text:
"Glinn" Kattell Seskal--another Seska alter ego
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July 27 2010, 01:57 PM
Nerys Ghemor
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Location: Cardăsa Terăm--Nerys Ghemor
Re: "Glinn" Kattell Seskal--another Seska alter ego
The braids were TOUGH to do--they do seem very thin and very tight in the pics I've seen--but this was just a quick drawing, not a refined portrait.
(One note about that armor...it's a good thing Cardassians seem to be a bit smaller-chested than human women, otherwise the armor could be a problem!)
Are you a Cardassian fan, citizen? Prove your loyalty--check out my fanfic universe,
Star Trek: Sigils and Unions
. Or keep the faith on my AU Cardassia,
Sigils and Unions: Catacombs of Oralius
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A resource for reliable information about significant people, places, events, and things in Minnesota history.
Tired of ethnic discrimination as well as dangerous working conditions, low wages, and long work days, immigrant iron miners on the Mesabi Range in northeastern Minnesota went on strike on July 20, 1907. It was the first organized strike on the state's Iron Range.
Roy W. Meyer's studies of the Dakota and United States policies dealing with them brought about thoughtful public conversation during the late 1960s and 1970s, a time of social turmoil in the country.
Mickey Crimmons and Bert Mattson opened Mickey's Diner, located at 36 West Seventh Street in downtown St. Paul, in 1939. Such diners had gained popularity early in the twentieth century as inexpensive, often all-night, eateries. Built to resemble a rail car, Mickey's was particularly notable for its unique look. Its unusual architecture made it a local landmark, and earned it a place on the National Register of Historic Places.
On April 15, 1913, John Benson opened a Minneapolis law office to offer legal help to the poor. By 2013, the office had morphed into Mid-Minnesota Legal Aid. It has served hundreds of thousands of Minnesotans.
The Moorish/Byzantine-style building at 1004 Oliver Avenue North in Minneapolis was home to the congregation Mikro Kodesh (Holy Assembly) from the 1920s through the 1960s. It is one of the few physical remnants of the now-dispersed North Side Jewish community.
The Minneapolis, St. Paul and Sault Ste. Marie Railroad, commonly known as the Soo Line from a phonetic spelling of Sault, helped Minnesota farmers and millers prosper by hauling grain directly from Minneapolis to eastern markets.
The fifty-three-foot-high Minnehaha Falls was purchased by Minneapolis in 1889. It was the centerpiece of a new state park. The falls remain one of the state's most popular attractions for both residents and visitors. Their name is derived from the Dakota words mni for "water" and gaga for "falling" or "curling"—literally "water fall."
Built in 1929, the Minnesota Building represents a turning point in the economic history of downtown St. Paul and the architectural history of the entire Twin Cities area.
The Minnesota Commission of Public Safety (MCPS) was a watchdog group created in 1917. Its purpose was to mobilize the state's resources during World War I. During a two-year reign its members enacted policies intended to protect the state from foreign threats. They also used broad political power and a sweeping definition of disloyalty to thwart those who disagreed with them.
When the Minnesota National Guard was federalized in the spring of 1917, the state was left without any military organization. To defend the state's resources, the Minnesota Commission of Public Safety (MCPS) created the Minnesota Home Guard. The Home Guard existed for the duration of World War I. Units performed civilian and military duties.
When James C. Burbank began his transportation business in 1851, it was a one-man operation. By 1859, Burbank's Minnesota Stage Company controlled all the major stagecoach lines in the state. In the years before railroads linked Minnesota communities, the Minnesota Stage Company played a crucial role in shaping the commercial and social life of the young state.
Minnesota's boundaries were established by treaties between the U.S. and Great Britain and the formation of the states of Michigan, Wisconsin, Iowa, and Minnesota.
The Minnesota State Public School for Dependent and Neglected Children operated from 1886 to 1947. The campus is one of the most intact examples of a state cottage school standing in the United States, and is significant on a national level.
In 1906, construction began for the Minnesota State Sanatorium for Consumptives, or Ah-Gwah-Ching, about three miles south of Walker in Cass County. Overlooking Shingobee Bay on the south shore of Leech Lake, the hospital evolved into a massive complex of distinctive buildings.
Minnesota State University, Mankato was founded as Minnesota's second normal school in 1868. It went through phases as a normal school, teachers college, college, and university. By 2011 it was one of Minnesota's largest and most comprehensive universities.
From 1881 to 1920, the Minnesota Woman Suffrage Association (MWSA) struggled to secure women's right to vote. Its members organized marches, wrote petitions and letters, gathered signatures, gave speeches, and published pamphlets and broadsheets to force the Minnesota Legislature to recognize their right to vote. Due to their efforts, the Legislature approved the Nineteenth Amendment in 1919.
By 1880 Goodhue County held within its borders four significant Euro-American immigrant enclaves: Minnesota's largest group of Swedish settlers and the second largest assembly of Norwegians, as well as one of the most densely populated German tracts. There was also an Irish colony at the county's center. The settling of Goodhue County serves as a case study of the state's early immigration patterns.
In 1962 and 1963, industrial accidents spilled 3.5 million gallons of oil into the Mississippi and Minnesota Rivers. The oil covered the Mississippi River from St. Paul to Lake Pepin, creating an ecological disaster and a demand to control water pollution.
Before World War II, operating streetcars was considered a man's job. A 1916 Twin City Rapid Transit (TCRT) report shows sixty-eight female employees out of a workforce of 4,300, and those few were telephone operators and clerical office workers.
Mount Sinai Hospital in Minneapolis was among the first private hospitals in the Twin Cities to admit minority doctors on its medical staff. The Jewish community opened the hospital in 1951. By the time Mount Sinai closed in 1991, local hospitals were open to doctors of all races and religions.
In 1856, eight German-Jewish families in St. Paul founded the first Jewish congregation in Minnesota. It was called Mount Zion Hebrew Association. In 2012, Mount Zion Temple had 1,000 members. The synagogue building on Summit Avenue in St. Paul was designed by internationally recognized architect Erich Mendelsohn.
When George D. Munsing came to Minnesota in 1886 to produce a new line of woolen union suits, he founded an underwear empire. From long johns to girdles, the Minnesota company urged generations of consumers, "don't say Underwear, say Munsingwear."
Divorce in Minnesota's nineteenth century Norwegian-Lutheran community was a rarity. Legal separation between a leading pastor and his wife was unheard of. But an 1879 court case in Holden Township led to both those outcomes, and triggered a public debate about married women's legal rights.
Ruth A. Myers was known as the "grandmother of American Indian Education in Minnesota." A persistent voice for American Indian children and their families, Myers focused on education policy. She focused on learning opportunities for American Indian children. She also worked for curriculum and resource materials that reflected the American Indian history and culture for all Minnesota learners.
In July 1902 St. Paul hosted the most important African-American political event of the year: the annual meeting of the National Afro-American Council (NAAC). St. Paul lawyer Fredrick McGhee organized it and hoped that it would produce a more united and effective national civil rights organization. The opposite occurred.

