image credit Roel Wijnants whose Flickr album, Love and Friendship, inspired this poor-man's poetry.


text:
Iowa State Patrol: 1 man killed, 1 man injured in Hardin County crash
Updated: 9:38 PM CDT Sep 24, 2021
A SPENCER MAN IS DEAD - AND ANOTHER MAN IN T HE HOSPITAL TONIGHT - AFTER A CRASH IN HARDIN COUNTY. IN HAPPENED AT 10-0 3 MORNING ON HIGHWAY 20 - NEAR MILE MARKER 1-69. THE IOWA STATE PATROL SAYS A PICK-UP DRIVEN BY 18-YEAR-OLD ALEXZANDER PURMAN OF ELDEKAR CROSSED THE MEDIAN AND HIT AN S-U-V HEAD ON. 61-YEAR-OLD BRN YA HARKEN OF SPENCER WAS DRIVING THE SUV - HE
A Spencer man died and another man was injured after a crash in Hardin County on Friday morning. The Iowa State Patrol said it happened at about 10:30 a.m. on Highway 20 near mile marker 169. The Iowa State Patrol said a pick-up driven by 18-year-old Alexzander Purman, of Elkader, crossed the median and hit an SUV head-on. Bryan Harkin, 61, who was driving the SUV was killed in the crash.Purman was taken by air ambulance to MercyOne in Des Moines.
HARDIN COUNTY, Iowa —
A Spencer man died and another man was injured after a crash in Hardin County on Friday morning.
The Iowa State Patrol said it happened at about 10:30 a.m. on Highway 20 near mile marker 169.
The Iowa State Patrol said a pick-up driven by 18-year-old Alexzander Purman, of Elkader, crossed the median and hit an SUV head-on.
Bryan Harkin, 61, who was driving the SUV was killed in the crash.
Purman was taken by air ambulance to MercyOne in Des Moines.

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: Size of sample data to conduct FFFT in JTransforms I am working on get frequency of the audio data on a phone. I am using Jtransforms to conduct the FFT on sample data to get the result. But I am not sure how to set the sample data array size.

*

*The hardware sample rate is 44100. My understanding is I can only get the frequency lower than 44100/2

*How should I set the FFT_Size, bufferSize in the code below, if I want to get the full range of frequency result 0~44100/2.

*When I get the result from realForward. How can I interpret the result into frequency magnitude inside a certain range(e.g. 5khz)?
recorder.read(audioData,0,bufferSize);
DoubleFFT_1D fft = new DoubleFFT_1D(FFT_Size);
fft.realForward(audioData);

Thank you very much for you time.

A: Given a particular sampling rate R, the results of an FFT can be thought of as a histogram of energy present in different frequency bands, ranging from -R/2 to R/2 Hz. So, for a 44100 Hz sampling rate, your frequency histogram ranges from -22050 Hz to 22050 Hz. The number of samples you input to the FFT is the number of bins that are output. So, if you input 1024 samples, you will have 1024 histogram bins between -22050 Hz and 22050 Hz, or 44100/1024 (about 430) Hz per bin. If you want resolution of 5000 Hz, you really only need about 9 samples.
Converting from the (real, imaginary) complex number format to (frequency, magnitude) is the same as converting from rectangular (complex) to polar (freq/mag) coordinates.

redpajama_set_name: RedPajamaStackExchange


Dual-registration deals have been agreed for Bath Rugby Academy players Richard Lane and Will Homer with Cornish Pirates this season.
Both players are likely to feature in upcoming British & Irish Cup matches for Pirates, who play in the Greene King IPA Championship.
Lane, who can play at wing and fullback, has made nine appearances for Bath's first team since joining the Academy two seasons ago.
Scrum-half Homer has featured for England U16 and U18 and has been an age group player at Bath Rugby for the past five seasons. He has already featured heavily in this year's Aviva A League campaign with Bath United.
Academy loosehead prop Beno Obano will continue his loan spell at Coventry RFC in National League One.


Hans Jansen is the Strategy Advisor at the National Library of the Netherlands. He has previously worked as the Director of International Relations and Head of Research at the National Library of the Netherlands. Over the past twenty years he has been involved in numerous national and European projects in the library field. Topics vary from digital preservation solutions to use of linked open data, development of services for digital humanities to innovations in the public library sector. He was in charge of a large renovation programme for the library.


text:
Bill Gates Quits Microsoft Chairman, Satya Nadela Replaces Steve Balmer as New CEO
By Young Kim ( [email protected] ) Feb 05, 2014 03:42 PM EST Comment
Satya Nadella, executive vice president of Microsoft's Cloud and Enterprise group, is seen in this undated Microsoft handout photograph released on February 4, 2014. REUTERS/Microsoft/Handout via Reuters
Steve Balmer has stepped down from his position as Chief Executive Officer, handing his role over to Satya Nadella and making him a member of the board of Directors effective Feb. 4. Nadella is the third CEO of Microsoft.
"Satya is a proven leader. He's got strong technical skills and great business insights," Balmer wrote in an email. "He has a remarkable ability to see what's going on in the market, to sense opportunity, and to really understand how we come together at Microsoft to execute against those opportunities in a collaborative way. I have worked closely with Satya for many years and I have seen these skills many times. He is not alone, though. Our Senior Leadership Team has never been stronger, and together this group will drive us forward."
Nadella, who has been working for Microsoft for 22 years, previously held the position of Executive Vice President of Microsoft's Cloud and Enterprise group. Nadella has played a major role in the company's move to using the cloud (a large network of computers connected through a communication network like the internet) and developing a cloud infrastructure that supports Bing, Xbox, Office, and other services.
"During this time of transformation, there is no better person to lead Microsoft than Satya Nadella," said Microsoft Founder and Board of Directors member Bill Gates. "Satya is a proven leader with hard-core engineering skills, business vision and the ability to bring people together. His vision for how technology will be used and experienced around the world is exactly what Microsoft needs as the company enters its next chapter of expanded product innovation and growth."
On the other hand, Bill Gates removed himself from the Chairman of the Board of Directors and has taken on a new role on the Board as Founder and Technology Advisor. For the past couple years, Bill Gates has turned his attention more towards humanitarian work and philanthropy alongside his wife through the Bill and Melinda Gates Foundation. He still will be involved with Microsoft, supporting Nadella in shaping and marketing the new technology and products.
"I'll have over a third of my time available to meet with product groups and it will be fun to find these next round of products working together," Gates said in a new video. "So there's a lot of opportunities in front of us and it's exciting that we have a strong leader to take us there."
John Thompson, lead independent director for the Board of Directors, will take over Gates' position as Chairman of the Board of Directors while resuming his previous position.
"Satya is clearly the best person to lead Microsoft, and he has the unanimous support of our Board," Thompson said. "The Board took the thoughtful approach that our shareholders, customers, partners and employees expected and deserved."
Nadella, born in India, is taking over Microsoft at a critical period. Many consumers and businesses have favored handheld devices produced by rival companies such as Apple Inc. over PCs. Microsoft's change in direction follows the worst decline on record for PCs in 2013. Shipments fell 10 percent and are expected to worsen through 2017. Before 2004, Microsoft's revenue growth averaged 24 percent; however, for the last 10 years it has only averaged 9.4 percent.
Not only will Nadella have to play catchup with Apple Inc. and Google Inc., he will be making strategy changes, which includes the $7.2 billion integration of Nokia's Oyj's handset product and turning Microsoft into a service and hardware provider.
"Microsoft is one of those rare companies to have truly revolutionized the world through technology, and I couldn't be more honored to have been chosen to lead the company," Nadella said. "The opportunity ahead for Microsoft is vast, but to seize it, we must focus clearly, move faster and continue to transform. A big part of my job is to accelerate our ability to bring innovative products to our customers more quickly."
Ron Johnson, Man Who Created Apple Store with Steve Jobs, to Talk Faith and Work
'I Can Only Imagine' Film Being Used by God to Bring Gospel to China, Reveals Director
Interview: Billionaire Walter Wang on Family, Career, Kingdom of God, Part II
Interview: Billionaire Walter Wang on Family, Career, Kingdom of God, Part I
Transportation Secretary Foxx and Google's Schmidt Try the Self-Driving Car While New Report Confirms Hot Economy in Silicon Valley


This apartment of 63,51 m² (about 683 ft²) contains 3 rooms including 2 bedrooms, 1 shower room and 1 toilet. It is equipped with a fitted and with a cellar. It's located on the 3rd floor. Heating : individual gaz. Others : intercom.


