text:
Featured, Music,
2Baba is having a golden career moment like no other artist from the last two decades
Nearly thirteen years ago, the release of "For Instance", off 2Baba's 'Grass to Grace' album, sparked rumors that he was being witch-hunted by president Obasanjo, Nigeria's first civilian president after many decades of different military regimes that silenced and persecuted free expression. Last year, 2Baba was allegedly bullied out of holding a march against the government. After weeks of prior build-up that somewhat tilted the country towards the possibility of another 'OccupyNigeria', 2Baba surfaced online, looking overdressed and exasperated with a video calling off the protest a week before the slated day.
In Nigeria, like many parts of the continent, revenue flows from bottom to the top and never back down, so income is constricted for 'frivolities' like music. Artists are forced to also try and make income from the same honeypot as politicians and big corporations. The hypocrisy of 2Baba then becomes apparent, especially after canceling out on fans who expected him to actually pull off the protest.
During a recent interview, 2Baba said: "We have a society where they play every type of music from morning till morning. There should be time for some kind of music that are immorally heavy (And) should play at a time when kids are sleeping". For all of the media storms that have swayed public opinions away from 2Baba, he understands better than anybody that the farce of a society's morality is only as true a reality as what people are allowed to talk about. Without a doubt, the two parts of Mr Idibia (2Face, 2Baba) have seen the light and dark of Nigeria. He's aware that while the young must be protected, truth should not be masked as evil or fallacy.
Since the end of colonization till date, Nigerian culture as a whole has witnessed several jumps because of the constant rifts between imported influences and long-held values. As a result, it always seems like nothing sticks for too long; Not our electricity, not our media, not our institutions, not even our democracy. But with the release of 2Baba's "Amaka", already making rounds on radio, its been over 20 years since he was a 'Plantashun Boi', and has saliently become one of the most consistent Nigerian 'truths'. So much so that the arch of his career is often told with the dreamy rhetoric of being inspirational for coming generations.
His debut album, 'Face 2 Face', shot him into the limelight and five albums, many singles and awards later, no other artist passes the test of serving as a blueprint for the conventions that have become the format for popular Nigerian music. Using a blend of Hip-hop-R&B, Caribbean music and his traditional African sounds, 2Face eased Nigeria and Africa into an era for refined popular music, made at home for people at home.
The important thing about 2Baba's staying as one of Nigeria's most relevant pop stars till date, is the rarity, especially given the kind of artist he is. Pop music's volatile nature is reflected in how Afropop seems to only be capable of assuming only one sound at any particular point in time; Think the recent 'ponpon' and 'shakushaku' rave. The P Square brothers, D'banj, Asa, are amongst the few who seem to have been around the block for just as long as 2Face, but none got into the spotlight before 2Face recorded "Omode Meta" with Tony Tetuila and Ruff Rugged and Raw in 2000. Think about this, 2Baba has seen as many inflation as careers that took off and crashed prematurely—and probably more.
Featured Image Credits: Instagram/official2baba
ICYMI: How 2Baba nearly removed himself from an industry he helped create
2Baba
Previous Article Hear Jamal Swiss' heartwarming new single, "No Stress"
Next Article Watch Skales and Harmonize on "Fire Waist"


text:
Q: How to convert time date from JSON to human readable? Kindly help me with converting JSON time data to 12 hrs human readable time in PHP.
Data I got as time from JSON is: 1380, 1395 and so on
Real time corresponding to JSON time data is as follows.
    For 1380 is 11.00PM
    For 1395 is 11.15PM
Now kindly tell me how to convert (1380, 1395, etc) into human readable time 12hrs in PHP
Thanks in Advance.

A: Assuming that this value is simply the number of minutes since midnight:
$value = 1395;
$hours = floor($value / 60);
$minutes = $value - ($hours * 60);

$time = $hours . ':' . $minutes;

Though some clarification on what happens on daylight savings days would be useful

A: It looks like 1380 is number of minutes for that day.
You can use gmdate(). First convert the minutes into seconds (by multiplying by 60) and then use it in gmdate function.
echo gmdate("h:i A", 1380*60);

redpajama_set_name: RedPajamaStackExchange


Women nowadays are thought to be interested in diverse products and alternatives that might give them an opportunity to look better. Therefore, they in most cases decide to spend sometimes a variety of money in order to obtain best goods such as for instance deodorants etc., thanks to them they maycan look and be more attractive.
In present world, a lot of businesses and individual users are dull and disappointed with items which come from Asia and which quality is very minimal. They are looking to look for the goods which excellence will be satisfied and which will be long lasting and practical in the same time.


On Oahu's northern shore is the quiet town of Hauula.
This neighborhood may be removed from the busy streets of Waikiki giving visitors a relaxing seaside vacation. While in Hauula, guests can visit the beach park of the same name. At Hauula Beach Park, visitors can snorkel safely because of the coral reef that lines the beach itself. Fishing is another popular activity here, which can be done onshore. Fish that can be caught in this area include papio and goatfish. Close to Hauula Beach Park is Kaipapau Beach, another beach in the area. Camping is available on this shore, as well as calming swimming and boating excursions. Another beach is Kokololio Beach, north of Hauula, and it offers a different array of water sports for visitors. During the summer, this beach is safe for swimming. The winter season offers a different array of sports, with body-boarding and surfing being the most popular.
The town of Hauula has a variety of beaches surrounding it giving visitors to the area a myriad of choices for all their water sports adventures.


text:
Tradecraft Update
A new entry in the annals of epic fails:
Bob Quick, Britain's most senior counterterrorism officer, was forced to stand down today after an embarrassing security leak resulted in a major anti-terror operation, designed to foil an alleged al-Qaida plot to bomb Britain, being rushed forward.
….Police were forced to carry out raids on addresses in the north-west of England in broad daylight yesterday, earlier than planned, after Quick, the Metropolitan police's assistant commissioner, was photographed carrying sensitive documents as he arrived for a meeting in Downing Street.
A white document marked "secret", which carried details of the operation being planned by MI5 and several police forces, was clearly visible to press photographers equipped with telephoto lenses.
The Guardian helpfully reproduces an enlarged, rotated, redacted version of the document here.

redpajama_set_name: RedPajamaCommonCrawl


Terry Touchdown, ladies and gentlemen. He was named the Manning Award Quarterback of the Week thanks to his performance down in the Swamp on Saturday.
Wilson went 11-of-16 through the air for 151 yards and two touchdowns and he also rushed for 105 yards and a score. The winner was announced via a Facebook contest where Wilson narrowly received more "likes" than Missouri's Drew Lock. Lock had the better stats, but he didn't end a 31-year losing streak or beat a top 25 team on the road.
Folks, UK's offense is getting more attention than any year I can remember. Maybe 2007? Benny Snell is finally getting noticed nationally and Terry Touchdown isn't far behind.
Let's pad those stats against Murray State, stay healthy and keep this thing rolling.
Also, I know we're all fatigued with jersey talk around these parts but any chance we could make the all-white uniforms the permanent combination, both home and away? Hey, the Cowboys can do it. That was such a sharp look on Saturday night.
Please, don't pad stats. We want the 1st and 2nd teams to come out and play very well, then I would like to see all the young people get as many snaps as possible. Our mistakes against Central Michigan hurt a golden opportunity to empty out our bench against a MAC team, which isn't a terrible conference by any stretch.
Hell yea. Keep it up young man!
Please stop reposting stories. I don't mind meaningless stories. You're Better than this KSR.
Very happy for Terry. He played his way through the adversity of a few early mistakes in each game so far. Can't wait to see him shake off the jitters and play a full game focused and mistake free. Really hoping it happens against Missy State.
Well deserved! It will be interesting to see if they come out flat against Murray State after a huge and emotional win. I think they come out and take care of business.
Sticking to 2-4 uniform combos would be good. Different uni every week seems gimmicky. Leave that to Oregon.
The CAT's been let out of the bag.


Ericom partnerships are based on a shared goal to meet the needs and requirements of our customers by building solutions around them.
Our partners include distributors and resellers, system integrators, and independent software or technology vendors who share Ericom's interest in bringing solutions to industries of all types.
Feel free to contact us and introduce yourself to Ericom, where partnerships tend to grow into successful business opportunities for all.
Technology companies and application software providers that use Ericom solutions to complement their product lines.
System integrators enhance their portfolio with Ericom's access delivery solutions.
Approved companies that sell and support Ericom Software products worldwide.


Home/Blog/Automation in Market 2019 – What Does It Mean?
Automation is getting smarter and virtual ISAs are getting less expensive and more scalable. But at the same time, better trained and more professional. Speed to lead will be even more important than ever before as we enter a shifting market. On the flip side, as the market shifts, the consumer will value the agent more than ever before.
There are several things happening in our industry currently. First, we have a market shift that is taking place. But this is nothing new for our industry, just remember: "there is no such thing as a bad market, it is always good for someone." As real estate agents, we need to identify "whom the market is good for" and adapt to serve their real estate needs which is how you thrive in shifts. The much larger thing taking place, and we will only continue to see more of it, is all these 'disruptors' moving into our space and we will see more of this in 2019. As real estate agents, we can't bury our heads in the sand and not take action — we need to take massive action on this as the future role of the real estate agent depends on it.