subset: commoncrawl


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Lyrics Depot is your source of lyrics to Silverlight by Fold Zandura. Please check back for more Fold Zandura lyrics. |
Silverlight LyricsArtist: Fold ZanduraAlbum: King Planet I've been the wayward son always moving on I've been wrong I've seen the lows and highs the color of a life and times after all I have seen I'm so blind it's only rain but it's so sweet sounds like music on the city street and at times like this oh, I feel so incomplete here is the only place I know against the walls, stand or fall every word like a shadow comes the waves rolling slow let me see the light, silver light open sky is all I need tonight I come alive when it shines so let me breath the air and let my spirit rise I hear silence and it's lovely voices tell a haunting story I don't believe everything I hear it speaks to me, let it be don't let the sights or sounds people, places drag you down just let the past go, face the future with eyes open wide I've been away so long I've been the wayward son I'm always moving on I've been wrong yeah, I've seen the lows and highs the color of a life and times but after all I have seen I'm so blind it's a wide world, such a wide world you can hide in the shadows for too long praying for light
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Sunday, May 22
Angel Stadium of Anaheim
Attendance: 40,098
Anaheim, CA (Sports Network) - Torii Hunter hit a two-run homer and Tyler Chatwood threw seven innings of one-run ball, as the Angels took the rubber match of their three-game interleague series against the Braves, 4-1.
Chatwood (3-2) limited the Braves to one run on five hits and two walks while fanning six, while Scott Downs and Jordan Walden closed out the win with a scoreless inning apiece.
Bobby Abreu scored a run and knocked in another for the Angels, who had lost five straight coming into the set.
Derek Lowe (3-4) took the loss, Atlanta's fourth in five games, surrendering three runs on five hits and five walks in his six-inning start.
"Lowe pitched well enough to win the ballgame. They got the big hits when they needed to and we didn't," Braves managed Fredi Gonzalez said.
Atlanta went ahead in the second inning when Joe Mather's humpback liner to left knocked in Freddie Freeman.
The lead didn't last long, as Abreu walked leading off the fourth and trotted home on Hunter's fifth home run of the season.
"I haven't seen one of those in awhile," said Hunter, who snapped a 28-game homerless drought. "[Lowe] doesn't make many mistakes and I was able to get one up."
The same duo helped tacked on a pair of runs later on, as Hunter doubled to open the sixth and scored on Alexi Amarista's groundout, and Abreu doubled off the wall in right-center to plate Erick Aybar in the seventh.
Chatwood faced the minimum over his last three innings, Downs hurled a 1-2-3 eighth, and Walden overcame a leadoff single in the ninth to secure his eighth save of the season.
Bob Davidson
D.J. Reyburn
Brian Knight
Jerry Layne