text:
Musée d'Orsay Welcomes Instagram Artist-in-Residence
By Manuel Charr
The world-famous Musée d'Orsay has announced that they have hired an Instagram artist-in-residence with the aim of bringing more attention to many of the masterpieces it has in its collection. Rather fittingly, the museum has decided that the works of many of deceased artists it has in its ownership can be boosted by using the most visually-centred of all social media sites, Instagram.
Of course, promoting a public institution with a social media account is nothing new. That said, the fact that the Musée d'Orsay welcomes an Instagram artist-in-residence to boost its public profile is an interesting move. This is because the appointment of Jean-Philippe Delhomme as the gallery's artist-in-residence will mean he is given complete artistic control over the Paris-based institution's official Instagram account. He will take charge of it every Monday over the course of the entire year to do exactly as he pleases.
A post shared by Musée d'Orsay (@museeorsay) on Jan 6, 2020 at 8:00am PST
Artistic Freedom to Reimagine Celebrated Artists
The idea of the project – at its outset, at least – is that Delhomme will post an illustration once a week that will show the gallery's collection in a new light. Delhomme began in January by depicting the nineteenth-century French art critic and writer, J K Huysmans, in a hand-drawn sketch. In it, the illustrator – who has worked extensively for publications like the New Yorker and UK Vogue in the past – imagines how Huysmans would have responded to a fictitious Instagram post to pay tribute to Edgar Degas and another contemporary, the impressionist painter J L Forain.
The post is the first this year but it already marks out the way in which Delhomme plans to operate as the museum's virtual artist-in-residence. "The concept is to think about what it would have been like if late nineteenth-century artists had been on social media," Delhomme said. The illustrator, who splits his time between the United States and France, went on to add that he was approaching the project by imagining how some of the artists who are in the collection of the Musée d'Orsay would behave if they had had their own Instagram accounts when alive. According to him, the idea is to make some of these artists seem more like real people to today's audience.
The artist-in-residence has already indicated that he will explore the imagined social media interactions of artists from the early twentieth century, too, such as Henri Matisse and Pablo Picasso. However, it is not yet known how Delhomme may develop his ideas as the project progresses. Which artists he will reimagine as social media operators and which works in the museum's collection he will choose to draw attention to remain open questions. That said, the illustrator, who is well-known for his artwork for the GQ column 'The Style Guy', has already gone on the record to state that he will only focus on artists that he finds inspiring. Delhomme indicated that painters such as Renoir, Manet and Vuillard could all be given the Instagram treatment whilst he is artist-in-residence at the gallery.
Promoting the Gallery Through Artistic Personalities
Le Figaro, one of France's most respected national newspapers, reported that the president of the Musée d'Orsay, Laurence des Cars, has approved of the twenty-first-century initiative. According to des Cars, welcoming an artist-in-residence to the gallery meant that artists from a hundred or so years ago would be brought closer to the public by "enrolling them in today's interactions." The president was also reported as saying that the residency of Delhomme should not be seen as trivialising or undermining some of the great works in the museum's collection. "Rather [it should]… draw attention to a particular moment in an artist's life," he claimed.
Des Cars said that he thought this would typically involve discussing the novelty of a new type of artwork or the way in which artists operating in the nineteenth-century would have interacted with one another. "Whether the comments are fictitious or not, they ought to evoke the loyalties or antagonisms that were aroused at the time," he added.
Boosting the Museum's Social Media Presence
Although there is a great deal of artistry in the way in which the Musée d'Orsay has chosen to run its online artist-in-residency scheme, there can be little doubt that the idea is to gain more attention in a competitive field. At the start of 2020, the gallery had just under 830,000 followers on Instagram. By contrast, the Louvre, a Parisian gallery that posts on a daily basis about works of art in its collection, has well over four times that amount. Indeed, Centre Pompidou, also in the French capital, has in excess of a million followers on Instagram. As such, Delhomme's success as an artist-in-residence is likely to be judged not only from his creativity with the museum's Instagram account but by the number of new followers he can attract to it.
MuseumNext
+ Find Out More
About the author – Manuel Charr
Manuel Charr is a journalist working in the arts and cultural sectors. With a background in marketing, Manuel is drawn to arts organizations which are prepared to try inventive ways to reach new audiences.
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Jason Scott is an American archivist, historian of technology, and filmmaker. He is the creator, owner and maintainer of textfiles.com, a web site which archives...
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Jasper Visser sits down with Dr Tristram Hunt, Director of V&A at MuseumNext London in June 2019 to talk about the expansion of the V&A,...


text:
Children's Corner, Prospect Park
Independence Day at Prospect Park
Wednesday, July 4 , 12 pm – 5 pm, 2018
Join Prospect Park Alliance on Independence Day for special family programming at the Prospect Park Audubon Center, 1912 Carousel and Lefferts Historic House! During this full day celebration, commemorate two Independence Days, America's independence from England in 1776 and the emancipation of enslaved African-Americans in New York in 1827.
Let us know if you are coming!
Nature Exploration, 12–4 pm
Prospect Park Audubon Center, Free
Join Prospect Park Alliance for nature education programs at the Prospect Park Audubon Center, the first urban Audubon Center in the nation.
Discovery Pack, 12–3 pm: Prospect Park Alliance invites you to get inspired by nature with our Discovery Packs, ready-to-go kits filled with nature activities for families.
Bird Nerd Game Hour, 1–2 pm: Learn about birds and nature in this fun, mildly competitive hour of puzzles, Bingo, card games, and more!
Animal Encounter, 2–3 pm: Join Alliance Naturalists in learning more about the animals in the Audubon Center's collection. This program starts promptly at 2 pm
Nature on the Go!, 3–4 pm: An Alliance Naturalist will lead children and families to areas near the Audubon Center, where you can learn about the nature that is all around us. This program leaves promptly at 3 pm.
Independence Day Celebration, 1 pm–4 pm
Lefferts Historic House, $3 suggested donation
Join Prospect Park Alliance in celebrating two Independence Days, America's independence from England in 1776 and the emancipation of enslaved African-Americans in New York in 1827. View historic articles published by African American newspapers, and look extra patriotic as you make yourself a plumed hat, similar to those worn by parade goers celebrating this momentus occasion. Then, sign your own "John Hancock" on a reproduction of the Declaration of Independence.
Carousel Rides, 12–5 pm
Children's Corner, $2.50 per ride, $11.50 for a book of 5 tickets, free with Prospect Park Alliance Family Supporter membership
Celebrate with a ride on the Park's beloved 1912 carousel. Join the Alliance at the $150 level and your family (up to 4 people) will receive unlimited rides on the Carousel for a full year!
Free, RSVP!
Audubon Center, Free, Kids, Lefferts Historic House, Nature Programs
Bartel-Pritchard Square
Wednesday Greenmarket at Bartel-Pritchard Square
Wednesday, July 4 , 8 am – 3 pm, 2016
Nestled inside Prospect Park's tree-shaded southwest corner, this much-loved market, occurring every Sunday and Wednesday, is where South Slope and Windsor Terrace residents stock up on locally grown staples. The offerings range from a selection of vegetables, fruits, baked goods, plants, and flowers, to fresh-caught fish and organic baked goods. For a full calendar of events and a list of sellers, visit the GrowNYC website.
This Greenmarket at Bartel-Pritchard Square is also open on Sundays, 9 am–3 pm, May 5 through December 22.
Note: The Greenmarket will be closed on December 25, 2019 and January 1, 2020.
Tennis House
Prospect Park Alliance Wednesday Woodland Corps - Introductory Session
Wednesday, July 4 , 10 am – 1 pm, 2018
Register online or call (718) 287-3400 for more information.
Join Prospect Park Alliance the first Wednesday of each month for this introduction to the Wednesday Woodland Corps, a dedicated team of volunteers who care for the Park's 250 acres of forest. The Woodland Corps assist with fence repair + maintenance, woodland trash pickup, invasive plant removal, planting, mulching, and other woodland related tasks. Volunteers who have attended an Introductory Session may attend additional Wednesday Woodland Corps events throughout each month.
Free, Volunteer
The Means of a Ready Escape: Brooklyn's Prospect Park
All Day, Wednesday, July 4, 2018
On view daily through February 10, 2019.
In celebration of the 150th anniversary of Prospect Park, Brooklyn Historical Society and Prospect Park Alliance present an exhibition that celebrates the founding vision of the Park, traces its social and historical trajectories, and examines the important role that Prospect Park has played as "Brooklyn's Backyard" for 150 years.
The Brooklyn Historical Society is closed on major holidays.
Visit the Brooklyn Historical Society website for hours of operation.
Citizens Creating Parks


text:
NNews
News / SC Collegium defers decision on Justice K M Joseph's elevation
SC Collegium defers decision on Justice K M Joseph's elevation
7:05 PM, 2 May 2018
The Supreme Court Collegium today deferred a decision on the issue of reconsidering its recommendation to elevate Uttarakhand Chief Justice K M Joseph as the judge of the apex court, after it was sent back by the government last week. The five member Collegium comprising Chief Justice Dipak Misra and justices J Chelameswar, Ranjan Gogoi, Madan B Lokur and Kurian Joseph met after the top court's working hours, but no decision was taken.
Besides Justice Jospeph, the agenda of the Collegium was to deliberate on the names of some judges from Calcutta, Rajasthan and Telangana & Andhra Pradesh High Courts for elevation as apex court judges. The resolution of the meeting uploaded on the apex court website said the Collegium had met "to consider the following agenda:'To reconsider the case of Mr Justice K.M. Joseph, Chief Justice, Uttarakhand High Court [Parent High Court:Kerala], pursuant to letters dated April 26 and 30, 2018 received from Ministry of Law & Justice, Government of India and also to consider the names of Judges from Calcutta, Rajasthan, and Telangana & Andhra Pradesh High Courts for elevation as Judges of the Supreme Court, in view of the concept of fair representation. Deferred," the resolution said.
Justice Chelameswar, who had not attended the court today, came for the collegium meeting. There was no official word on when the Collegium would meet next. Justice Joseph's name was recommended along with then senior advocate Indu Malhotra on January 10 for their elevation as apex court judges. The government had on April 26 declined to accept the recommendation of the Collegium and asked it to reconsider Justice Joseph's name. Malhotra was sworn in as the judge of the apex court on April 27.
Justice K M Joseph, who had headed the bench that had quashed the Narendra Modi government's decision to impose President's rule in the Congress-ruled hill state in 2016, was not considered to be elevated as a Supreme Court judge by the Center. The government had said that the proposal for his name was not in accordance with the top court's parameters and there was adequate representation of Kerala in the higher judiciary from where he hails.
His seniority was also questioned by the Center which had said "he stands at Sl. No.45 in the combined seniority of High Court Judges on all-India basis." Justice Joseph, who turns 60 this June, has been the Chief Justice of the Uttarakhand High Court since July 2014. He was appointed a permanent judge of the Kerala High Court on October 14, 2004 and assumed charge of the Uttarakhand High Court on July 31, 2014. The members of the collegium including Justices Chelameswar, Gogoi, Lokur and Kurian Joseph had expressed concern over the delay of the government in clearing the name of the Uttarakhand Chief Justice as the apex court judge.
Notwithstanding the letters written by the collegium members to the CJI which had come into the public domain, the Centre disregarded the recommendation about Justice Joseph.
Chief Justice Dipak Misra, collegium, K M Joseph, Supreme Court


Billy Graham is an ordained Southern Baptist preacher whose career is principally known because of a series of more than 400 "Crusades" in 185 countries between 1947 and 2005. Beginning with circus tents set up in parking lots, he eventually filled stadiums with tens-of-thousands of interested listeners. The largest Crusade attracted more than a million people to one service. Many of his Crusades were broadcast on television. He hosted a radio show, Hour of Decision, from 1950 to 1954. In October 1989 Graham became the only functioning minister to have a star on the Hollywood Walk of Fame.
Graham was widely recognized and a popular Evangelical minister who has been one of the "most admired men" in America for 55 years. He would end Crusades with an invitation for any who felt convicted and wanted to "accept Jesus Christ as your personal savior" to publicly come forward. Thousands responded to his invitation.
Graham was an adviser to several US Presidents, including Dwight Eisenhower, Lyndon Johnson and Richard Nixon, and has met with many Presidents from Harry Truman to Barack Obama. He was friends with Martin Luther King, and once paid for his bail to free him in 1963 after his arrest for participation in a Civil Rights demonstration. King and Graham preached together on several occasions, at Graham's invitation.
Graham was regarded as America's Protestant patriarch, providing a Christian conscience to the nation. He also organized and supported evangelism worldwide. He supported training conferences to increase the evangelical presence in many nations.
Though still living, Graham has suffered from Parkinson's disease since 1992 which led to his retirement because of failing health.
Today is not a day to mourn his passing, but to respect and appreciate his life's work.