Migrants confront Macedonian police during clashes at the Greek-Macedonian border, August 21, 2015.
Macedonian police fired tear gas and stun grenades to drive migrants and refugees back from its southern border from Greece on Friday but crowds continued to build up at a new bottleneck in an increasingly desperate flight to western Europe.
At least 10 people were hurt in the brief flare-up, a day after the impoverished Balkan country declared a state of emergency on its border to halt a daily influx of up to 2,000 Syrians, Afghans, Iraqis and others heading north.
When news that several hundred would be let through every few hours reached those on the border, a crush formed after the first group streamed through.
Amid screams, at least 10 people fainted and were treated by aid workers, a Reuters witness said. Riot police wielding batons held the line.
"We have to protect the border and allow entry to only a number of migrants to whom we can offer adequate, humane treatment," said Interior Ministry spokesman Ivo Kotevski.
Suleiman, 30, from Pakistan said the police were behaving like those back home. "Shame on them. I lost my son in the crush," he said.
Events on Thursday and Friday saw Macedonia become the latest flashpoint of a crisis that has dragged the conflicts of the Middle East – most notably Syria – to Europe's doorstep.
After a cold, damp night in the open in no-man's land, hungry and angry crowds tried to force their way into Macedonia early on Friday. Police responded with tear gas and stun grenades, driving them back. Several people bore leg wounds and Medecins Sans Frontieres said it had treated 10 people on the Greek side.
"The situation is dramatic," said spokeswoman Julia Kourafa.
Amnesty International said it had spoken to some refugees who gave accounts of police beatings and shots being fired in the air. Authorities denied being heavy-handed, and began rationing passage later in the day.
Even with the limited passage, the numbers stranded in no-man's land and stuck on the Greek side threaten to rise. A record 50,000 reached land by boat from Turkey in July alone.
Trying to relieve the pressure on its islands, Greece has begun transporting Syrian refugees by boat to the mainland, from where they head north to Macedonia. A ferry packed with some 2,100 Syrian refugees arrived in Athens from the Aegean islands on Friday.
Macedonia says it has registered over 40,000 migrants and refugees entering from Greece in the past two months; most move quickly through the country to Serbia and then walk into Hungary and on to the more affluent countries of western and northern Europe through the borderless Schengen area.
But the sight of men, women and children from the Middle East, Africa and Asian sleeping in parks in sleepy border towns has angered some in the Balkans, putting pressure on governments to act.
Hungary is racing to complete construction of a fence along its 175 km border with Serbia to keep them out, a step that threatens to create a bottleneck of tens of thousands in Serbia.
A UNHCR official on the ground said Greece estimated between 3,000 and 4,000 men, women and children were in the border area.
The refugee wave has diverted some attention from a political crisis rocking the conservative government of Macedonian Prime Minister Nikola Gruevski for most of the year over allegations of illegal wire-taps, corruption and authoritarianism.
He now faces an early election in April next year. Some commentators suggested it may play well with voters for the government to be seen taking on Greece for allowing thousands of migrants to pour across its northern border.
Macedonia and Greece have long enjoyed an uneasy relationship, rooted in a dispute over Macedonia's name since it broke away from socialist Yugoslavia in 1991. The row has effectively blocked Macedonia's integration with NATO and the European Union.
Macedonia has confronted refugee crises before, most notably in 1999 during the war in Serbia's then southern province of Kosovo when hundreds of thousands of ethnic Albanians took shelter in refugee camps on Macedonia's northern border.


Irvine, CA (April 25, 2018) Soho Network Services won second place among 100 competitors in an international hackathon to design a mobile application.
Soho's vast network of partners means you don't need to deal with a long list of vendors.
Linux/Unix: ...system of choice for ... business clients.
Running a business is difficult enough without the complexities, costs and hassles of managing IT. With today's fast-moving technology, organizations must continuously transform themselves to stay on top of the latest innovations.
When special IT needs arise, whether an emergency situation or a business opportunity requiring IT support, Soho can help. Our one-stop shop provides a full range of services, including data center hosting, process automation, wireless/mobile, VoIP and special projects.
Soho technicians can work at your location or at our operations center to support your IT project quickly and efficiently.
Whether it's a large project (minimum of 15 hours) or long-term IT support, we adapt our IT projects to meet our client's business needs and requirements.


I am looking to embed a dynamic HTML infographic into a storymap. Where is the best place to host the standalone html page on the web? I tried saving it to google drive but couldn't get it to work. If anyone can be of assistance that would be much appreciated. Thanks.
Hi William -- you can host your page anywhere that can host static web pages like a standard web server, Amazon S3, Windows Azure, GoDaddy, etc. Just make sure to make your files public when you upload them or else you won't be able to see them inside the story map.
For example, if we don't have access to servers. Can we place these exported dynamic HTML infographics on DropBox/Box/Google Drive and get a shareable link from them in order to use them in story maps?
Also, are these infographics interactive after we integrate them into our Story Maps or just static images?
I have tried the same but somehow it didnt work and it keeps on loading forever and says "refused to connect".
Would really appreciate if you could help me with this. Thank you.
If you don't have access to external servers, you can host using a web server that your organization uses to host content via their website where you can control CORS and other same-origin headers.


The Fourth Executive Committee Meeting was held in the conference room of NTT Advanced Technology Corporation in Otemachi, Tokyo on the afternoon of Wednesday, October 31, 2001. In this meeting, Fellow Nomination Committee Chair Yoh'ichi Tohkura proposed a revision of the recommendation procedure, to provide nominators with a better guideline for IEEE Fellow Nominations. The recommendation of Fellow candidates will be closed at the beginning of December, and then the committee will determine the candidates who have obtained the Section's endorsement by the end of December.
The third IEEE Japan Council Committee Meeting was held at the Aoba Memorial Building at Tohoku University in Sendai on the afternoon of Friday, October 12, 2001. In this meeting, the tellers committee reported the result of the IEEE Japan Council election of officers for 2002. Dr. Takeo Nakahara, Dr. Yasuyoshi Inagaki, Dr. Keiichi Koyanagi and Dr. Yoichi Hori were elected as Chair, Vice Chair, Secretary and Treasurer, respectively. At this committee meeting, long and middle range aims of IEEE activities in Japan were discussed, based on a report from the Long Range Strategy Committee that was formed in August 2001 for the purpose of reinforcing it. The first committee meeting was held on the morning of October 12 at Tohoku University, prior to the Japan council committee meeting. After the Committee meeting, an information exchange meeting with the Sendai Section followed, where constructive discussions were conducted on the subjects of the Chapter's activities, student activities and membership development.
The Student Branch Leadership Training Workshop was held at the Hongo Campus of Tokyo University on Friday, November 2, 2001, with 40 student participants and the Branch counselors from a total of 13 universities in Japan.
The Student Branches of Tokyo University and Osaka University were recognized on their 25th anniversaries and awarded their Branch banners and commemorative plaques, which were presented by Student Activities Committee Chair Dr. Kiyoharu Aizawa. A noteworthy event was the group discussion, with 6 to 7 students from different universities making up a group, which focused on how to recruit students for IEEE membership. Again, each group contributed a lot of effective and unique ideas.
The Seventh Asia-Pacific Conference on Communications (APCC2001) was held at the University of Electro-Communications on Monday, September 17 through Thursday, September 20, 2001.
During the 4 days, about 300 participants attended the Conference from 17 countries /areas: 213 participants from Japan, 35 participants from Korea, 17 participants from China, and so on. After the keynote address by Dr. Toshiharu Aoki, President of NTT Data, two tutorial sessions, three panel sessions, and several technical sessions were held.
The APCC-IEEE ComSoc APB Joint Award was presented to Mr. Jun-ichi Kani for the most excellent paper entitled: 100Mbps/1Gbps Asymmetric Bandwidth Wide-area Access Network Based on Super-dense WDM Technologies.
Have you renewed your IEEE membership for the year 2002?
By using your IEEE Web Account, you can renew your membership make online.


text:
Which player will be the biggest name at the 2017 World Cup?
TalkSport: The most influential names at the World Cup.What will be their legacy?Will it be the star player or the coach?Who will win?Who could be the most influential?This is the third in a series on the future of football in South Africa and South Africa Football Association (SAFA).
Published by admin in October 12, 2021
Australia's government wants to ban the sale of laptops from the US
Australia's cabinet has approved the controversial move, as it considers the countrys largest electronics retailer to close its doors amid a crackdown on sales of US-made laptops.The decision to scrap the Australian import license was announced in a Cabinet meeting on Thursday, with Industry Minister James Paterson describing the move as "the best-case scenario" and…
Digital music producer to launch new product in Australia
Digital music producers in Australia are set to be among the first to receive a new version of the company's intellectual property solution in the coming months.The new platform will be available in Australia by the end of March.The new platform is named Digital Music Production, and will allow musicians to create and share content…
Published by admin in July 13, 2021


text:
\section{Introduction}
Outflows are very common phenomena of AGNs. They are frequently observed through blue-shifted absorption lines both in UV and X-ray bands (see a review by Laha et al. 2021). In the UV bands, the absorption lines arise from the ions $\rm C_{ IV}$, $\rm N_{ V}$, $\rm O_{ VI}$, $\rm Si_{ IV}$, $\rm C_{ II}$, $\rm Si_{ II}$ and $\rm Fe_{II}$. In the hard X-ray bands, highly ionized outflows are observed through blue-shifted $\rm Fe _{XXV}$ and $\rm Fe _{XXVI}$ K-shell absorption lines (e.g., Pounds et al. 2003; Tombesi et al. 2010, 2011, 2012; Gofford et al. 2013, 2015). The velocity of the hard X-ray absorbers is in the range $0.03-0.3 c$ (with $c$ being speed of light). The mean value is $0.1 c$. The column density is in the range $N_{\rm H} \sim 10^{22}-10^{24} {\rm cm^{-2}}$. Due to its highly velocity, the highly ionized outflows are named ultra-fast outflows (UFOs). The UFOs are believed to originate from the black hole accretion disk. The launching location of UFOs is around hundreds of Schwarzschild radius from the central black hole. The UFOs can be magneto-centrifugally driven (Blandford \& Payne 1982; Fukumura et al. 2015, 2018a) or driven by radiation force due to spectral lines (Murray \& Chiang 1995; Proga et al. 2000; Nomura et al. 2016; Nomora \& Ohsuga 2017; Yang et al. 2021).