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Donohue wins Rolex 24 endurance race
David Donohue won the 24-hour endurance auto race Sunday at the Daytona (Fla.) International Speedway by 0.167 seconds ahead of Juan Pablo Montoya.
Donohue's victory at the Rolex 24 came on the 40th anniversary of his late father's win at this race, and spoiled a bid by Chip Ganassi Racing for a fourth consecutive Rolex 24 checkered flag.
Donohue passed Ganassi's Montoya with 39 minutes remaining and recorded the closest margin of victory in the race's history.
I'm just proud that I can deliver the goods for the team,
Donohue said. I was just the guy who got to be able to do it.
The previous record for closest finish was in 2000 with a margin of 30.879 seconds.
I was actually surprised we even fought for the win, to be honest,
Joao Barbosa finished in third place, and Max Angelelli was fourth.


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In retail, the shopper's experience is everything. It's how browsing becomes buying, customers become brand advocates and how you, the retailer, influence the purchase path. With the retail solutions offered by Motorola Solutions, you have a partner with the industry knowledge, consumer insight and retail mobile technology solutions to help you build experiences that connect with shoppers and keep them coming back. Learn what's next with our expert insights, resources and trends, so you can be ready to build a stronger business, today.
Try our new RFID ROI Calculator to determine the impact Motorola RFID solutions can have on sales uplift, as well as reduction of safety stock, shrink and out-of-stocks on a monthly and annual basis. Simply input your store, sales and operational information, along with projected growth and estimated costs, to see the financial impact per store and company-wide.
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Current Time
Tuscany restaurants
The area's culinary traditions reflect the gruff, no-nonsense Tuscan character, with its firm territorial roots and resistance to change. You'll find the same classic dishes in most trattorias and many more upmarket places too: bistecca alla fiorentina, the classic Tuscan T-bone steak, cut three or four fingers thick and grilled over a wood fire (preferably oak) for just five minutes on each side; or filling soups like ribollita (a rich vegetable broth with beans and bread) and pappa al pomodoro (another bread soup, this time with tomato, onion, garlic, and a touch of chili). Popular starters include crostini (small rounds of bread, sometimes but not always toasted like bruschetta) with olive paste, beans, liver paste, artichoke purée and other such toppings, while pasta specialties (not as ubiquitous in Tuscany as in some other Italian regions) include papparedelle alla lepre (thick pasta strips in hare sauce) and, south of Siena, pici all'aglione (hand-rolled spaghetti in a tomato and garlic sauce). Finish up with a panna cotta ("cooked cream," a sort of rich blancmange) topped with frutti di bosco (wild berries) or caramel, or opt for the classic Tuscan dinner wrap, cantucci con vin santo—dry almond biscuits served with a glass of dessert wine for dunking and drinking.
At first glance, this historic buca in Lucca's centro storico looks like a parody of an Italian trattoria, with copper pots and whole prosciutti hanging from...more
Perfect for a light lunch, tea, or just a rest stop after trekking through Montepulciano, the historic Art Nouveau café, with its balcony overlooking the...more


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InvestigatorSubmitted by Devo (not verified) on Thu, 02/04/2010 - 5:25am.
Well, how convienent. The lead investigator for some of the cases against R.C. is in trouble. Resulting in cases against R.C. being thrown out. What are the two key words here?..... oh yeh, Politics and Fall guy »
Reply |


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Regardless of what one thinks about the legislation to fast-track the legalization of fracking in North Carolina, you would think that since the bill calls for the state to embark upon an enormously ambitious regulatory/rule-making process over the next several months, lawmakers would want to actually have state employees in place to make it happen.
You would think.
But, of course, we're not talking about a rational situation here; we're talking about the Alice-in-Wonderland world of the 2012 General Assembly. Read More