text:
\section{Introduction}
\label{sec:intro}

The double-peak structure of blazar spectra is well modeled with
leptonic models
\citep[e.g.][]{ghi85,der93,sik94,tav98,bot00,kin02,cel08,bot13}.
In the leptonic models, gamma-ray emission is
generated via inverse Compton (IC) scattering.
The synchrotron-self Compton (SSC) process up-scatters
synchrotron photons produced by the same electron population
in jets \citep[e.g.][]{mar92}.
Since Flat Spectrum Radio Quasars (FSRQs) have more luminous disk, external photons surrounding
the disk dominate the seed photons for the IC scattering \citep[e.g.][]{sik94}.
In most models, the non-thermal electrons are assumed to be accelerated
via shocks with the Fermi process.
However, there are several unsolved problems in the particle acceleration
mechanism in blazars.
Some blazar spectra imply that the electron power-law index is smaller
than 2, the value from the simplest shock acceleration model.
The change of the index at the spectral break is
very large inconsistently with the cooling break \citep[see e.g.][]{hay12,yan14}.
To reproduce the curved photon spectra, an emission model requires an
electron energy distribution with many phenomenological parameters,
such as a double-broken power-law with a low-energy cutoff
\citep[e.g.][]{abd11}.

The maximum electron energy in blazars is much smaller than
the value implied from the Bohm limit \citep{ino96}.
The acceleration timescale in blazars
seems to be very long compared to the timescale of the shock acceleration
considered in supernova remnants \citep{aha99} or pulsar wind nebulae \citep{ato96}.

Also from the theoretical point of view, the shock acceleration in blazars
has difficulties.
To dissipate significant kinetic energy consistently with
blazar luminosity, a relativistic shock is favored.
However, a relativistic shock tends to become superluminal
\citep{kir89}, where electrons moving along the magnetic field
in the downstream cannot return to the upstream
so that the shock acceleration is inhibited \citep{sir15}.
Furthermore, the shock acceleration can operate only in weakly
magnetized plasma \citep{lem11}, which may contradict
the magnetization implied from the spectral modeling \citep[e.g.][]{tav98,hay15}.
This is because, for a relativistic shocks propagating in a marginally magnetized plasma,
the turbulence in the upstream as the shock precursor is hard to be excited by the particles
reflected from the shock front.
The absent of the precursor turbulence in the upstream prohibits electrons
from returning to the downstream.

As for the spectral hardness in the shock acceleration theory,
the nonlinear effect of the cosmic-ray pressure may modify the shock structure
and harden the electron spectrum \citep{mal01}.
However, a Monte Carlo simulation by \citet{ell13}
shows that the nonlinear effect of the cosmic-ray
on the shock structure weakens, and the acceleration efficiency
is also suppressed, as the shock speed
becomes relativistic.

An alternative candidate of acceleration mechanism
is the stochastic acceleration by turbulence \citep[e.g.][]{sch84,par95,bec06,cho06,sta08},
which is phenomenologically equivalent to the second-order Fermi acceleration.
The required turbulence may be excited by Kelvin--Helmholtz instability \citep{ros08}
at the boundary of the spine--sheath structure \citep{ghi05},
Rayleigh--Taylor and Richtmyer--Meshkov instabilities in the transverse jet structure
\citep{mat13}, kink instability \citep{bro16}, tearing mode instability \citep{sir14},
or the star--jet interaction \citep{bar12}.

The turbulence acceleration is slower process than the shock acceleration.
In addition, this process can produce a hard electron spectrum
with an index smaller than 2.
Given the energy diffusion coefficient $D_{\varepsilon \varepsilon} \propto \varepsilon^q$,
the number spectrum in the steady state without the escape effect
is proportional to $\varepsilon^{1-q}$, where $\varepsilon$ is the particle energy.
If the particle scattering is dominated by the gyro-resonant scattering with
turbulent waves,
the power-law index $q$ in $D_{\varepsilon \varepsilon}$ is determined
by the magnetic wave spectrum as $\delta B^2(k) \propto k^{-q}$
\citep{bla87}.

The turbulent acceleration model has been adopted to blazars
by many authors \citep[e.g.][]{bot99,sch00,kak15,asa14,asa15}.
However, \citet{kak15} shows that a very extreme parameter set,
such as tiny emission region,
is required to reproduce the spectra of Mrk 421 and Mrk 501
by the steady state one-zone model.
The results in \citet{kak15} imply that the steady
state of the electron energy distribution is hard to be realized
by the balance among the turbulence acceleration, injection,
cooling, and escape of electrons.
In the slow acceleration process,
the temporal evolution of the electron energy density along the jet
is essential to discuss the resultant photon spectrum.
Adopting the Kolmogorov index ($q=5/3$), \citet{asa14} shows
that a model taking into account the radial evolution of the
electron energy distribution reconciles the observed spectrum of Mrk 421,
but the model in \citet{asa14} requires a non-trivial evolution
of the electron injection rate.

On the other hand, the model in \citet{asa15} succeeds in reproducing
the spectra for both the steady and flare states of 3C 279
with a simple assumption and the hard-sphere index $q=2$,
with which the acceleration
timescale is independent of the particle energy.

In this paper, we pursue the hard-sphere-like acceleration in blazars
by fitting spectra of five representative blazars, Mrk 421, 1ES 1959+650,
PKS 2155-304, 3C 279 and PKS 1510-080, taking into account the radial evolution
of the electron energy distribution.
The sample consists of both types of blazars, BL Lac objects
and FSRQs.
Blazars emission often shows strong variability.
Thanks to recent improvements of observational instruments,
broad-band data from contemporaneous observations become available
not only in high-flux flaring states but also in general steady states of the blazars.
We demonstrate that the broad-band spectra of those blazars
in the steady states are reproduced with the hard-sphere-like acceleration model
with a small number of parameters.

In \S \ref{sec:meth}, we explain our model and method to
produce model spectra.
The results for several blazars are summarized in \S \ref{sec:res}.
\S \ref{sec:dis} is devoted to discuss the implication
for the acceleration mechanism in blazars.

\section{Method}
\label{sec:meth}

In this paper, the steady state photon spectrum is calculated
by the numerical code in \citet{asa14}
\citep[see also,][]{asa15}.
To explain the model parameters summarized in Table \ref{param_tab},
we shortly review the calculation method below.
The steady emission from a blazar is modeled with a steady
outflowing jet, for which we consider continuous shell ejection
from the initial radius $R_0$.
Although a conical jet with an opening angle
of $1/\Gamma$ is assumed to calculate the emission,
where $\Gamma$ is the bulk Lorentz factor of the jet,
the electron injection rate $\dot{N}'$ is normalized
by a spherically-equivalent volume,
\begin{equation}
V'_0=4 \pi R_0^3/\Gamma,
\end{equation}
at $R=R_0$. Hereafter, we denote values in the comoving frame
by prime characters.
The volume expands as $V' \propto R^2$ for the conical geometry.
The electron injection rate into the above reference volume $\dot{N}'$
is assumed as constant during the expansion timescale.
Then, the injection rate density behaves as
$\dot{n}'=\dot{N}'/V' \propto R^{-2}$ from $R=R_0$ to $2 R_0$.
The electron injection is monoenergetic with an initial
Lorentz factor of $\gamma'_{\rm inj}$.
We have confirmed that a power-law injection
yields a harder electron spectrum than the examples
in this paper. Since our purpose is to yield a soft spectrum
with the turbulence acceleration model,
we assume the monoenergetic injection.

The particle acceleration by turbulences
is regulated by the energy diffusion coefficient,
\begin{equation}
D'_{\varepsilon \varepsilon}=K \varepsilon'^2_{\rm e},
\label{difdif}
\end{equation}
where $\varepsilon'_{\rm e}$ is the electron energy.
In this paper, we consider only the hard-sphere type
acceleration as defined in equation (\ref{difdif}).
The parameter $K$ is constant for $R \leq 2 R_0$.

The radial evolution of the electron energy distribution
is calculated taking into account the electron injection,
turbulence acceleration, radiative cooling, and adiabatic cooling.
For $R > 2 R_0$ the injection and energy diffusion shut down.
Our numerical code follows the evolution of the electron energy distribution
and photon production as far as $R=R_{\rm out}$.
The synchrotron emissivity and self-absorption are calculated
with the magnetic field evolving as
\begin{eqnarray}
B'=B_0 \left( \frac{R}{R_0} \right)^{-1},
\end{eqnarray}
where $B_0$ is the initial value.

In addition to SSC,
IC emission due to the external photon field (EIC)
is calculated for FSRQs.
The models for the external photon fields are the same as discussed in \citet{hay12}
with the broad line emission and the infrared dust emission.
When the broad line region (BLR) is considered as the external photon source,
the energy density is written as
\begin{eqnarray}
U'_{\rm UV}=\frac{0.1 \Gamma^2 L_{\rm D}}{3 \pi c R^2_{\rm BLR} (1+(R/R_{\rm BLR})^3)},
\end{eqnarray}
where
$L_{\rm D}$ is the disk luminosity, and
the size of BLR is described as
\begin{eqnarray}
R_{\rm BLR}=0.1 \left( \frac{L_{\rm D}}{10^{46}~\mbox{erg}~\mbox{s}^{-1}} \right)^{1/2}~\mbox{pc}.
\end{eqnarray}
The external photon spectrum from BLR is approximated by the diluted Planck distribution
with photon temperature of
\begin{eqnarray}
T'_{\rm UV}=10 \Gamma~\mbox{eV}.
\end{eqnarray}

The infrared dust emission is an alternative source of the external photon field
for a relatively larger $R_0$.
In this case, we adopt a steeply dropping function as
\begin{eqnarray}
U'_{\rm IR}=\frac{0.1 \Gamma^2 L_{\rm D}}{3 \pi c R^2_{\rm IR} (1+(R/R_{\rm IR})^4)}.
\end{eqnarray}
The parameters in this case are expressed as
\begin{eqnarray}
R_{\rm IR}&=&2.5 \left( \frac{L_{\rm D}}{10^{46}~\mbox{erg}~\mbox{s}^{-1}} \right)^{1/2}~\mbox{pc},\\
T'_{\rm IR}&=&0.3 \Gamma~\mbox{eV}.
\end{eqnarray}

In summary, the model parameters are $\Gamma$, $R_0$, $B_0$, $\gamma'_{\rm inj}$, $K$,
$R_{\rm out}$, and $L_{\rm D}$.
The shape of the electron spectrum is adjusted by only the diffusion coefficient
$K$ and the cooling effect.
The conically expanding outflow in this model seems reasonable and simplest
assumption. We do not need to put an additional parameter for particle escape.
The adiabatic cooling effect suppresses the emission at $R \gg R_0$,
so that the steady outflow results in a steady emission without the escape effect.