In the soft X-ray bands, slowly moving warm gas outflows (warm absorbers) with velocity $100-2000 {\rm km \ s^{-1}}$ are also frequently observed (e.g, Halpern 1984; Reynolds 1997; George et al. 1998; Canizares \& Kruper 1984; Madejski et al. 1991; Kaastra et al. 2000; Kaspi et al. 2000; Reeves et al. 2004; Sako et al. 2001; Behar et al. 2001; Blustin et al. 2004, 2005; McKernan et al. 2007; Laha et al. 2014, 2016). WAs are just mildly ionized with the ionization parameter $\log \xi$ (see Equation 9 for definition) in the range $-1-3 \ {\rm erg\ s^{-1}}$. The column density is in the range $N_{\rm H} \sim 10^{20}-10^{22.5} {\rm cm^{-2}}$. The observed location of WAs is $1-1000 {\rm \ parsec}$ (Blustin et al. 2005).

Two models have been proposed to explain the launching mechanism of WAs. The first one is the magneto-centrifugal driving outflow model (Blandford \& Payne 1982). Fukumura et al. (2018b) have used this magnetohydrodynamic (MHD) scenario to explain the WAs observed in NGC 3783. It is found that the WAs features can be well explained by the MHD scenario if they assume proper radial wind number density distribution and viewing angle.

The second one is the thermal driving outflow model (Begelman et al. 1983; Woods et al. 1996). The accretion disk can be heated up by the X-rays from the region very close to the black hole. When the sound speed of the gas at the disk surface exceeds the local escape velocity, the gas will form outflows. The thermal driving model can be applied to the region far from the black hole, where the escape velocity of outflows is very low. Owing to the slow velocity and low ionization level of WAs, several works have suggested a thermal origin of WAs (Krolik \& Kriss 1995; Krolik \& Kriss 2001; Dorodnitsyn et al. 2008; Mizumoto et al. 2019).

In this paper, we propose a third model for the production of WAs. The velocity of UFOs generated from the black hole accretion disk is much higher than the escape velocity at the location where it is launched. Therefore, the UFOs are capable to move a large distance to interact with the ISM. In this case, the energy/momentum of UFOs can be transferred to the ISM (Pounds \& King 2013). There is the possibility that the WAs are the ISM driven by UFOs. In this paper, we investigate under what ISM conditions the WAs can be driven by UFOs. We also compare the properties of the UFO driven WAs to observations. The purpose of the comparison is to study whether the scenario proposed in this paper is sufficient to produce the observed WAs.

We organize the paper as follows. In Section 2, we introduce our methods including the equations, numerical settings, physical assumptions and initial and boundary conditions of the simulations. In Section 3, we introduce our results. In Section 4, we give discussions. We summarize our results in section 5.

\section{Numerical method }

\subsection{Parameters of UFOs}
Observations show that the mass flux of UFOs is comparable to the accretion rate onto the black hole (Gofford et al. 2015). Therefore, in this paper, we assume that the mass flux of UFOs equals to the accretion rate onto the black hole. We set the accretion rate of the black hole by using the bolometic luminosity ($L_{\rm bol}$) of the AGNs. The black hole accretion rate is calculated by $\dot M_{\rm BH} = L_{\rm bol}/(\eta c^2)$, with $\eta=0.1$ being the radiative efficiency. In some models we set $L_{\rm bol} = 0.1 L_{\rm Edd}$, with $L_{\rm Edd}$ being Eddingtong luminosity. In other models, we set $L_{\rm bol} = 0.5 L_{\rm Edd}$ (see Table 1). One can also calculate the accretion rate of the black hole based on the accretion rate at the inner radial boundary. In such case, because our inner radial boundary is far away from the black hole, one need to assume the radial profile of the mass inflow rate in the region between our inner radial boundary and the black hole horizon. This will complicate the problem. Therefore, in this paper, for simplicity, we give a fixed value to the black hole accretion rate (or $L_{\rm bol}$) and assume that it does not vary with time.

Tombesi et al. (2011) found that the mean and maximum velocities of UFOs are $0.1c$ and $0.3c$, respectively. In this paper, we set velocities of UFOs either equal to $0.1 c$ or $0.3 c$.

The third important parameter of UFOs is its opening angle. We set the opening angle of the UFOs according to the observations of UFOs in some radio-loud AGNs. Tombesi et al. (2014) analyzed the properties of UFOs in some radio-loud AGNs. The inclination angel of the jet in these AGNs is known. Therefore, it is easy to know the angle at which UFOs are present. It is reported that UFOs are detected over a wide range of jet inclination angles ($\sim 10^\circ - 70^\circ$; see also Mehdipour \& Costantini 2019). In our models, we inject UFOs at the inner boundary in the region $10^\circ \leq \theta \leq 70^\circ$ (see the definition of $\theta$  below). The density and velocity of UFOs are assumed to be uniformly distributed in this angular region.

The sound speed of UFOs gas should be significantly smaller than its bulk velocity. Therefore, the internal energy flux of UFOs should be significantly smaller than its kinetic energy flux. In this paper, we set the temperature of the UFOs injected at the inner radial boundary equals to the gas temperature at its adjacent active zone. We have done test by setting a fixed temperature to UFOs, we find that the effects of temperature of UFOs on the results are negligibly small.

\subsection{Equations}
The mass of the central black hole is set to be $M_{\rm BH}=10^9M_{\odot}$, with $M_{\odot}$ being solar mass. We carry out two-dimensional hydrodynamic simulations by using the ZEUS-MP code (Hayes et al. 2006). The spherical coordinates ($r$,$\theta$,$\phi$) are employed. The equations solved are as follows,
\begin{equation}
 \frac{d\rho}{dt} + \rho \nabla \cdot {\bf v} = 0,
\end{equation}
\begin{equation}
 \rho \frac{d{\bf v}}{dt} = -\nabla p - \rho \nabla \Phi
\end{equation}
\begin{equation}
 \rho \frac{d(e/\rho)}{dt} = -p\nabla \cdot {\bf v} + \rho \dot E
\end{equation}
$\rho$, $\bf v$, $e$, $p$, $\Phi$, $\dot E$ are respectively gas density, velocity, gas internal energy per unit volume, gas pressure, gravitational potential of the central black hole, and the net heating/cooling rate per unit mass. Ideal gas equation of state $p=(\gamma-1)e$ is adopted, with $\gamma=5/3$ .

For an AGN, it is generally believed that a compact hot corona is above and below the central black hole (Reis \& Miller 2013; Uttley et al. 2014; Chainakun et al. 2019). The corona emits X-ray photons. Observations of some luminous AGNs have shown that X-ray photons contribute a little to the bolometric luminosity. Therefore, as in previous pioneer work, we assume that X-rays contribute 5 percents of the bolometric luminosity (e.g., Liu et al. 2013). The left 95 percents of the bolometric luminosity are mainly optical/UV photons. We further assume that the X-ray photons are spherically emitted. Therefore, the X-ray flux is
\begin{equation}
F_{\rm X}=0.05 L_{\rm bol} \exp{(-\tau_{\rm X})}/4\pi r^2
\end{equation}
$\tau_{\rm X}=\int_0^r \rho \kappa_{\rm es} dr$ is the scattering optical depth, with $\kappa_{\rm es}= 0.4 \ {\rm cm^2 \ g^{-1}}$ being the Thomson scattering opacity.

\begin{figure*}
\begin{center}
\includegraphics[scale=0.5]{WA600.eps}\hspace*{0.1cm}
\includegraphics[scale=0.5]{WA800.eps}\hspace*{0.7cm}\\
\hspace*{0.5cm} \caption{Distribution of WAs at $5.3 \times 10^7$ year (left panel) and $8.4 \times 10^7$ year (right panel) year for model L0.1v0.3D21T6. Colors denote the logarithm density and arrows show the velocity vector. Note that in this figure, we only show the distribution of WAs. In the regions without WAs, we set the color to dark blue. It does not mean that the regions without WAs have significantly low density. The purpose of plotting this figure in this way is try to protrude the WAs. \label{Fig:vectorWA}}
\end{center}
\end{figure*}

\begin{table*} \caption{Models and results }
\setlength{\tabcolsep}{1.5mm}{
\begin{tabular}{ccccccccc}
\hline \hline
 Model & $\dot m_{\rm inject}$ & $v_{\rm inject}/c$  &  $\rho_0$ & $T_0$ & $C_f$  & $\dot M_{\rm WA}$   & ${\rm \dot E_{kWA}}/L_{\rm bol}$ & ${\rm \dot p}_{\rm WA}/ (L_{\rm bol}/c)$ \\

  & ${L_{\rm Edd}/(0.1 c^2)}$ &  & ($10^{-21}\text{g cm}^{-3}$) & $ 10^5 {\rm K}$ &    & $L_{\rm bol}/(0.1 c^2)$    &  &   \\
(1)    & (2)         & (3)          & (4)         &  (5)  & (6)     &     (7)          &        (8)   & (9)   \\