\section{Results}
\label{sec:res}

\begin{table*}[!hbtp]
	\caption{Model parameters}
	\begin{center}
		\begin{tabular}{lcccccccccc}
			\hline\hline
			 & & $\gamma'_{\rm inj}$ & $R_0$ & $R_{\rm out}/R_0$ & $\Gamma$ & $B_0$  & $K$ & $\dot{N}'$ & $L_{\rm D}$ & UV/IR \\
			 & & & cm & & & G & $\mbox{s}^{-1}$ & $\mbox{s}^{-1}$ & erg $\mbox{s}^{-1}$ & \\
			\hline
			Mrk 421 & A &  10 & $1.5 \times 10^{17}$ & 30 & 15 & 0.18 & $4.8 \times 10^{-6}$ & $2.4 \times 10^{47}$ & --- & --- \\
			 & B &  100 & $1.5 \times 10^{17}$ & 30 & 15 & 0.16 & $3.7 \times 10^{-6}$ & $9.8 \times 10^{46}$ & --- & --- \\
            \hline
			1ES 1959+650 & A & 100 & $1.6 \times 10^{17}$ & 30 & 20 & 0.18 & $5.0 \times 10^{-6}$ & $3.7 \times 10^{46}$ & --- & --- \\
			 & B & 100 & $1.6 \times 10^{17}$ & 10 & 20 & 0.18 & $5.0 \times 10^{-6}$ & $3.7 \times 10^{46}$ & --- & --- \\
			 & C & 10 & $4.0 \times 10^{16}$ & 30 & 40 & 0.5 & $4.3 \times 10^{-5}$ & $1.5 \times 10^{47}$ & --- & --- \\
			\hline
			PKS 2155--304 &   & 10 & $6.0 \times 10^{16}$ & 30 & 20 & 1.2 & $1.2 \times 10^{-5}$ & $1.5 \times 10^{48}$ & --- & --- \\
			\hline
			3C 279 &   & 10 & $7.1 \times 10^{16}$ & 30 & 15 & 8.0 & $9.5 \times 10^{-6}$ & $7.3 \times 10^{49}$ & $6.0 \times 10^{45}$ & UV \\
			\hline
			PKS 1510--089 &   & 10 & $6.0 \times 10^{17}$ & 30 & 20 & 0.38 & $9.0 \times 10^{-7}$ & $7.3 \times 10^{49}$ & $5.0 \times 10^{45}$ & IR \\
			\hline\hline
		\end{tabular}
	\end{center}
	\label{param_tab}
\end{table*}

We select several spectral data for the blazars in non-flaring states.
The model parameters we obtained
are summarized in Table \ref{param_tab}.
In all the cases, the acceleration timescale $K^{-1}$
is comparable to the dynamical timescale $R_0/(\Gamma c)$.
A slight difference in $K$ results in a drastic change
of the resultant photon spectrum.
Below we discuss the individual cases.

\subsection{Mrk 421}
\label{sec:Mrk421}

First, we discuss a famous BL Lac object Mrk 421
(redshift $z=0.031$)
based on the spectrum of the 4.5 month long multifrequency
campaign \citep{abd11}.
For this data set, \citet{asa14} and \citet{kak15} have already
fitted the spectrum with turbulence acceleration models.
The steady one-zone model of \citet{kak15} requires
a nontrivial energy-dependence of the diffusion coefficient,
$D'_{\varepsilon \varepsilon} \propto \varepsilon'^{1.85}_{\rm e}$,
and very small region ($\sim 10^{14}$ cm) to make electrons escape
faster.
On the other hand, the model in \citet{asa14} is the same as
the model in this paper, but the diffusion coefficient
was assumed as the Kolmogorov type,
$D'_{\varepsilon \varepsilon} \propto \varepsilon'^{5/3}_{\rm e}$.
To reproduce the broad photon spectrum,
a rapid evolution of the particle injection with radius
was required.
In this section, we demonstrate that the hard-sphere model
can reproduce the spectrum even with a constant injection rate.
The macroscopic parameters $R_0$ and $\Gamma$ in our model
roughly agree with the values in the original work on the campaign data \citep{abd11}.
The variability timescale $\sim R_0/\Gamma^2$ corresponds
to about $0.3$ day.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f1.eps}
\caption{Evolutions of the energy distribution of the electron density
in the model A for Mrk 421.}
\label{Ele}
\end{figure}

Figure \ref{Ele} shows the radial evolution of the electron energy
distribution for model A (see Table \ref{param_tab}).
Here, we inject electrons with the initial Lorentz factor $\gamma'_{\rm inj}=10$.
In the hard-sphere case, the electron energy distribution
is sensitive to the ratio of the acceleration timescale $K^{-1}$
to the elapsed time $t'$ as analytically demonstrated in \citet{asa16}.
The energy injected from turbulence grows exponentially
as $\propto \exp{(Kt')}$ for $Kt' \geq 1$.
In the low-energy part above $\gamma'_{\rm inj} m_{\rm e} c^2$,
the spectrum can be approximated as a power-law of $n'(\varepsilon'_{\rm e})
\propto \varepsilon'^{-1}_{\rm e}$.
The spectral shape around the peak is curved, which is characteristic
for the stochastic acceleration.
After the shutdown of the electron acceleration and injection
($R>2R_0$), we can see that the adiabatic cooling effect shifts
the spectral shape to lower energy.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f2.eps}
\caption{Model photon spectra A (red) and B (blue) for Mrk 421.
The observed data points are partially extracted from the data of the 4.5 month
campaign \citep{abd11}.}
\label{Mrk421}
\end{figure}

Owing to the curved electron spectrum and its radial evolution,
the curved spectrum for Mrk 421 is well reproduced even from radio
to gamma-ray as shown by the red line in Figure \ref{Mrk421}.
The synchrotron spectrum is broad enough to agree with the observation
differently from the Kolmogorov case in \citet{asa14}.
Although the radio data seems on the extrapolation from the optical/IR data,
the radio emission has been neglected as another component
in the previous models \citep[e.g.,][]{tra09,abd11},
in which absorption due to synchrotron self-absorption
is crucial in the radio band.
Owing to the hard electron spectrum in our model,
the emission region is optically thin even for radio emission.

Here, we also test model B (blue), in which
$\gamma'_{\rm inj}$ is higher.
Even for a different value of $\gamma'_{\rm inj}$,
which is highly uncertain, a slight change of the other parameters
produces a quite similar spectrum.
As shown in Figure \ref{Mrk421}, a higher $\gamma'_{\rm inj}$
tends to produce a slightly narrower spectrum.

\subsection{1ES 1959+650}
\label{sec:1ES1959}

1ES 1959+650 ($z=0.047$) is categorized as a high-frequency peaked BL
Lac object (HBL) and one of the most frequently observed TeV gamma-ray
blazars. Here we focus on a multi-wavelength campaign conducted during
a low TeV flux state in May 2006, where simultaneous X-ray data by
Suzaku and very-high-energy gamma-ray data by MAGIC are available
\citep{tag08}.

As shown in Figure \ref{1ES1959}, the synchrotron component
shows a similar shape to that in Mrk 421.
Compared to the spectrum of Mrk421,
the spectral peak energies of the synchrotron and SSC components are similar
while the ratio of the gamma-ray flux to the synchrotron flux in 1ES
1959+650 is relatively small.
It suggests that the typical electron energy and magnetic field may
be similar in the two objects,
but the efficiency of the SSC emission in 1ES1959+650 needs to be
reduced by increasing the bulk Lorentz factor slightly.

Our results are summarized in Figure \ref{1ES1959},
in which the parameter values of $R_0$, $\Gamma$, and $B_0$
are basically consistent with the previous results in \citet{tag08}.
Model A (red) approximately reproduces the curved
spectral shape for the synchrotron component,
but the IR/optical flux is slightly higher than the observed flux.
This difference may be within theoretical uncertainty in our idealized model.
For instance, since the magnetic field may be not purely toroidal,
the field may decay faster than $B' \propto R^{-1}$.
In such a case, the synchrotron emission for a large $R$ would
be suppressed.
As model B (blue, where $R_{\rm out}=10 R_0$) shows,
if the emission from $R>10 R_0$ is neglected,
the synchrotron spectrum becomes more consistent with the observed data.
The slight difference in the spectra below 10 eV between models A and B
exhibits the small contribution of emission at $R>10 R_0$.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f4.eps}
\caption{Model photon spectra A (red), B (blue) and C (green) for 1ES 1959+650.
The black open circles are measured flux points from the multiwavelength campaign
in 2006 May \citep{tag08}.
The gray open circles are taken from the LAT 4-year Point Source Catalog
\citep[3FGL,][]{ace15}.}
\label{1ES1959}
\end{figure}

While the spectral shape of the synchrotron component
in model A or B seems consistent with the observation,
the gamma-ray spectrum may contradict the observed date
in the GeV energy range.
Note that the gray data points in the GeV range shown in Figure \ref{1ES1959} are
4-year averaged spectral data,
and they were not simultaneously obtained with the data in other energy ranges.
The variability in the GeV energy range \citep[e.g.,][]{kau17,pat18}
may resolve the discrepancy.
If we seriously incorporate the soft spectrum indicated by
the {\it Fermi} data points,
a broader energy distribution is required for electrons.
Model C (green), in which a smaller $\gamma'_{\rm inj}$ and higher $\Gamma$
are adopted, shows a broader gamma-ray spectrum.
Even in this case, the model flux below 1 GeV
is significantly lower than the observed data,
and the synchrotron spectrum becomes
broader than the data.
To reconcile both the narrow synchrotron and soft IC component,
an external photon field may be required as discussed
in \citet{asa14}.