\hline\noalign{\smallskip}
L0.1v0.1D21T5  & 0.1 & 0.1 & 1 & 1 & $13\%$  &  2.3 & $1.4\times 10^{-4}$ & $6\times 10^{-2}$  \\
L0.1v0.1D22T5  & 0.1 & 0.1& 0.1 & 1 & $6\%$ & 1.2 & $3.6 \times 10^{-5} $ & $3\times 10^{-2}$  \\
L0.1v0.1D23T5  & 0.1 & 0.1& 0.01 & 1 & $10\%$ & 0.7 & $4.5\times 10^{-5} $ & $2\times 10^{-2}$  \\
L0.1v0.1D24T5  & 0.1 & 0.1& 0.001 & 1 & $0.1\%$ & $4\times 10^{-3}$  & $4.8\times 10^{-8}$ & $6\times 10^{-5}$  \\
L0.1v0.1D21T6  & 0.1 & 0.1& 1 & 10 & $11\%$ & 1.4  & $1.1\times 10^{-4}$ & $4\times 10^{-2}$  \\
L0.1v0.1D22T6  & 0.1 & 0.1& 0.1 & 10 & $4\%$ & 0.1  & $6.3\times 10^{-6}$ & $3\times 10^{-3}$  \\
L0.1v0.1D23T6  & 0.1 & 0.1& 0.01 & 10 & $7\%$ & 0.4  & $2.1\times 10^{-5}$ & $1\times 10^{-2}$  \\
L0.1v0.1D24T6  & 0.1 & 0.1& 0.001 & 10 & $6\%$ & 0.4  & $3.3\times 10^{-5}$ & $2\times 10^{-2}$  \\
L0.5v0.1D21T5  & 0.5 & 0.1& 1 & 1 & $6\%$ &  0.3 & $1.9\times 10^{-5}$ & $8\times 10^{-3}$  \\
L0.5v0.1D22T5  & 0.5 & 0.1& 0.1 & 1 & $20\%$ & 4.5 & $4.0\times 10^{-4}$ & $2\times 10^{-1}$  \\
L0.5v0.1D23T5  & 0.5 & 0.1& 0.01 & 1 & $1.7\%$ & $3.7\times 10^{-2}$ & $3.5\times 10^{-6}$ & $1\times 10^{-3}$  \\
L0.5v0.1D24T5  & 0.5 & 0.1& 0.001 & 1 & $0.004\%$ & $2.3\times 10^{-5}$  & $4.3\times 10^{-11}$ & $1\times 10^{-7}$  \\
L0.5v0.1D21T6  & 0.5 & 0.1& 1 & 10 & $47\%$ & 34.9  & $1.1\times 10^{-3}$ & $5\times 10^{-1}$  \\
L0.5v0.1D22T6  & 0.5 & 0.1& 0.1 & 10 & $3\%$ & 1 & $2.0\times 10^{-5}$ & $2\times 10^{-2}$  \\
L0.5v0.1D23T6  & 0.5 & 0.1& 0.01 & 10 & $4\%$ & 0.1 & $1.5\times 10^{-5}$ & $6\times 10^{-3}$  \\
L0.5v0.1D24T6  & 0.5 & 0.1& 0.001 & 10 & $0.005\%$ & $6.8\times 10^{-5}$  & $1\times 10^{-10}$ & $3\times 10^{-7}$  \\
L0.1v0.3D21T5  & 0.1 & 0.3 & 1 & 1 & $23\%$  &  95.6 & $4.4\times 10^{-3}$ & 2.4  \\
L0.1v0.3D22T5  & 0.1 & 0.3& 0.1 & 1 & $52\%$ & 54.5 & $4.7 \times 10^{-3} $ & 2  \\
L0.1v0.3D23T5  & 0.1 & 0.3& 0.01 & 1 & $2\%$ & 0.1 & $2.4\times 10^{-6} $ & $2\times 10^{-3}$  \\
L0.1v0.3D24T5  & 0.1 & 0.3& 0.001 & 1 & $0.01\%$ & $6.4\times 10^{-4}$  & $4.7\times 10^{-8}$ & $2\times 10^{-5}$  \\
L0.1v0.3D21T6  & 0.1 & 0.3& 1 & 10 & $47\%$ & 135  & $3.1\times 10^{-3}$ & 1.8  \\
L0.1v0.3D22T6  & 0.1 & 0.3& 0.1 & 10 & $6\%$ & 0.7  & $7\times 10^{-5}$ & $3\times 10^{-2}$  \\
L0.1v0.3D23T6  & 0.1 & 0.3& 0.01 & 10 & $4\%$ & 0.4  & $7.7\times 10^{-6}$ & $5\times 10^{-3}$  \\
L0.1v0.3D24T6  & 0.1 & 0.3& 0.001 & 10 & $1\%$ & 0.2  & $1.2\times 10^{-5}$ & $6\times 10^{-3}$  \\
L0.5v0.3D21T5  & 0.5 & 0.3& 1 & 1 & $28\%$ &  48 & $3\times 10^{-3}$ & 2  \\
L0.5v0.3D22T5  & 0.5 & 0.3& 0.1 & 1 & $35\%$ & 6.7 & $4.5\times 10^{-4}$ & $2\times 10^{-1}$  \\
L0.5v0.3D23T5  & 0.5 & 0.3& 0.01 & 1 & $0.9\%$ & $2.8\times 10^{-2}$ & $1.8\times 10^{-7}$ & $2\times 10^{-4}$  \\
L0.5v0.3D21T6  & 0.5 & 0.3& 1 & 10 & $29\%$ & 35  & $2\times 10^{-3}$ & 1  \\
L0.5v0.3D22T6  & 0.5 & 0.3& 0.1 & 10 & $4\%$ & 0.6 & $6.9\times 10^{-5}$ & $3\times 10^{-2}$  \\
L0.5v0.3D23T6  & 0.5 & 0.3& 0.01 & 10 & $6\%$ & 0.1 & $1\times 10^{-5}$ & $4\times 10^{-3}$  \\

\hline\noalign{\smallskip}
\end{tabular}}

Note: Col. 1: model names. Col. 2: injected mass flux of UFOs in unit of $L_{\rm Edd}/(0.1c^2)$. Col. 3: velocity of injected UFOs in unit of speed of light. Col 4: the density for initial condition. Col 5. the temperature for initial condition. Col 6. the time-averaged covering factor of WAs. Col 7. the time-averaged mass flux of WAs in unit of the black hole accretion rate. Col. 8: the time-averaged kinetic power of WAs in unit of the bolometric luminosity of the AGN. Col. 9: the time-averaged momentum flux of WAs in unit of $L_{\rm bol}/c$ .
\end{table*}

The last term in Equation (3) is the cooling/heating term. The X-rays from the central black hole region can cool/heat gas by Compton process. The gas can also be heated by photoionization process and cooled by recombination process. Bremsstrahlung cooling and line cooling are also considered. The heating/cooling equations used in this paper are same as those in Proga et al. (2000). The cooling/heating rates are for gas with cosmic abundances. They are as follows,
\begin{equation}
S\rm c=8.9\times10^{-36}n^2(T_X-4T)\xi \ {\rm erg \ cm^{-3} \ s^{-1}}
\end{equation}
\begin{equation}
G\rm x=1.5\times10^{-21}n^2 \xi^{1/4} T^{-1/2} (1-T/T_X) \ {\rm erg \ cm^{-3} \ s^{-1}}
\end{equation}
\begin{equation}
B\rm r=3.3\times 10^{-27}n^2\sqrt{T} \ {\rm erg \ cm^{-3} \ s^{-1}}
\end{equation}
\begin{equation}
\begin{split}
L_{\rm line}=1.7\times10^{-18}{\rm n}^2\exp(-1.3\times10^5/{\rm T})/\xi/\sqrt{\rm T}+\\
            10^{-24} {\rm n}^2 \ {\rm erg \ cm^{-3} \ s^{-1}}
\end{split}
\end{equation}
$S_{\rm c}$, $G_{\rm X}$, $B_{\rm r}$ and $L_{\rm line}$ are Compton heating/cooling, photoionization heating-recombination cooling, bremsstrahlung cooling, and line cooling, respectively. In these equations, ${\rm n}=\rho/\mu m_{\rm p}$ is gas number density, with $\mu=1$ being mean molecular weight and $m_{\rm p}$ being proton mass, respectively. ${\rm T}$ is gas temperature. ${\rm T_X}$ is the Compton temperature of the X-ray photons. As done by Mo\'{s}cibrodzka \& Proga (2013), we set ${\rm T_X}=1.16\times 10^8$ K. $\xi$ is the ionization parameter which is defined as follows,
\begin{equation}
\xi=\frac{4\pi F_X}{\rm n}=0.05 L_{\rm bol} \exp(-\tau_X)/{\rm n} r^2
\end{equation}
The net heating/cooling rate in Equation (3) is expressed as $\rho \dot E=S {\rm c} + G {\rm x} - B {\rm r} - L_{\rm line}$.

\subsection{Initial and boundary conditions}
We study the interaction of UFOs with the ISM in the region from $1 {\rm parsec}$ to $1000 \ {\rm parsec}$. To make the problem as simple as possible, we assume that the ISM has zero angular momentum. Initially, we put ISM with uniform density ($\rho_0$) and temperature ($T_0$) in our computational domain. After a period of evolution, a quasi-steady state of accretion towards the center forms. Then, we inject UFOs from the inner radial boundary. We simulate the region above the midplane, therefore, in $\theta$ direction, we have the domain $0 \leq \theta \leq \pi/2$. Our resolution is $192 \times 64$. In $r$ direction, logarithm grids are adopted in order to well resolve the inner region. In $\theta$ direction, grids are uniformly spaced.

At the inner radial boundary, in the region $\sim 10^\circ - 70^\circ$, we inject UFOs. For other $\theta$ angles, we use outflow boundary conditions. We set the boundary conditions at the outer radial boundary as follows. For a given $\theta$ angle, when we find gas at the last active zone at this angle $v_r < 0 $, then, we inject gas into the computational domain at this angle. The injected gas density and temperature are same as those for the initial conditions. If we find $v_r>0$ at the last active zone at a given $\theta$ angle, then at this angle, outflow boundary conditions are employed. The settings can guarantee continuously gas supplies at the outer boundary. At $\theta=0$, axis-of-symmetry boundary conditions are adopted. At $\theta=\pi/2$, reflecting boundary conditions are employed.

\section{Results}
\begin{figure}
\begin{center}
\includegraphics[scale=0.5]{L0.1v0.3D21T6-NH.ps}\hspace*{0.7cm}
\hspace*{0.5cm} \caption{Angular distribution of the column density of WAs for model L0.1v0.3D21T6. The solid and dashed lines are for $5.3\times 10^7$ year and $8.4\times 10^7$ year, respectively. \label{Fig:NH-WA}}
\end{center}
\end{figure}

We initially set uniform density and temperature in our computational domain. We first run the simulation without UFOs injection. We find that after a period of $\sim 3.8\times 10^7 {\rm year}$, the flow will achieve a quasi-steady state. The indication of the quasi-steady state is that the mass accretion rate measured at the inner radial boundary does not vary much with time. At the quasi-steady state, we inject UFOs at the inner boundary and mark the time when we inject UFOs as ${\rm time} = 0 {\ \rm year}$. After another period, we will find another quasi-steady state. We judge the quasi-steady state as follows. We calculate the total mass outflow rate at the outer radial boundary. When we find that the mass outflow rate does not monotonously decrease or increase with time, but oscillates around a mean value, we think a quasi-steady state has been achieved. We find that after another period of $\sim 3.8\times 10^7 {\rm year}$, the flow will set down to another quasi-steady state. We mark the time at the beginning of the new quasi-steady state as ${\rm time} = 3.8\times 10^7 {\ \rm year}$. We time-average the properties of WAs from ${\rm time} = 3.8\times 10^7 {\ \rm year}$ to ${\rm time} = 9.8\times 10^7 {\ \rm year}$.

We recognize the WAs features to be detected if the following conditions are satisfied: (A) the velocity of outflowing gas with $-1 \leq \log \xi \leq 3 \ {\rm erg\ s^{-1}}$ is in the range $100-2000 {\rm km \ s^{-1}}$. (B) The column density of the outflowing gas satisfying condition (A) is in the range $N_{\rm H} \sim 10^{20}-10^{22.5} {\rm cm^{-2}}$.

\begin{figure}
\begin{center}
\includegraphics[scale=0.5]{vector600.eps}\hspace*{0.7cm}
\hspace*{0.5cm} \caption{Two-dimensional properties of the flow at $5.3 \times 10^7$ year for model L0.1v0.3D21T6. Colors denote the logarithm density (color) and arrows show the unit velocity vector. \label{Fig:vector}}
\end{center}
\end{figure}

The column density of WAs ($N_{\rm H} (\theta)$) is a function of viewing angles between $\theta = 0^\circ$ and $90^\circ$. The covering factor of WAs are calculated as follows,
\begin{equation}
C_f = 4\pi \int^{\pi/2}_0 C_{\rm WA}(\theta) \frac{\sin{\theta} d\theta}{4\pi}
\end{equation}
The parameter $C_{\rm WA}(\theta)$ is defined as follows. At a given $\theta$ angle, if we find that $N_{\rm H} (\theta) = 0$, then we set $C_{\rm WA}(\theta)=0$; when $N_{\rm H} (\theta) \neq 0$, we set $C_{\rm WA}(\theta)=1$. The parameter $C_{\rm WA}(\theta)$ guarantees that we only integrate over viewing angles that having WAs.

The mass flux, kinetic power, and momentum flux of WAs are calculated as follows,
\begin{equation}
\dot M_{\rm WA} = 4\pi r^2 \int^{\pi/2}_0 C_{\rm WA}(\theta) f_{\rm WA} \rho \max(v_r, 0) \sin{\theta} d\theta
\end{equation}
\begin{equation}
\dot E_{\rm kWA} = 2\pi r^2 \int^{\pi/2}_0 C_{\rm WA}(\theta) f_{\rm WA} \rho \max(v_r^3, 0) \sin{\theta} d\theta
\end{equation}
\begin{equation}
\dot {\rm p_{\rm WA}} = 4\pi r^2 \int^{\pi/2}_0 C_{\rm WA}(\theta) f_{\rm WA} \rho \max(v_r^2, 0) \sin{\theta} d\theta
\end{equation}
In Equations (11)-(13), the parameter $f_{\rm WA}$ is defined as follows. If the outflowing gas at a given computational grid has $-1 \leq \log \xi \leq 3 \ {\rm erg\ s^{-1}}$ and $100 \leq v \leq 2000 {\rm km \ s^{-1}}$, we set $f_{\rm WA}=1$. Otherwise, we set $f_{\rm WA}=0$. This can guarantee that the quantities calculated by Equations (11)-(13) are only for WAs.

As shown below, in addition to WAs, UFOs can also drive non-WAs outflows. The properties of the non-WAs outflowing gas (column density, ionization parameter and velocity) do not satisfy the requied conditions of WAs. We define the mass flux, kinetic power, momentum flux of all the outflows (including WAs and non-WAs) as $\dot M_{\rm total}$, $\dot E_{\rm total}$ and $\dot p_{\rm total}$, respectively. We can obtain the values of $\dot M_{\rm total}$, $\dot E_{\rm total}$ and $\dot p_{\rm total}$ by just directly using Equations (11)-(13) with the dropping of the factor of $C_{\rm WA}(\theta) \ f_{\rm WA}$.

There are two ways to obtain time-averaged values of WAs. We take the mass flux of WAs as an example. The first way is as follows. we first time-average the density and velocity. Then, we use the time-averaged density and velocity to calculate the mass flux of WAs. In the second way, we first get the mass flux of the WAs at each snapshot. Then, we time-average the mass flux. If the flow is much laminar, the two ways will give similar results. However, if the flows are quite turbulent, the two ways will give totally different results. For a turbulent system, the first way will erase important information about the true nature of the flow. In this paper, we find that the flow is quite turbulent, therefore, we choose the second way to obtain the time-averaged values of the WAs in Table 1.

We summarize all the models in Table 1. Column 2 gives the injected mass flux of UFOs in unit of $L_{\rm Edd}/(0.1c^2)$. Column 3 gives the velocity of injected UFOs in unit of speed of light. Columns 4 and 5 give the initial density and temperature, respectively. Column 6 gives the time-averaged covering factor of WAs. Column 7 gives the time-averaged mass flux of WAs in unit of the black hole accretion rate. Column 8 gives the time-averaged kinetic power of WAs in unit of the bolometric luminosity of the AGN. Column 9 gives the time-averaged momentum flux of WAs in unit of $L_{\rm bol}/c$.

From Table 1, we can see that generally models with higher density have stronger WAs. We take model L0.1v0.3D21T6 which has strong WAs as our fiducial model to study the properties of WAs.

\subsection{Model ${\rm L0.1v0.3D21T6}$}
We find that the angular location of WAs is changing with time. In order to illustrate this result, we plot Figure \ref{Fig:vectorWA}. This figure shows the distributions of WAs. Colors are for logarithm density of WAs. Arrows show the velocity of WAs. In this figure, the left and right panels are for $5.3 \times 10^7$ year and $8.4 \times 10^7$ year, respectively. Note that in this figure, we only show the distribution of WAs. In the regions without WAs, we set the color to dark blue. It does not mean that the regions without WAs have significantly low density. The purpose of plotting this figure in this way is try to protrude the WAs. It can be easily seen that at $5.3 \times 10^7$ year, WAs are mainly distributed in the region $48^\circ < \theta < 82^\circ$. There is also little amount of WAs in the region $\theta < 30^\circ$. At $8.4 \times 10^7$ year, WAs are distributed in the region $\theta < 45^\circ$. Figure \ref{Fig:NH-WA} shows the angular distribution of the column density of WAs at $5.3 \times 10^7$ year (solid line) and $8.4 \times 10^7$ year (dashed line). This figure also indicates the changing of angular locations of WAs with time. For an AGN, our viewing angle is fixed. Our results indicate that for an AGN, WAs can be observed intermittently. For the observations do not show signiture of WAs, it might not mean that WAs are not present. Instead, WAs may move out of our line of sight.

There are two possible reasons for the changing of angular distributions of WAs. The first reason may be that the angular locations of WAs do vary with time. In order to illustrate the second reason, we plot Figure \ref{Fig:vector}. In this figure, we plot the two-dimensional properties of the flow at $5.3 \times 10^7$ year. Colors show logarithm density including both inflows and outflows. Arrows show unit velocity vector. Comparing this figure to the left panel of Figure \ref{Fig:vectorWA}, we can see that WAs are just parts of the total outflows. For example, there are outflows at $\sim 38^\circ$ close to the outer radial boundary. The outflows at this location do not satisfy the conditions of WAs. We call the outflows do not satisfy the conditions of WAs as non-WAs outflow. If the outflows here keep present but with the properties changing with time, the non-WAs outflows may become WAs. Therefore, the second possible reason for the changing of angular distributions of WAs is that due to the changing of properties, the WAs/non-WAs outflow can become non-WAs/WAs outflows.

\begin{figure*}
\begin{center}
\includegraphics[scale=0.7]{Flux-L0.1v0.3D21T6.ps}\hspace*{0.7cm}
\hspace*{0.5cm} \caption{Time-averaged radial profiles of mass flux (left panel), kinetic power (middle panel) and momentum flux (right panel) of outflows. The solid line is for WAs. The dashed line is for total outflows. \label{Fig:flux}}
\end{center}
\end{figure*}

The time-averaged covering factors of the WAs listed in Table 1 are calculated as follows. We first calculate the covering factor at each snapshot. Then, we do the time-average for the covering factors at different snapshots. The time-averaged covering factor is $47\%$.