\subsection{PKS 2155--304}
\label{sec:PKS2155}

PKS 2155--304 ($z=0.116$) is one of the most luminous HBL
objects in the TeV energy band.
The object is famous for short-timescale variability ($\sim$ minutes)
in the TeV gamma-rays. Recently, a spectral hardening in the hard
X-ray band has been discovered from observations with the NuSTAR satellite
\citep{mad16}. The spectral hardening can be interpreted by
the onset of the IC component. The observations were performed in a
very low X-ray state together with XMM-{\it Newton} and {\it Swift}-UVOT, which provide
soft X-ray and UV data for the synchrotron component.
We apply our model for the broad band spectrum
also including gamma-ray data by {\it Fermi}-LAT as reported in \citet{mad16}.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f5.eps}
\caption{Model photon spectrum (red) for PKS 2155--304.
The open circles for optical, X-ray and gamma-ray are fluxes measured in 2013
April \citep{mad16}.
The gray thin line is the broken power-law model in \citet{mad16}.
The radio data points represent core fluxes taken from NASA/IPAC Extragalactic Database (NED)}
\label{PKS2155}
\end{figure}

As the thin grey line in Figure \ref{PKS2155} shows,
the photon spectrum is fitted by a model with
a broken power-law electron distribution (the low-energy index
is 2.2, high-energy index is 3.8, and the break Lorentz factor
is $2.6 \times 10^4$) in \citet{mad16}.
However, this soft electron spectrum implies
the proton luminosity of $>10^{47}~\mbox{erg}~\mbox{s}^{-1}$
assuming the same number for protons and electrons.
\citet{mad16} concluded that the obtained proton luminosity is too large
as an HBL-type blazar.

The hard spectrum in the turbulence acceleration model
significantly suppresses the number of electrons.
The model shown in Figure \ref{PKS2155} (red) seems
consistent with the curved feature in the soft X-ray data.
In this model, the mean energy of electrons is about GeV:
the mean Lorentz factor is $\sim 2000$,
while that is $5.6$ in the model of \citet{mad16}.
Thus, we can reduce the proton luminosity by a factor of 400.

However, the model flux in the hard X-ray regime
is lower than the best-fit model of \citet{mad16},
because our model spectrum is significantly harder than
the model in \citet{mad16}.
To reconcile with the hard X-ray flux, we need another
external photon field as the IC seed photons again
\citep[see the model and discussion in][]{asa14}.

\subsection{3C 279}
\label{sec:3C279}

We revisit a famous FSRQ 3C 279 ($z=0.538$), while
we have tested this blazar with the turbulence acceleration model
in \citet{asa15}.
The adopted data of the spectrum
were obtained in an active period \citep[period ``D'' in][]{hay12},
but the data are averaged over five days, which may be
significantly longer than the variability timescale.
Thus, we adopt a steady emission model even in this case.
In \citet{asa15}, the external photon field was assumed to be
spatially constant.
With the photon field model explained in section \ref{sec:meth},
a similar result to \citet{asa15} is obtained as shown in Figure \ref{3C279}.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f6.eps}
\caption{Model photon spectrum for 3C 279.
The open circles are measured flux points in 2009 February
\citep{hay12}.}
\label{3C279}
\end{figure}

The low-energy cutoff in the radio band is due to synchrotron self-absorption.
The X-ray bump is attributed to SSC emission, while EIC emission
produces the gamma-ray peak.
The synchrotron spectral shape especially for the high-energy region
is well reproduced by our model.

\subsection{PKS 1510--089}
\label{sec:PKS1510}

To test the case of the infrared dust emission as the external photon field,
we fit the spectrum of a FSRQ PKS 1510--089 (z=0.36).
\citet{nal12} obtained broad band spectra from
multi-wavelength observations including Herschel satellite pointing
for far-infrared bands using PACS and SPIRE instruments.
They considered three components for the emission origin: jet
emissions in BLR and the hot-dust region, and
emission attributed to the accretion disk. The optical/UV bump and
X-ray components are considered to be the contributions from the
accretion disk and the hot disk corona, respectively, while
synchrotron emission is dominant in the far-infrared band observed by
Herschel.

\citet{nal12} adopted the two zone model, where the GeV emissions
are emitted from BLR and the emission from the hot-dust region
does not contribute to the gamma-ray emission so much. However,
\citet{ale14} reported detections of sub-TeV emission even during steady states and
possible correlations between GeV gamma-ray flares and radio core
appearances. Those results suggest that the gamma-ray emission is
likely to be originated outside of BLR. In this
paper, we consider the emission from only the hot-dust region;
the X-ray and optical components are not weighted so much
because of the contributions from disk and corona emission.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f7.eps}
\caption{Model photon spectrum for PKS 1510-089.
The open circles are measured flux points in 2011 August
\citep[epoch ``H2'',][]{nal12}.}
\label{PKS1510}
\end{figure}

Our model parameters in Table \ref{param_tab} imply
that the radius $R_0 \sim 0.2$ pc is
outside $R_{\rm BLR} \sim 0.07$ pc, but inside
the hot-dust region ($R_{\rm IR} \sim 1.8$ pc).
Figure \ref{PKS1510} shows our fitting results.
The gamma-ray spectral component is the EIC emission
from the hot-dust region.
The SSC emission is negligible because of the low synchrotron photon density
at the large initial radius.
The success in Figure \ref{PKS1510} suggests possible turbulence
acceleration even in the hot-dust region.

\section{Discussion}
\label{sec:dis}

The model with the hard-sphere like electron acceleration
in this paper is constructed only under simple assumptions;
constant energy diffusion coefficient,
constant injection rate of electrons, conical geometry ($V' \propto R^2$),
and $B' \propto R^{-1}$.
Nevertheless, our model spectra
have well reproduced the curved photon spectra of the blazars
from the radio to the high-energy gamma-ray bands,
though the low-energy tails of the SSC components
for 1ES 1959+650 and PKS 2155-304 would require
some modification in our model,
such as an extra photon field or a low-energy extra population of electrons.
In our model, the electron energy distribution is controlled by the three timescales:
dynamical ($R_0/\Gamma/c$), acceleration ($1/K$),
and cooling timescales.
The combinations of those parameters can produce variety
of the spectral shape without extra parameters.

\begin{figure}[!h]
\centering
\epsscale{1.0}
\plotone{f8.eps}
\caption{Radial evolution of the energy density ratios for model B of Mrk 421 (black),
model B of 1ES 1959+650 (blue),
PKS 2155-304 (green), 3C 279 (red), and PKS 1510-089 (magenta).}
\label{Eneden}
\end{figure}

Here we have not specified the mechanism of the turbulence excitation
to accelerate particles.
One candidate is magnetic reconnection in highly magnetized plasma
\citep[e.g.][]{sir14,sir15,ois15,tak18}.
As \citet{sir15} demonstrated numerically,
the energy dissipation due to magnetic reconnection
leads to an equi-partition between the magnetic field and
non-thermal particles.
As shown in Figure \ref{Eneden},
the energy densities of the magnetic field and electrons
are equi-partition only for the case in 3C 279
\citep[see also,][]{der14}.
In this case, magnetic reconnection is a promising mechanism
for the turbulence excitation, or reconnection may directly
accelerate electrons, which can be equivalent to the stochastic acceleration
expressed by the diffusion coefficient in this paper.

On the other hand, the other objects in Figure \ref{Eneden},
the magnetic field is subdominant compared to the electron energy density.
Even for the case of 3C 279,
it is reported that the magnetic field energy became much lower than
the electron energy for the gamma-ray flare states \citep{hay15,asa15}.
In those cases, magnetic reconnection is unlikely
as the energy source of turbulences or non-thermal electrons.

The acceleration timescale in the hard-sphere model
does not depend on electron energy.
When particle scattering is dominated by a certain size
of eddy, the acceleration timescale will be
common irrespectively of electron energy.
However, the turbulence may be expressed by a superposition of MHD waves
in small scales.

The fast mode is the most likely dominant wave mode as the electron energy source
in low-magnetized plasma implied from our results.
The energy of the turbulence is injected at a large scale
($<R_0/\Gamma$) as fast waves, and cascade to shorter scales following
the Kolmogorov law; $k E(k) \propto k^{-2/3}$,
where $k$ is the wave number.
On the other hand, the power spectrum of the magnetic field
tends to be flatter than the kinetic one
\citep{cho00,cho09}.
At a scale, where the magnetic power is comparable
to the kinetic one,
the kinetic energy transfer mechanism in the turbulence cascade process
changes from the hydrodynamical one to
the magnetohydrodynamic one.
The power spectra for both the kinetic and magnetic energies
become steeper at this equi-partition scale \citep[$k=k_{\rm max}$,][]{gs95,ino11}.
In this case, the acceleration timescale may be regulated
by this scale.

If the Larmor radius of electrons is significantly shorter
than the wavelength $k_{\rm max}^{-1}$,
the pitch angle diffusion via gyro resonance
is not responsible for particle scattering.
In this case, the main mechanism of the energy exchange between electrons and waves
is transit time damping \citep[TTD,][]{ber58};
electrons are accelerated when their velocity along the magnetic field
equals to the parallel component of the phase velocity.
For non-relativistic waves, the number fraction of relativistic electrons that satisfy
the TTD resonance condition is small.
Only electrons with their pitch angle $\sim \pi/2$ can interact with waves.
However, the phase velocity of the wave in the blazar emission region
may be mildly relativistic.
Furthermore, the mirror force can broaden the resonance condition of TTD
as shown by \citet{yan08}.
We can expect that a significant fraction of electrons
interact with the waves.