A interesting question is that how much mass can be carried away by WAs. We plot the radial profile of the mass flux of WAs in the left panel (solid line) of Figure \ref{Fig:flux}. The mass flux of WAs increases with the increase of radius. This means that when WAs move outwards, more and more gas becomes WAs. The mass flux of WAs is a function of radius. The mass flux of WAs listed in Table 1 is its maximum value. The maximum mass flux of WAs can be more than two orders of magnitude higher than the black hole accretion rate. As introduced above, in addition to WAs, there are also non-WAs outflows. In the left panel of Figure \ref{Fig:flux}, we also plot the mass flux of all the outflows (including both WAs and non-WAs) using a dashed line. The mass flux of all the outflows is more than one order of magnitude higher than that of the WAs.

\begin{figure*}
\begin{center}
\includegraphics[scale=0.5]{ion600D21T6.eps}\hspace*{0.1cm}
\includegraphics[scale=0.5]{ion600D24T6.eps}\hspace*{0.7cm}\\
\hspace*{0.5cm} \caption{Two-dimensional distributions of logarithm of ionization parameter of gas at $5.3 \times 10^7$ year for model L0.1v0.3D21T6 (left panel) and L0.1v0.3D24T6 (right panel). \label{Fig:xi}}
\end{center}
\end{figure*}

The solid line in the middle panel of Figure \ref{Fig:flux} denotes the kinetic power of WAs. The kinetic power of WAs is lower than $0.5 \%$ of the bolometric luminosity. It has been shown that an outflow with kinetic power larger than $0.5\% L_{\rm bol}$ can give sufficient feedback to its host galaxy (e.g., Di Matteo et al. 2005; Hopkins \& Elvis 2010). Therefore, the WAs can not play some important role in regulating the properties of its host galaxy. The kinetic power of the UFOs injected at the inner radial boundary is $1/2 \dot m_{\rm inject} v_{\rm inject}^2 \sim 0.5 L_{\rm bol}$. The kinetic power of all of the outflows ($\dot E_{\rm total}$) is showed by using the dashed line in the middle panel of Figure \ref{Fig:flux}. It can been seen that inside $10 \ \rm parsec$, $\dot E_{\rm total}$ is comparable to that of the injected UFOs. Also, we note that inside $10 \ \rm parsec$, the mass flux of total outflow $\dot M_{\rm total}$ is significantly larger than that of UFOs. The results indicate that the kinetic energy of the UFOs is very effectively transferred into the ISM.  $\dot E_{\rm total}$ decreases with increase of radius. This is because that when moving outwards, the gravity of the black hole do negative work to the outflows. Parts of the kinetic energy of outflows are transferred into their gravitational energy. At the radial outer boundary, $\dot E_{\rm total} \sim 10\% L_{\rm bol}$. Therefore, the UFO driven outflows can have a significant influence on the evolution of its host galaxy.

The kinetic power of outflow is $\dot E = 1/2\dot M v^2$. The momentum flux of outflow is $\dot p = \dot M v$. Therefore, we have $\dot p = 2\dot E/v $ and $\dot p/(L_{\rm bol}/c) = \frac{2 \dot E}{L_{\rm bol}} \frac{c}{v}$. From the middle panel of Figure \ref{Fig:flux}, we can see that $\dot E_{\rm total} \sim L_{\rm bol}$. Also, the velocity of the outflows is significantly smaller than the speed of light. Therefore, the momentum flux of the outflow $\dot p_{\rm total}$ can be significantly higher than $L_{\rm bol}/c$ (see the right panel of Figure \ref{Fig:flux}). The UFOs driven outflow can go to larger radii to interact with the gas in its host galaxy. If the host galaxy gas can very quickly cool down after interacting with the outflows and photons from the central AGN, the behaviour of the gas will be controlled by the momentum carried by the radiation and outflow from the AGN. In such case, the outflows should play much more important role in regulating the properties of the galaxy, because the momentum flux of outflows is significantly higher than that of the radiation.

\begin{figure}
\begin{center}
\includegraphics[scale=0.5]{WA-compare.ps}\hspace*{0.7cm}
\hspace*{0.5cm} \caption{Time evolution of the mass flux of WAs measured at the outer radial boundary. The black and red lines are for models L0.1v0.3D21T6 and L0.1v0.3D21T6-Bn, respectively. \label{Fig:WA-compare}}
\end{center}
\end{figure}
\subsection{Effects of changing properties of gas}
We now investigate the effects of changing the properties of gas. The results in Table 1 show that generally, with the decrease of the gas density, the strength (mass flux, kinetic power, momentum flux) of WAs decreases. The reason is that with the decrease of gas density, the ionization parameter will become larger. The gas is more easily to have ionization parameter larger than the upper limit of the ionization parameter of WAs ($\log \xi = 3$). We take models L0.1v0.3D21T6 and L0.1v0.3D24T6 to do comparisons. Figure \ref{Fig:xi} plots the two-dimensional distribution of $\log \xi$ at $5.3 \times 10^7$ year for model L0.1v0.3D21T6 (left panel) and L0.1v0.3D24T6 (right panel). It is clear that the gas in model L0.1v0.3D24T6 has higher ionization parameter. In a significant larger region in model L0.1v0.3D24T6, the gas has ionization parameter much higher than the upper limit of the ionization parameter of WAs ($\log \xi = 3$). Therefore, models with lower gas density tend to generate weaker WAs.

From Table 1, we see that the initial gas temperature has very little effects on the strength of WAs. The reason is as follows. The mass flux of WAs increases with the increase of radius (see Figure \ref{Fig:flux}). Therefore, most of the WAs are generated at large radii. At large radii ($> 100$ parsec), we find that the cooling/heating timescale calculated as $e/\rho \dot E$, is significantly smaller than the escape timescale ($r/v_r$) of WAs. Therefore, the internal energy of gas can be quickly changed before gas can move a large distance. In other words, because of the quick cooling/heating, gas can quickly lose the memory of its initial internal energy. Thus, the initial gas temperature has little effects on the strength of WAs.

\subsection{Effects of strength of UFOs}
We discuss the effects of strength of UFOs on the properties of WAs. We can change both the velocity and mass flux of UFOs injected at the inner radial boundary. From Table 1, it is clear that generally when the initial gas density is high ($10^{-21} {\rm g \ cm^{-3}}$), with the increase of the velocity or mass flux of UFOs, the WAs will become stronger. This is easy to understand that stronger UFOs can drive stronger WAs. However, we note that the increase of strength of WAs with the increase of strength of UFOs is not significant. When the initial gas density is lower than $10^{-21} {\rm g \ cm^{-3}}$, the effects of changing the strength of UFOs are extremely weak. The reason is as follows. When the initial gas density is much lower, as introduced above, the ionization parameter of gas will be much higher. In this case, the ionization parameter of gas is too higher that only a tiny fraction of the gas can satisfy the ionization parameter criterion of WAs. For such high ionization parameter gas, the increase of strength of UFOs can hardly increase the strength of WAs. The increase of strength of UFOs does help drive stronger outflows. However, most fraction of the stronger outflows still not satisfy the ionization criterion of WAs.

\subsection{Effects of outer boundary conditions}
In this paper, in order to achieve a quasi-steady state, we allow gas to freely move out/into the computational domain at the outer radial boundary (see Section 2.3). This kind of settings can keep continuous supplying of gas into the computational domain from the outer radial boundary. We do find that quasi-steady state can be achieved by using such kind of boundary conditions. The time evolution of the mass flux of the WAs measured at the radial outer boundary for our fiducial model L0.1v0.3D21T6 is shown by the black line in Figure \ref{Fig:WA-compare}. It is clear that the mass flux oscillates around some mean values. A quasi-steady state has been achieved in this model. Note that at some snapshots, the mass flux of WAs at the outer boundary is 0. This is because WAs are not smoothly distributed in the computational domain. They are much clumpy (see Figure \ref{Fig:vectorWA}). There are no WAs at the outer boundary for these snapshots. Another kind of usually adopted boundary condition is the outflow boundary condition. Outflow boundary condition allows gas to freely flow out of the computational domain, but gas is not permitted to go into the computational domain from the boundaries. Therefore, the total mass in the computational domain will keep decreasing with time. We carry out a model L0.1v0.3D21T6-Bn to test the effects of such boundary conditions. The only difference between model L0.1v0.3D21T6-Bn and our fiducial model L0.1v0.3D21T6 is the setting of outer radial boundary conditions. In model L0.1v0.3D21T6-Bn, at the outer radial boundary, we use outflow boundary conditions to not allow gas to flow into our computational domain. The mass flux of WAs measured at the outer radial boundary is shown by the rad line in Figure \ref{Fig:WA-compare}. It is clear that the mass flux decreases with time. After $3\times 10^7$ year, the WAs disappear. The reason is as follows. The UFOs blow out the overlying ISM continuously, without newly injected gas into the computational domain, the only left gas is the UFOs injected from the inner radial boundary. From the analysis above, we conclude that the properties of the WAs mainly depend on the density of the ISM injected into the computational domain from the outer radial boundary.

In a real galaxy, there may be two cases for gas supplies from the galaxy scale to the central AGN. In the first case, gas in the galaxy scale continuously supplies to the central AGN. This case is mimicked by the free inflow/outflow outer boundary conditions used in the models in Table 1. In the second case, there is no gas supplies from the galaxy scale to the central AGN. This case is mimicked by the boundary conditions used in model L0.1v0.3D21T6-Bn.

In our models, we assume that UFOs are always present. In reality, the UFOs may be intermittently produced by the AGN. For the intermittently generated UFOs, there are two related timescales. The first one is how long the UFOs can last once it is produced. The second one is that after the UFOs disappearing, how long it will take for another UFOs to be generated. There is no information about the two timescales from both observations and theory.

We discuss the possible effects of intermittent UFOs in the case that there is no continuously gas supplies from the galaxy scale to the central AGN (boundary conditions in model L0.1v0.3D21T6-Bn). If the UFOs do not last sufficiently long time to push the gas away from our computational domain, the gas with velocity smaller than the escape velocity may fall back after UFOs's shutting down. If the shutting down timescale of UFOs is not so long, the fall back gas may not have sufficient time to go into the region inside 1 parsec. If both the two conditions are satisfied, the WAs may be generated periodically. On a time-averaged sense, this will produce more WAs compared to continuously UFO injection (model L0.1v0.3D21T6-Bn). However, it is not clear whether the two conditions can be satisfied simultaneously. Therefore, it is hard to judge whether can intermittent UFOs produce more WAs.

In the case that there is continuously gas supplies from galaxy scale to the central AGN (the models in Table 1), due to the lack of information about the duration timescale of UFOs, it is also quite hard to guess the effects of intermittent UFOs on the WAs.

\subsection{Comparison to observations}
\subsubsection{covering factor and launching mechanisms}
WAs are detected in $65\%$ of the nearby AGNs (Laha et al. 2016). Assuming that the nearby AGNs are observed with random viewing angles, the covering factor of WAs in these sources is $65\%$. In this paper, we find that the covering factor of WAs varies with numerical settings of the simulations. The covering factor of WAs mainly depends on the gas density. For models with high gas density, the covering factor of WAs can reach a value as high as $52\%$ (model L0.1v0.3D22T5). For models with much lower gas density, the covering factor of WAs can be lower than $0.01\%$. The gas density in the nearby AGNs which show the existence of WAs should vary significantly from source to source. Therefore, in these sources, UFOs may play some role in driving WAs. However, this scenario is not sufficient to explain the high covering factor of WAs in these sources. Other WA driving mechanisms should be at work in these sources.

One possible mechanism is the magneto-centrifugal outflow model (Blandford \& Payne 1982). This model requires that a large scale open magnetic field should be present. The magnetic field is anchored in a thin accretion disk at the midplane. Also, it is required that the angle between the magnetic field line and the accretion disk should be smaller than $60^\circ$. An accretion disk can be present inside hundreds or thousands of Schwarzschild radii. At larger radii, the accretion disk should be gravitationally unstable. Observations show that the distance of WAs to the AGN center has a very broad distribution. The minimum location of WAs can be as small as 0.1 parsec. The maximum location of WAs can reach 1000 parsec or beyond (Laha et al. 2016). We note that, the observed location of WAs should be the upper limit of the distance to the center where the WAs are launched. In other words, it is possible that WAs are launched at a smaller distance to the black hole. After be launched, WAs move to larger radii and then be detected by observations. If the WAs are launched at the accretion disk scale, then the MHD scenario may be applicable. In this case, at the launching point, the outflow may be not recognized as WAs. For example, due to the close distance to the center of the AGN, its ionization parameter may be too high to satisfy the conditions of WAs. When the outflows move to large radii, the properties of outflows (ionization parameter, velocity) may change into the scope of WAs. There is another possibility that WAs are launched at the location where it is observed. In this case, there should be no stably existing accretion disk at the midplane. Consequently, it should be hard to keep an appropriate angle between magnetic field lines and the disk to launch outflows. In this case, the magneto-centrifugal model should be problematic.

The second possible mechanism is the thermally driven outflow model. Mizumoto et al. (2019) studied this mechanism. It is found that the thermal driven outflow model can successfully predict the velocity of the WAs. However, the column density of the thermally driven outflows is lower than the observed value. It is suggested that additional outflow launching mechanism is needed for the WAs (Mizumoto et al. 2019).

The third mechanism is the radiation pressure driven outflow model. The nearby AGNs are mainly sub-Eddington sources. Therefore, the radiation pressure due to Thomson scattering is not possible to driven WAs. In addition, the warm absorbers have temperature around $10^6$ K. The radiation pressure due to spectral lines (line force) can not play a role for such a temperature (Proga 2007). The opacity of dust is much larger than that of the electron scattering, so there is a `force multiplier' effect, which reduces the effective Eddington limit. Fabian et al. (2008) find that the cross-section of dust can be $\leq 100$ for column density $\sim < 10^{21} {\rm cm^{-2}}$. Therefore, the bright nearby AGNs are effectively super-Eddington for low column density dusty gas. Radiation pressure on dust may play some role in driving WAs. However, the WAs with column density $> 10^{21} {\rm cm^{-2}}$ can not be driven by radiation pressure on dust.

In summary, it seems that the WAs can not be driven by a solely mechanism. All the four mechanisms (UFOs driven, magneto-centrifugal driven, thermal driven, radiation pressure driven) may play some role in driving WAs.

\subsubsection{mass flux and kinetic power}
It is quite hard to directly give the mass flux of WAs by observations. The formula often used to estimate the mass flux of outflows in observational literatures is as follows,
\begin{equation}
\dot M \sim \mu m_{\rm p} {\rm n} r^2 v(r) \Omega
\end{equation}
$\Omega$ is the opening solid angle of the WAs. The value of $\Omega = C_f \ 4\pi$. Further assuming that ${\rm n} r \sim N_{\rm H}$, the above equation can be re-written as,
\begin{equation}
\dot M \sim 4 \pi C_f \mu m_{\rm p} r N_{\rm H} v(r) C_v
\end{equation}
$C_v$ is the volume filling factor of WAs. For an AGN, the viewing angle is fixed. One can only obtain the column density along the line of sight. The column density along other directions is not known. Therefore, one should use the parameter $C_v$ to estimate the mean value of the column density. The mean column density equals $C_v N_{\rm H}$. The velocity of WAs can be obtained by using the information of the absorption lines. There are some methods to estimate the location of the absorbers (see Blustin et al. 2005). The only unknown parameter in the above equation is $C_v$. The value of $C_v$ is quite hard to estimate. It must be less than or equal to 1. Blustin et al. (2005) analyzed the properties of WAs in a sample of Seyfert type AGNs. By assuming that the WAs are launched by radiation pressure and setting the momentum flux of the WAs equaling to the radiation momentum, Blustin et al. (2005) found that the value of $C_v$ is
never more than $8\%$. It is found that in $70\%$ of the AGNs in their sample, the mass flux of outflow is greater than the black hole accretion rate. In most of the AGNs in their sample, the kinetic power ($1/2\dot M v^2$) of WAs is found to be significantly less than $1\%$ of the bolometric luminosity.

In the present paper, we find that the mass flux of WAs in some sources can be higher than the black hole accretion rate. However, the kinetic power of WAs in all the models is lower than $1\%$ of the bolometric luminosity (see Table 1). The consistence of our simulation results with the observation results (Blustin et al. 2005) may be a coincidence. The consistence suggests that WAs either by radiation pressure driven (Blustin et al. 2005) or UFOs driven can not supply sufficient feedback to its host galaxy.

\section{Discussion}
The optical depth is used to calculate the ionization parameter of the outflows. When we calculate the optical depth, we only consider the contribution of gas outside 1 parsec. Actually, when the radiation from the vicinity of the central black hole propagates outwards, some portion of photons should be scattered into other directions by the gas inside 1 parsec. It is generally believed that inside 1 parsec, at the midplane, there is a thin disk; above and below the midplane, there is outflow. For the direction along the midplane, the optical depth inside 1 parsec is contributed by the thin disk. It should be much larger than 1. In this case, for the direction along midplane, the optical depth may be significantly larger than that used in this paper. However, the thin disk inside 1 parsec should be significantly thin. Therefore, it can only affect the calculation of optical depth in a negligibly small angular region.  Above and below the midplane, if there are just UFOs outflows, the optical depth contributed by UFOs above and below the midplane is $\sim \mu m_{\rm p} \rho dr \sim \mu m_{\rm p} N_{\rm H}$. Given that the column density of UFOs $<10^{24} \ {\rm cm^{-2}}$ (Tombesi et al. 2011), the optical depth contributed by the gas inside 1 parsec should be smaller than 1. In this case, the contribution to optical depth in the region above and below the midplane by the gas inside 1 parsec is not important.  In addition to UFOs, if there are other types of outflows below and above the midplane inside 1 parsec, the optical depth used in this paper is further underestimated. However, because the ionization parameter of WAs spans four orders of magnitude, the non-accurate optical depth used in this paper should not significantly affect the recognition of WAs.

The gas is assumed to have zero angular momentum. Therefore, the centrifugal force of gas is neglected. The strength of WAs may be underestimated. We note that the omission of centrifugal force may not significantly affect the acceleration of outflows. The reason is as follows. If we assume angular momentum of outflows is conserved when outflows move outwards, we have $v_{\phi} \propto r^{-1}$. The centrifugal force $v_{\phi}^2/r \propto r^{-3}$. The gravitational force $\propto r^{-2}$. The maximum rotational velocity of gas equals to the Keplerian value. Even if gas has Keplerican angular momentum, the centrifugal force only contributes significantly at the starting location of the outflows. When outflows move outwards, the centrifugal force decreases faster than gravity. Therefore, the omission of centrifugal force may not severely affect our results.

\section{Summary}
We perform two-dimensional hydrodynamic simulations to study whether the WAs found in nearby AGNs can be driven by the UFOs. We find that when UFOs collide with the ambient gas, WAs can be generated. The properties (covering factor, mass flux, kinetic power) of WAs mainly depend on the density of the ISM injected into the computational domain from the outer radial boundary. Higher density gas can generate higher covering factor WAs. The highest covering factor of WAs found in this paper is $\sim 50\%$ when the ambient gas has a initial density $10^{-21} {\rm g \ cm^{-3}}$. When the gas has much lower density, the covering factor will become smaller. Observations show that the WAs in nearby AGNs have covering factor $65\%$ (Laha et al. 2016). Therefore, we conclude that UFOs should play some role in driving WAs. However, this scenario alone is not sufficient to explain observations. Other mechanisms should also contribute to the formation of WAs. We also find that the WAs driven by UFOs have kinetic power much lower than $1\%$ of the bolometric luminosity of its host AGN. Therefore, the UFOs driven WAs might not affect the evolution of its host galaxy (e.g., Di Matteo et al. 2005; Hopkins \& Elvis 2010).