When electrons are scattered by waves, whose wavelength are longer
than the gyro radius,
the description of the second order Fermi acceleration may be valid.
The scattering time scale is $\sim (c k_{\rm max})^{-1}$,
and the average energy change per scattering is $\Delta \varepsilon_{\rm e}/\varepsilon_{\rm e}
\sim v(k_{\rm max})/c$.
Let us assume that the turbulence velocity $v(k_{\rm max})$ at $k=k_{\rm max}$
is expressed by the Kolmogorov law as $v^2(k_{\rm max})=v_0^2 (k_{\rm max}/k_{\rm min})^{-2/3}$,
where $v_0$ is the turbulence velocity at the injection scale $k_{\rm min}^{-1}$.
Then, the acceleration frequency becomes
\begin{eqnarray}
t_{\rm acc}^{-1} \sim c k_{\rm max} \left( \frac{v(k_{\rm max})}{c} \right)^2
= c k_{\rm max} \left( \frac{v_0}{c} \right)^{2}
\left( \frac{k_{\rm max}}{k_{\rm min}} \right)^{-2/3}
\end{eqnarray}

Here we take model B for Mrk 421 as an example.
As shown in Figure \ref{Ele}, TeV is sufficient for the maximum energy of electrons
to reproduce the photon spectrum.
In this model, the Larmor radius of TeV electrons is $2 \times 10^{10}$ cm,
which should be shorter than $k_{\rm max}^{-1}$ to realize the non-gyro-resonant
scattering as dominant acceleration process.
On the other hand, we need a $k_{\rm min}^{-1}$ shorter than $R_0/\Gamma=10^{16}$ cm.
Those conditions imply $k_{\rm max}/k_{\rm min}<4.8 \times 10^5$.
With a conservative assumption of $k_{\rm min}=\Gamma/R_0$,
$c k_{\rm max} (k_{\rm max}/k_{\rm min})^{-2/3}< 2.3 \times 10^{-4}~\mbox{s}^{-1}$.
The turbulence velocity at the injection would be slower then the sound speed
in relativistic plasma: $(v_0/c)^2<1/3$.
Finally, the maximum value of $t_{\rm acc}^{-1}$ is estimated as
$7.8 \times 10^{-5}~\mbox{s}^{-1}$, which is much larger
than $K \sim 10^{-6}~\mbox{s}^{-1}$ required in the model.
If the turbulence is exicited by the star-jet interaction,
a value of $k_{\rm min}$ much larger than $\Gamma/R_0$ is possible,
which further shortens $t_{\rm acc}$.
Thus, the non-gyro-resonant scattering
may provide a mechanism to realize the hard-sphere-like
acceleration in blazars as required by our models.

Our simplest model with
the Kolmogorov-like model ($q=5/3$) cannot fit the blazar spectra.
Both the synchrotron and IC components become narrower than
the observed shape for those cases.
If the particle acceleration is due to turbulence in the jet,
the hard-sphere-like diffusion in the energy space seems necessary.
However, it is difficult to distinguish observationally
turbulence acceleration from other mechanisms.
As demonstrated in \citet{asa14}, the flare light curves may provide
a hint for the acceleration mechanism.
In this context, the GeV flare with a very hard spectrum in 2013
is an encouraging example as discussed in \citet{asa15}.
Future gamma-ray observations including CTA will give us
opportunity to verify the acceleration mechanism.

\acknowledgements

First we appreciate the anonymous referee for the helpful advice.
We thank Greg Madejski and Krzysztof Nalewajko for their providing SED
data points of PKS 2155-304 and PKS 1510-089.
This work is supported by Grants-in-Aid for Scientific
Research nos. 16K05291 (K.A.) and 18K03665 (M.H.) from the Ministry
of Education, Culture, Sports, Science and Technology
(MEXT) of Japan.

redpajama_set_name: RedPajamaArXiv


Benilov ES (1992) On the surface waves in a shallow channel with an uneven bottom. Studies in Applied Mathematics. 87: 1-14.
This paper examines surface gravity waves in a shallow channel with periodic or random bottom irregularities. Three types of bottom topography are distinguished, allowing a simplification of the basic shallow-water-wave equations. For two of them, asymptotic equations of the Korteveg-de Vries type are derived (the third type has been considered earlier by other authors).


Newly built. Or old and worn. From "properly renovated" to "badly in need of a fresh coat of paint" to "it'd be better to tear it down." From "worth every penny" to rip-off. From wow to meh. So many rooms with so few outlets. And why are those outlets in spots that make no sense? All those worn mattresses that make you feel like you're sleeping in a tub. Every once in a while there's a heavenly mattress ... I'm so tired. I need to sleep.
Worn sheets. Crisp sheets. Thin blankets. Heavy blankets. An infinite number of pillows that are too soft. Small useless desks. All these lamps and light fixtures, and still no proper lighting. Why? How hard can this be?
Closets with a few hangers. Flimsy ironing boards. Old irons. Sometimes brand new irons. Leaky irons. But no convenient outlets. Who selected the artwork? Art? Sometimes real glassware. I like that! Often just plastic cups. I hate that! $4 for a bottle of water. I really hate that!
All those loud and inefficient wall AC units. And those loud in-room fridges. So many blinking alarm clocks. Why are thermostats set to arctic blast? TVs with an infinite number of sports channels. There's at least one channel for every imaginable and unimaginable sport. I will sleep here tonight, but I wish I were at home. I want to sleep in my own bed. I'm so tired. I need to sleep now. I have to catch an early flight in a few hours.


text:
CHEZIDEK
Chezidek started singing from an early age at school concerts, and was a member of St. Ann's Bay Marching Band.[2] After finishing school he performed on sound systems in the area, as Chilla Rinch, singing and DJing at various dance and talent shows.[3]
He left St. Ann's Bay for Kingston where he linked up with record producer Philip "Fatis" Burrell from Xterminator Production.[3] He recorded his first album in 2002, entitled Harvest Time (distributed by VP Records), with popular tracks such as "Can't Hear Must Feel", "Breakfree" and the title track "Harvest Time".[2]
His first number one hit single "Leave De Trees" on the Our Promotion label,[4] produced by Hugh Miller (aka Bunny Dan) went on BBC Top 10 dancehall chart.[3] Since then he has performed on major events such as Magnum Sting, Teen Splash, Dancehall Jam Jam, Bob Marley Tribute, and Tribute to Peter Tosh, Rebel Salute and Western Consciousness. He was awarded best new artiste by the Jamaica Federation of Music and Affiliated Artiste (JFM) for Middlesex (County).[3]
Chezidek's album Inna Di Road was produced by Bobby "Massive B" Konders and distributed by Greensleeves Records in September 2007. "Call Pon Dem" as well as covers of "Mi Nah Run" from his album Inna Di Road is featured on the fictional radio station Massive B Sound system in Grand Theft Auto IV.
Source: Wikipedia https://en.wikipedia.org/wiki/Chezidek
Chezidek Youtube
Chezidek Instagram
Chezidek Facebook
Chezidek Lastfm
Chezidek Spotify
Chezidek Apple Music
Reggaeville


Wednesday 29th August-Carbon backflip-option expiry looms plus the "Hole!"No one sent Super Mario a ticket it seems!! | Beeks Downunder-Because not all financial news is boring!
Our market put in a late spurt yesterday as shorts covered in front of the Jackson Hole meeting and the option expiry on Thursday. News that Julia had executed another triple pike with a twist on Carbon Tax helped as well…getting very puzzled now that a impost designed to change our habits and save the World is giving us cash back and now watered down with new floor price abolition..not sure I get it anymore..isn't the impost designed to hurt so we change…lost me sorry!
I remain of the view that the market has priced in too much optimism on further stimulus..I feel that Jackson Brown will be a damp squib and markets will be disappointed..happy to be proved wrong though!!
The range is still 4000 to 4400 and as we near the top in a market that is going Ex Div I am wary!.The reporting season has generally been ok with some big winners and similarly some big losses..FXJ I am looking at you now…but whether it is enough for the next leg whilst Commodity stocks languish remains to be seen..I suspect not..the big surprise out of the season (to be Jolly) is the strength of Industrial shares and the weakness of Resource stocks..we were supposed to be having a resource boom after all and if you read the media ,which I gather fewer and fewer people are doing, then you would think that Industrial business is dead..deceased..it is no more..well maybe it's just pining for the Fjords!
News yesterday was positive from Seven Media on the back of big Tonka Toy business…Aristocrat surprised on the upside as its Japanese gaming machines took off..Flight Centre was a ripper but warned on growth ahead getting harder..
As far as things to buy ..I would suggest that you lie down for a few days and wait to see what happens ..Jackson will be a dud and the market will go Ex Div in September ,together with eth German Constitutional Vote on the 12th…expect some weakness after the run we have had….if we do push higher in the coming days ..may be time to lighten your long positions!! Banks may be a place to start!!!
Things to make me go all Jackson Hole!
2.Obama's US is now officially in debt to the tune of $16,000,000,000,000BAMA!Ouch..only took 286 days to go from $15trillion to $16trillion!!
3.NCM has had a problem with its communications from PNG as they are experiencing a close down of their operations…did take them four days to report it…love continuous disclosure!!
5.African resources conference today..bigger than Diggers and dealers..that's saying something..
6.More trouble in Catalan as they ask for $5bn… The region says it will not accept political interference as part of the loan.
..and news just in that ECB President Mario Draghi has decided not to attend the annual Jackson Hole meeting of central bankers on Friday sparked plenty of speculation that the central bank is preparing to fire its 'big bazooka'. I thought he was going to do whatever it takes…can't even get on a plane..I mean really!!!
7.Rumours of a Prince Harry video as well…lovely stuff..Mum would have been proud!
8.Grahame Morris calls Leigh Sales(ABC Journo who poleaxed Abbott with her questions) a Cow…bless! Love these old Howard Gov people..
9.Japanese figures yesterday a worry..China manufacturing numbers also out soon..they just need to make up a number ..look inside the fortune cookie perhaps..
10.Market going nowhere today I am afraid!
Last year I upgraded from Boyfriend 5.0 to Husband 2.0 and noticed a slowdown in the performance of flower and jewelry applications that had operated flawlessly under boyfriend 5.0.
In addition, Husband 2.0 uninstalled many other valuable programs, such as Romance 9.9, and installed undesirable programs such as AFL 5.0 and League 3.0.


As a part of the re-equipment of the vehicle fleet, two reach stackers (type: Gloria) with AdBlue technology have been acquired for the Neuss terminal. The vehicles have been additionally equipped with a central lubrication system and tablets for use with the Terminal Operation System (TOS).
Following instruction and training, the reach stackers went into operation as planned on 01.01.2016.
AdBlue is an aqueous urea solution which cuts the amount of nitrogen oxide in the exhaust gas from diesel engines by 90 percent. Another advantage of AdBlue technology is the decrease in fuel consumption, which may be as much as five percent.
By switching all reach stackers and container stackers to AdBlue, Contargo Neuss is making a significant contribution to the reduction of climate-damaging emissions.


Generally speaking, silicon keypads along with carbon contact drugs are used to stimulate and deactivate electric tracks (a contact tablet is shaped on the back of a plastic plastic button). When a silicone plastic keyboard is pressed, its position changes so that a carbon contact tablet finishes electrical signal thus enabling the electric current to flow. Weighed against the other types of enterprise service, this one is probably the most cost effective and reliable because it generally does not employ mechanical changes known for their short lifetime and large generation cost.
Particular kinds of electrical gear run below freezing point. The keys that are accustomed to activate them are made out of silicone rubber because this material has the capacity to tolerate very low temperatures.
Because silicone is resistant to the uv light, plastic rubber buttons are used in UV light medical devices.
Kid toys should not silicone molds for arts crafts soap sourced elements of dangerous toxins that may harm the child's health. Because of the silicone's non-toxicity, kid toys equipped with plastic plastic buttons create no chance to their owners.
Silicon is just a non-sticky product, making plastic rubber links very convenient and pleasant to use.
Minimal generation charge of the silicone rubber links and their subsequent low wholesale price offers an exceptional prospect to save money for the production firms that get them from the suppliers.
Following functions are used to manufacture plastic rubber products and services: vulcanization, also referred to as compression molding, and treatment molding.
Through the vulcanization silicon enters chemical reactions with sometimes sulfurs or peroxidesor urethane crosslinkers or metallic oxides or dueces or acetoxysilanes. The goal of the procedure is always to force silicon rubber to get the form of a mold.
At first of the injection molding method silicone matter is positioned in to a barrel which can be hot over the silicon reduction temperature. Next large device force can be used to fill dissolved plastic in to a cold mold. Water silicone requires the design of a mould and gradually hardens while their temperature declines to the room temperature level.
The modifications in the mould types are almost endless, helping to make possible to have conclusion services and products of any sizes and shapes. As far as rubber buttons are worried, a single mould could be properly used to make a few forms of buttons of arbitrary shapes.


text:
// Copyright 2017 Twitter. All rights reserved.
//
// Licensed under the Apache License, Version 2.0 (the "License");
// you may not use this file except in compliance with the License.
// You may obtain a copy of the License at
//
//    http://www.apache.org/licenses/LICENSE-2.0
//
// Unless required by applicable law or agreed to in writing, software
// distributed under the License is distributed on an "AS IS" BASIS,
// WITHOUT WARRANTIES OR CONDITIONS OF ANY KIND, either express or implied.
// See the License for the specific language governing permissions and
// limitations under the License.

package com.twitter.heron.api.hooks.info;

import java.time.Duration;

import com.twitter.heron.api.tuple.Tuple;

public class BoltAckInfo {
  private Tuple tuple;
  private int ackingTaskId;
  private Duration processLatency; // null if it wasn't sampled

  public BoltAckInfo(Tuple tuple, int ackingTaskId, Duration processLatency) {
    this.tuple = tuple;
    this.ackingTaskId = ackingTaskId;
    this.processLatency = processLatency;
  }

  public Tuple getTuple() {
    return tuple;
  }

  public int getAckingTaskId() {
    return ackingTaskId;
  }

  public Duration getProcessLatency() {
    return processLatency;
  }
}

redpajama_set_name: RedPajamaGithub


Twitter by far has been the most transformational social media platform that i have used. I truly believe that one of the best ways to give back to a community is by being a part of it. Twitter is a great example because so many people I think write it off as being confusing and not engaging without realizing that if you want to become a part of the twitter community and really take advantage of all that it has to offer you have to invest some time becoming a part of it.
This week on Summer Social Im taking you on an in depth look at Twitter, why you should use it, how to get started and tips and tricks to help you successfully navigate the Twitterverse.
In today's video I talk about why twitter and the top five ways you'll benefit from joining.


text:
Stipe Miocic holding out for Daniel Cormier rematch: 'I know I'm the better fighter'
Stipe Miocic is not giving up on getting a rematch with Daniel Cormier, the man he lost his heavyweight title to back in July 2018.
By Harry Davies@harrydavies14 Feb 4, 2019, 10:00pm EST
Share All sharing options for: Stipe Miocic holding out for Daniel Cormier rematch: 'I know I'm the better fighter'
Stipe Miocic has revealed getting a rematch with the man he lost his heavyweight title to last year, Daniel Cormier, holds more importance to him then actually getting his title back.
Miocic (18-3) won the heavyweight belt when he knocked out Fabricio Werdum at UFC 198 in May 2016. The 36-year-old went on to defend his belt three times, breaking the record for the most consecutive UFC heavyweight title defenses.
ESPN+ Has Live Sports Covered
Be sure to catch all the upcoming fights, including UFC 234: Whittaker vs Gastelum on Saturday, Feb 9, by subscribing to ESPN+…
SUBSCRIBE HERE TO WATCH THE FIGHTS ON ESPN+
The rematch with Cormier holds so much importance to Miocic purely because he feels he is the better fighter of the two. Having a baby daughter, Meelah, just a few weeks after that fight with Cormier, Miocic feels he now as something to fight for.
"Oh, 100 percent," Miocic told MMA Fighting. "It's everything. Just because I know I'm the better fighter — I believe I'm the better fighter. In my heart. I'm fighting for something, I'm fighting for her. It's not just about me, my wife and doing what I love. I'm doing what I love, but now I'm doing it for an even better reason."
Miocic still continues his job as a firefighter in addition to his UFC career. The former champion feels he was winning the fight up until he got caught with the finishing blow from Cormier, but maintains 'DC' doesn't hit as hard as Francis Ngannou, the last man Miocic successfully defended his title against before losing it to Cormier.
"I felt like I was winning the fight, I felt like I kind of got off track of what I was doing, not doing my usual and listening to the game plan. And just kind of overstepped what I needed to do and he caught me with a punch — a punch I didn't see." Miocic said. "I'll say to this day, he doesn't hit as hard as [Francis] Ngannou. It was just right on the button, right where it needed to be.
"It wasn't like he was wiping the floor with me. I just knew I was the better fighter in there. And let me tell you something, next time it happens, next time we fight, you'll see a different fighter. A whole new me. A lot has changed."


The problem of letting down of milk is attributed due to keeping away from calf, death of calf during / after birth, stress of travel, changing of place the change of person habituated while milking, environmental changes, etc. Herbal cattle feed supplement, Dhara is effective in solving problem of letting down of milk.BVG Dhara makes the animals psychologically stable and calm and oxytocin is released naturally.
milch animals by using the naturally available medicinal plants.
2. As herbal product safe to use.
1. Solves problem of letting down of milk in cows and buffaloes within 3 – 5 days.
2. Helps in expulsion of placenta.
animal, that releases oxytocin hormones, leads to release of milk.
getting best results. Repeat the dose of All Clear after every 6 months.
consecutively (within 1 and 1/2 day) or change as per Veterinarian's recommendation.


Kimball County Tourism, in conjunction with PrairieAdventure Tours, is offering prairie wildflower tours in celebration of Nebraska Wildflower Week from May 30 through June 7. Tours will be led by local rancher and biologist, Shaun Evertson.
Tours will be offered Saturdays, May 30 and June 6, and Sundays, May 31 and June 7 at 8 a.m. An evening tour on Wednesday, June 3 is scheduled for 6 p.m. All tours are free and open to the public. Also, available are free brochures identifying roadside flowers and grasses.
Tours will last approximately 90 minutes. Anyone interested should call (308) 241-0573 to reserve a spot. Meet in the parking lot of the High Point Welcome Center of Western Nebraska, I-80, exit 20 (204 S. Kimball Blvd.).


From the personal experience, the darkness of the darkness is just annoying. As a woman of color, I have to deal with a shadow in my adult life. In most cases, I did not consider it. I mean, in any case, they have hidden 90% of the time. Then, when I put my phone on my head to get the perfect summer selfie, the moment came, my repair station was fully displayed. My photos are instantly dark and smudged. So, I started to doubt. What causes the armpits to darken over time? What can I do?
And guess the cause of hyperpigmentation. Shaving.
Charles said: "People shave a lot of underarms, which can lead to inflammation, as well as repeated trauma and friction." "Whenever there is any repeated rubbing on the skin, the skin becomes slightly thicker and the skin becomes thicker and becomes thicker." Darker, or hyperpigmented."
Ok, so if it is scraped off. How about waxing? Charles explained that the process is not so good, tearing off the hair with regular wax can actually make things worse - especially if you are prone to grow your hair. He said: "If you have thick and thick hair - may cause trauma and inflammation through ingrown hair - you may be more susceptible to dark areas of the body." In fact, Charles said, thick black hair even The armpit can be made darker before the skin surface grows.
Laser hair removal solves all of these problems. Charles said: "We often treat people with black areas on their arms because the hair is rough, laser hair removal machine, because it is much less traumatic, and this type of hair removal helps to grow finer hair overall. "Thin hair means less ingrown hair and less shaving, and is good for fighting hyperpigmentation."
If there is no diode laser hair removal machine in your future plan or budget (a session can cost you more than $200 each time, and you need four to six times to see the results), there are steps you can take to reduce the shaving of the skin. Try to shave in the same direction as the hair grows and make sure to use the shaving cream to soften the skin and hair before picking up the razor.
Your dermatologist can use retinoids or fading creams to treat existing dark underarms, but Charles says, "This is definitely not an easy problem," because there is a lot of skin and skin friction on your arms that can cause irritation. So if you want to brighten your skin, you should work with a professional and usually show this area as much as possible. Moderation is the best option to prevent the future from being darker.