\section*{Acknowledgments}
D.-F. Bu is supported by the Natural Science Foundation of China (grant 11773053). X.-H. Yang is supported by the Natural Science Foundation of China (grant 11973018) and the Chongqing Natural Science Foundation (grant cstc2019jcyj-msxmX0581). This work made use of the High Performance Computing Resource in the Core Facility for Advanced Research Computing at Shanghai Astronomical Observatory.

redpajama_set_name: RedPajamaArXiv


The Apps may be used by two types of users: promoters and participants.
Promoters create and manage polls, quizzes and contests, gather answers or entries from participants and have control on such answers or entries.
Participants provide promoters with answers or entries for particular polls, quizzes or contests.
Unless a distinction is indicated, this Policy applies to both promoters and participants.
Promoters may collect personal information through the Apps. They commit to using personal information in accordance with applicable laws and regulations but we do not monitor promoters' practices and take no responsibility for any use or disclosure of personal information by promoters.
We collect basic public information about your Facebook account, such as your name, gender, Facebook ID and email address, when you create an account with us.
We collect information you provide to us by email or via Facebook when you contact us.
We automatically collect browsing information when you use the Apps, such as your IP address, your operating system, the configuration of your browser or mobile device. This information is not associated with your identity unless you created an account with us or provided a promoter with access to your Facebook account.
Promoters collect basic public information about your Facebook account, such as name, gender, Facebook ID and email address when participants provide answers or entries other than anonymously. They may collect additional personal information when participants provide answers or entries to promoters through the Apps, depending of the nature of offered polls, quizzes or contests. Our role with respect to any such additional personal information collected is limited to holding said information for its use by promoters.
Promoters may offer polls, quizzes or contests without disclosing their identities. Participants should be aware that any personal information they provide through the Apps may be collected and retained by promoters, even after a promoter's account is deleted.
We use your personal information to contact you about our services and respond to your enquiries.
We DO NOT (i) use personal information for any other purpose than to provide our services to promoters and participants, (ii) sell personal information, (iii) share personal information with other entities, except as provided in this Policy.
We use information collected automatically on an aggregated basis in order to improve the Apps, develop new features and monitor Apps use.
Promoters may use personal information provided by participants in accordance with their own policies. As a participant, you should review any such available policy before submitting personal information using the Apps. We do not monitor the use of personal information gathered through the Apps by promoters or third-parties. If you provide personal information to a promoter through the Apps, you do so at your own risk, we disclaim all responsibility for any personal information use or disclosure performed by a promoter or third-party.
We will disclose personal information only to the employees, officers or directors of Code Rubik that need to access such information to perform their duties. We may also disclose personal information to suppliers, contractors, consultants or other entities assisting us in the conduct of our business, provided they pledge to keep such information confidential and to the extent that access to such information is necessary in order for said person or entity to perform its obligations towards us.
We store personal information on virtual servers using Heroku. Physical servers are located in North Virginia, USA. Their location may change from time to time but personal information will always be stored within the United States of America. We maintain constant access to information stored on our virtual servers, and personal information is protected with the same security measures as our own confidential information.
You may ask us to access any personal information we hold about you and ask that any error be corrected or such information removed. We will comply with written requests from individuals who are registered with an account to use our services within a reasonable delay, in any case a maximum of thirty (30) days after receipt of a request. We may verify the identity of individuals seeking to access personal information.
As a participant, it may not be possible to retrieve all personal information we may hold about you. Promoters control information gathered via their polls, quizzes or contests and they may remove some information from our database or render it impossible to effectively retrieve.
Removal of information from our servers will render such information unavailable to us or any third-party, but we cannot guarantee that removed information will be impossible to retrieve.
We respect laws and regulations governing the transmission of commercial electronic messages. If you are unhappy with our email communication practices or wish to stop receiving email messages from us, please contact us at the following address: privacy@coderubik.com.
If you have any further questions with respect to our practices regarding privacy, please contact us at the following address: privacy@coderubik.com.


text:
Hexatoma fenestrata är en tvåvingeart som först beskrevs av Enrico Adelelmo Brunetti 1911.  Hexatoma fenestrata ingår i släktet Hexatoma och familjen småharkrankar. Inga underarter finns listade i Catalogue of Life.

Källor

Småharkrankar
fenestrata

redpajama_set_name: RedPajamaWikipedia


You searched for: jamaican clothing! Etsy is the home to thousands of handmade, vintage, and one-of-a-kind products and gifts related to your search. No matter what you're looking for or where you are in the world, our global marketplace of sellers can help you find unique and affordable options. Let's get started!
Find great deals on eBay for Jamaican Dress in Elegant Dresses for Women. Shop with confidence.
Afro-Jamaican leaders are typically charismatic men and women who are said to have special "gifts" or to be "called." Rituals and Holy Places. Rituals include "preaching" meetings as well as special healing rituals and ceremonies such as "thanksgiving," ancestral veneration, and memorial ceremonies.
Find men's clothing, dresses, jeans, and tops in casual, formal and work-ready styles online at cheap prices. Your favorite clothes brands are on sale at Coolmarket the Jamaican clothing & jewelry store. Free shipping on all eligible orders!
High quality Jamaican inspired Women's Clothes by independent artists and designers from around the world.All orders are custom made and most ship worldwide within 24 hours.
Pants as disrespect – Some Rastafari women do wear pants but it is highly discouraged and seen as disrespect to the faith, and he Creator who designed you as a woman. Babylon Colors For Clothing – Rasta women may wear any colors except for pink, blue and purple.
jamaican fglag leggings small & big flag havic Style AND comfort can both be king in one perfect pair of custom leggings. Custom made with care, each pair of leggings is printed before being sewn, allowing for fun designs on every square inch.
Find great deals on eBay for jamaican women clothes. Shop with confidence.
Alibaba.com offers 76 jamaican clothes products. About 11% of these are hangers & racks, 7% are men's t-shirts, and 5% are rhinestones. A wide variety of jamaican clothes options are available to you, such as plus size, breathable, and quick dry.
Clothing and Attire in Jamaica The right clothes can help make your vacation to Jamaica a breeze. particularly for women (but it is best to err on the side of caution!). not be a problem. As long as you pack clothing that is cool and comfortable, you won't look back and regret the clothes you wore on your Jamaican vacation.
Find great deals on eBay for Jamaican Clothing in T-Shirts and Men's Clothing. Shop with confidence.
Women's fashion today is much like traditional Jamaican clothing; consisting of a long dress/skirt and blouse, headband/bandana or hat, and shoes. The dress or skirt covered most of the body and was usually ankle – or calf -length.
Jamaican clothes are comfortable and flamboyant at the same time, just like the mood of the place. From the land of the sun and sea, of coconut palms, reggae, and the Jamaican rum, we might not get a clothing style that is renowned, but it certainly is a style that is different.
5/12/2015 · This feature is not available right now. Please try again later.
Selection of Jamaican Clothing including dresses, t-shirts, swimwear, belts, scarfs and accessories. Shop online at RastaEmpire.com.
Jamaican culture consists of the religion, norms, values, and lifestyle that define the people of Jamaica. The culture is mixed, with an ethnically diverse society, stemming from a history of inhabitants beginning with the original Taino people .
Jamaican Kids T-Shirts for Men at Spreadshirt Unique designs 30-day returns Shop Jamaican Kids Men T-Shirts now!
Both women and men wear lightweight cotton clothing, with men usually dressing in T-shirts or golf shirts and lightweight pants. More than anything else, Jamaicans dress for comfort in the island heat.
Shop for Jamaican Women's Clothing, shirts, hoodies, and pajamas with thousands of designs to choose from and high quality printing.
High quality Jamaican inspired Kids & Babies' Clothes by independent artists and designers from around the world.All orders are custom made and most ship worldwide within 24 hours.


A bid to host the 1953 Worldcon in New York City which was comprised of three New York City fan groups including the venerable Queens SFL and led by Will Sykora. This was an exceptionally complicated race (see 1953 Site Selection results for details, and included two bids from New York City (the other was the Amalgamated Greater New York Fan Groups in '53, led by Dave Kyle, a long-time rival of Sykora's and a Niagara Falls in '53 bid from Upstate.
At the last moment, just before voting at Chicon II, Kyle dramatically withdrew his bid in favor of Philadelphia in '1953 which won. The Queens bid finished fourth.
See 1953 Site Selection results for details.


text:
//
//  Demo_SketchpadSwift-Bridging-Header.h
//  Demo_SketchpadSwift
//
//  Created by SACRELEE on 16/2/25.
//  Copyright © 2016年 SACRELEE. All rights reserved.
//

#ifndef Demo_SketchpadSwift_Bridging_Header_h
#define Demo_SketchpadSwift_Bridging_Header_h

#endif /* Demo_SketchpadSwift_Bridging_Header_h */

redpajama_set_name: RedPajamaGithub


text:
class AddVersionToContentSections < ActiveRecord::Migration
  def self.up
    create_table :content_section_versions do |t|
      t.integer :content_section_id, :version, :author_id
      t.string  :name
      t.text    :contents
      t.timestamps
    end
    add_column :content_sections, :version, :integer, :default => 1
  end

  def self.down
    remove_column :content_sections, :version
    drop_table :content_section_versions
  end
end


text:
About Montana
Area Communities
Jennifer Monroe, Owner Broker – CRS, GRI, AHWD
Jennifer hosted the nationally syndicated American Dream Radio show for one year featuring consumer oriented information related to all facets of real estate. For four years she was the real estate "tip" person on NBC's Montana Today Show offering common sense advice and updates on the latest real estate trends. Originally from Northern California, Jennifer chose Bozeman for the quality of life and excellent schools. She makes an effort to attend local as well as national real estate educational seminars and focuses on national as well as international investment and relocation. Jennifer served on the advisory board for the Sonoran Institute, which promotes community decisions that respect the land and the people of the North American West.
Email Jennifer
Carolyn Goodell, Licensed Sales Associate, GRI
Carolyn was raised in Bozeman, MT and it has been her home for more than 20 years. She loves to travel internationally, and lived in Los Angeles for three years, but decided to move back to the area that she calls home. She bought a home in Livingston and is very familiar with the real estate market there, as well as in Bozeman.
Carolyn graduated with a BA in Elementary Education and worked as a nanny for seven years before deciding to follow in her mother's footsteps and focus on a career in real estate. She was always exposed to the world of real estate through her mother, and enjoyed helping around the office and attending the Parade of Homes each year. She realized that this could become an exciting and rewarding career for herself, and that she had the resources and guidance to make her a competitive and knowledgeable agent.
Carolyn is a member of the Gallatin Association of Realtors® as well as the Southwest Montana Multiple Listing Service. She attends all weekly MLS meetings in Bozeman, which allows her first opportunity to hear about listings fresh to the market and network directly with other active, full time agents servicing the Gallatin and Park County areas.
Email Carolyn
119 North G Street
Livingston, MT 59047
Resources For Sellers
Resources For Buyers
© 2023 Absaroka Realty Inc.