Looking for a Cool Maternity T-shirt?
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A must-have for the mum-to-be.
Available in black with a metallic pink print.
Each Maternity t-shirt is designed exclusively for us using fair-trade cotton and sweatshop free manufacturing.
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"I don't live in Orange at the moment, I travel each day to work at Rhonda's Hairstyling Salon. My partner and I are currently looking for a house to buy in Orange in the new year. I look forward to living here, I love the distinct seasons and all of the amazing local produce, I'm also a fan of food and wine week.
My hobbies include CrossFit, yoga, photography, shopping, fishing, kayaking, going to music concerts, and playing with my dog. I am quite interested in nutrition and of course the hairdressing/beauty industry and keeping up to date with new trends and techniques.
In the summer I love anything that involves being close to a beach. Unfortunately, I can't do that every weekend, so I am quite content going kayaking, camping, going out for dinner or catching up with friends. Anything outdoors in the sunshine is always bliss. I'm always happiest when I am wearing Lorna Jane because usually an adventure is about to happen.
Dec 13 Very well done kids…all of you!


We are a full-service financial firm committed to helping people achieve their financial goals. We offer a wide range of financial products and services. We believe the more you know, the better decisions you can make. That is why we endeavor to teach first and only then can we have a conversation about how to choose the best solution to meet your individual needs.
Please feel free to contact any of the below listed professionals if you need help. There is never a charge for an initial meeting. We would be pleased to help you define your "Strategy".


BATTER-UP was designed to keep a ballplayers's bat close at hand and off the ground. It's also the perfect place to hang a batting helmet. BATTER-UP is small and light weight, which makes it easy to drop in a batbag. It has been designed to weave into the chain link fencing found on most dugouts, but it can also be hung on netting or a nail.
Every ballplayer who owns a bat or helmet NEEDS a BATTER-UP. Currently available in Red, Blue, Yellow, Teal, Purple and Black.
The BATTER-UP is great for young players!
When placed in the proper batting order, the players know when it is their turn at bat.
HOW TO USE YOUR BATTER-UP!
BATTER-UP is against the first link. Then, turn the hook as shown.
turn the slide tab over a strand of the net. BATTER-UP!


At Abu Khader Group, We have implemented Management Trainee Program and Business Excellence Officers Program where new graduates go through a full rotation program across all functions for one year. Upon evaluation of the experience learned and the skills of the Management Trainees they will be assigned a full time job.
The priority Candidates for this program are the university students who complete a summer internship program with our group. Our Summer Internship program covers all fields related to our businesses mainly Mechanical/Electrical/Mechatronics/Industrial Engineering students in addition to Business School Graduates related fields. We accept (50 – 60) trainees each year, attracted from many sources including universities and vocational training centers. We provide our trainees with professional and comprehensive training experiences, which contribute to the overall development of their confidence levels and independence, in addition to their personal achievement. Our Interns will have the opportunity to learn effective, efficient Techniques. This experience gives the trainees an opportunity to be one of our team in future.


Merlin Shepherd's clarinet provides the perfect foil for his deep musicality. Whether he's playing traditional Klezmer with the Sound&Light Cinematic Duo or wild ecstatic music with Frank London's Klezmer Brass Allstars and Boban Marcovic, or free-form wailing with Aaron Alexander's Midrash Mish-Mosh or playing with his own quartet, his music is a powerful and emotional force that redefines the instrument.
His unique musical voice can be experienced on his debut solo CD of original material, "Intimate Hopes & Terrors", (released on Oriente Musik) a unique collaboration with 10 of the top Klezmer musicians from the former Soviet Union. This recording was given a 5 star rating and also a "Top of the World" track on the cover CD of Songlines.
Has been Musical Director for The Royal National Theatre, Royal Shakespeare Company and Shakespeare's Globe Theatre, London. He was also Klezmer Advisor for the Royal Shakespeare Company for their 1992 production of Anski's "The Dybbuk". Composed scores for numerous dance and theatre companies. Leads The Merlin Shepherd Kapelye featuring The Former Soviet Union Klezmer Allstars that perform Merlin's compositions in traditional and new klezmer style. Also leads the Merlin Shepherd Quartet, the smaller more intimate version of his Kapelye.
Leader of Hamsa Quintet since 2014, a Mediterranean Klezmer Funk band.
Merlin also works with Polina Shepherd as The Sound & Light Cinematic Duo, playing to the Yuri Morozov Collection of B&W silent Jewish films made in Kiev from 1908-1945.


text:
Home > other > King of the Jungle 2013
King of the Jungle 2013
Zhang Jie once said a famous say, Don't imagine that every word you say is true, but it is true that every word you say is true.However, even so, the emergence of King of the Jungle 2013 still represents a certain significance.This makes us think deeply.
Or as J.H. Newman famously said, Fear not that the life shall come to an end, but rather fear that it shall never have a beginning.How to realize King of the Jungle 2013.With these words, we have to examine this issue more carefully!
Liang Qichao said a famous quote, Success is easy to win, Shifeng, on stage, shallow and deep knowledge of people like Yan, who thought of hanging.King of the Jungle 2013 seems to be a coincidence, but if we look at the problem from a larger perspective, it seems to be an inevitable fact.Although this sentence is very short, it makes me think about it.
Spencer once said a famous say, Education should try to encourage the process of individual development. Children should be guided to explore their own, their own to infer. Give them the best possible, and guide them to find the more should be as far as possible.What is the crux of the problem?Although this sentence is very short, it makes me think about it.
Sue Home Linsky Once said, Educators should be a profound understanding of the minds of the people who are growing up in their entire education career to continue to study the psychology of students, deepen their psychological knowledge, to become a real expert in education.The so-called King of the Jungle 2013, the key is how to deal with King of the Jungle 2013.With these words, we have to examine this issue more carefully!
Leo Burnett said a famous quote, Let's continue to be famous:"this agent has spent most of the time improving its ideas, and not on the right to justify it.".With these problems, let's take a look at King of the Jungle 2013.This sentence brings us to a new dimension to think about this problem.
Someone said a famous quote if you find a job that you enjoy, then you won't have to work another day.What is the crux of the problem?With these words, we have to examine this issue more carefully!
Balzac said that inadvertently, There is no such thing as a great talent without great will - power.Everyone has to face these problems. How should we deal with this kind of problem?I hope everybody can also understand this sentence well.
Mattin Luther King said a famous quote, We must accept finite disappointment, but we must never lose infinite hope.This issue has caused wide public concern for King of the Jungle 2013.This makes us think deeply.
Taylor said a famous quote, Management's first goal is to make higher wages and lower labor costs combined.As far as I am concerned, King of the Jungle 2013 is of great significance to me.Although this sentence is very short, it makes me think about it.
Zhang Jie once said a famous say, Don't imagine that every word you say is true, but it is true that every word you say is true.Everything has two sides and King of the Jungle 2013 is not an exception,it has both advantages and disadvantages.This inspired me how to develop next.
Zuozhuan said a famous quote, The husband, and also the name of germany. Germany, the foundation of the state.Why does King of the Jungle 2013 happen?With these words, we have to examine this issue more carefully!
2023-01-29Pure love romance
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2023-01-29Rape class Director
2023-01-29instant
2023-01-29Passion website
2023-01-29The old ford
2023-01-29Female safety period
2023-01-29The outbreak of
2023-01-29Potassium chloride
2023-01-29Cupid II- Battle Thai Drama
2023-01-29Attack of the rat
2023-01-29The waves of the sea
2023-01-29Female warrior 3 d
2023-01-29Psychedelic Black rainbow
2023-01-29The Werewolves Season 1
2023-01-29Digimon Season 3
2023-01-29Alien attack
2023-01-29Dr Strangelove or how do I learn to stop being afraid and love bombs
2023-01-29The man from Deep River
2023-01-29Jon Rahm
2023-01-29May Day 2022
2023-01-29Spencer Haywood
2023-01-29Ridley Road
2023-01-29Nikki Glaser
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2023-01-29Mike Lindell MyPillo
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2023-01-29Kate Spade
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Waxing used to mean one of two things – an expensive trip to the salon, or a wild experiment that could feature one or more of the following: a microwave, hot wax, an electric cauldron, hope, tears, and human sacrifice.
Luckily these practices are something out of the past, thanks to devices such as the EasyWax Electrical Roll-On Kit. An all in one device that heats the wax, and also works as the applicator to make for smooth, even coverage.
This method of hair removal is a form of epilation, which is removing hair at the root, rather than just the visible portion above the skin. It takes the hairs up to four weeks to make themselves known again (as opposed to the 2-3 days after shaving) and with time, you will notice that they come back finer, keeping you smoother for longer.
To use the EasyWax Electrical Roll-On Kit, you just have to put the wax refill into the device, plug it into the mains (so no expensive batteries) and leave it for about twenty minutes, until the wax has melted. You then roll it onto the areas that you wish to remove the hair from; the wax cartridge has a roller head to ensure that the wax comes out in a smooth and even layer. If you are tackling underarm hair, or your bikini zone, you can use specific refills with specially designed heads, for further ease and comfort. You then take the provided fabric strip and push it down onto the wax, leave for a few seconds, before pulling it off in a fluid motion against the direction of hair growth. Use the provided perfect finish wipes to get rid of any excess wax, although if you've run out of these you can use baby oil and a cotton swab. If any individual hairs somehow managed to escape, then these can be plucked out carefully; make sure you don't wax the same area twice.
For the best results, it helps to exfoliate the day before, wash the area with warm water and dry it carefully immediately before waxing. This removes some of the oils on your skin that can interfere with the wax, and also helps open up your pores so the hair comes out much easier.


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Rifat Chadirji
An Internationalised Tradition In Architecture
The Iraqi Rifat Chadirji was born in Baghdad and trained as an architect at Hammersmith School of Arts and Crafts, London, qualifying in 1952. On returning to his own country, he set up the practice Iraq Consult of which he is still president. Between 1954 and 1963 he also held a number of top government posts, and from 1980 - 1982 he was in charge of a massive conservation and development program for Baghdad.
His work - including public and private building large and small - has been widely exhibited in Europe, the Middle East and Africa and has won numerous awards. In 1986 he received the Chairman's Award of the Aga Khan Award for Architecture.
Since 1982 he has been dividing his time between the USA, where he has been a Visiting Scholar at both Harvard and MIT, and England, where he is preparing future books. Already published are several in Arabic and "Concepts & Influences: Towards A Regionalised International Architecture", London, KPI, 1986, is in English.
In his talk he covers much the same ground as in the latter book, but with greater accent on his own work in Iraq. His thesis, that form is determined by the interaction of social technology and social need, offers a different approach to the usual historical analysis of architecture. He argues that architecture's future lies in lessons learned from the past, from man's way of dealing with regional variations in nature and in his means of production.
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