text: Forums General Hospital AMC – Sonyab's recaps 8/31/11 Viewing 3 posts - 1 through 3 (of 3 total) Author Posts September 1, 2011 at 1:50 am #119405 sonyab1974 703 Posts Botulism. The hospital: Agnes Eckhart (who is none other than the creator of AMC AGNES NIXON) is rushed in. Poor Agnes Eckhart looks so sick! David says there would be no hospital without Agnes. He wants her looked after immediately. Agnes is in her own room. Cara asks what she ate today. Agnes tells her and Cara is sure it's botulism. Later, David comes in to see Agnes and she tells him she was in the tunnel of light and saw his father who had a message for him.:( He's worried about how David turns peoples' lives upside down and that he'll make the wrong choices. Cara leaves. Agnes is so grateful to Cara she wants to help her somehow. David tells her that Cara has an immigration problem. Agnes agrees to help. Later David explains to Cara that Agnes has influenced the state department and she no longer needs to be married to Tad. She can focus on Orpheus. YAY!!!!! Cara is in shock! The way she is looking at David, it looks like she is falling in love with him! Krystal's BJ's: Marissa tells Bianca about JR blackmailing her and about the tape. Poor Marissa doesn't know what to do. Bianca says they'll fight him together. Marissa is sad that this is ruining their happiness. She wanted to tell people in her own way. This video is not how she planned it. She's worried the kids will be harassed. Bianca says they are a family and they will get through it. Wow! Now Marissa has no confidence and Bianca has a lot! Strange. Chandler Mansion: Scott is there!!!! Now where is Madison? JR asks Scott to take a look at his computer. He shows him the video of Marissa and Bianca sex tape. Gee JR does it turn you on? Do you like watching it a lot? Scott is in shock. JR says he needs to blackmail to get and keep his son. Scott threatens to stop him from using the tape. Colby joins them and Scott suggests she ask JR what they were talking about. Colby sees the tape and is NOT happy! Liza comes in and is horrified that there are still copies of the tape around. JR says the deal is off. Colby wants to know what deal. Liza explains the deal is if she helped with AJ, JR would convince Colby to give her mom another chance. Colby is PISSED OFF! Colby wants to move out! JR doesn't want her to but she is going to. Liza says she wants her to move in with her and that she will give her a lot of space. Colby agrees. She and Liza both leave. Scott warns him not to use the tape and leaves. JR is sure his son is coming home. Later, Scott shows up again and tells JR it's a good thing his father isn't around to witness this. And JR's father. JR says Adam will pat me on the back and give me a hand. JR also says that Marissa is a wimp! She will give into his blackmail easy. Marissa and Bianca walk in to confront JR. Marissa is strong and not a wimp. She tells him go ahead and do it. Marissa says if AJ asks where the video came from Marissa will tell him the truth. She isn't going to be the one to hurt AJ it will be him! The ladies leave. Scott says Marissa isn't a wimp afterall. JR isn't happy ROFL! Ellie's grave: Angie is still at Ellie's grave. She is still crying and is very upset. She wants to know about Ellie. Jesse tells her she was tiny and had her dimples. She was an angel. He should have told her right away but couldn't. He comes there every day to tell Ellie how much she's loved. Angie asks where the Lucy came from. She remembers she called out to hold her baby and he handed her Lucy. He says that's almost exactly how it happened. He wanted to will their baby back to life when he heard a baby cry. He thought it was a sign. The baby was left in a box with no identification. Suddenly she realizes the baby is Maya's!!!!! She is in shock!!! She asks when he found out. She can't believe he let Maya look after her own baby. Angie screams at him!!!! They have to tell Maya the truth. Jesse wants to go home but Angie won't leave her baby. She's angry that Jesse kept all of this from her. She tells him to leave her alone with her baby. He walks away but watches her from afar. Martin zoo: Tad tells Dixie that his marriage to Cara wasn't in the cards and doesn't want to talk about it. He knew there was nothing going on between Dixie and David and the past is over. Awwww! Now come on Tad tell David the truth! The truth that you are INLOVE WITH HIM! She wants them to face their issues. Dixie regrets the pain she caused him. Dixie come on!!! Tad hurt you in the past too!!!! He worries about her trusting that oily snake. ROFL! Tad is still jealous and wants David. Dixie cries and Tad reassures her she's forgiven. Awww! Dixie thinks she upset Tad's and Cara's marriage by showing up. That they were in love. He says his marriage to Cara couldn't hold a candle to theirs. Damn straight! They have a chance to pick up where they left off and get it right. Cara suddenly walks in with good news. She got her green card and he's free. YAY!!! Now Tad go and find David and give him a loving hug. Tad never realized that Agnes had that much influence. Cara cries and says she'll never forget what he's done for her. They hug and she leaves. Outside the door, Cara takes her wedding ring off and then gets dizzy. Hmmm baby David Jr? Or Cancer? September 1, 2011 at 6:03 am #841624 Ryan-Scott 156 Posts LOVED SEEING AGNES TODAY! September 1, 2011 at 6:26 am #841628 sonyab1974 703 Posts [quote=Ryan-Scott]LOVED SEEING AGNES TODAY![/quote] Yeah love seeing her!!! It was great! Viewing 3 posts - 1 through 3 (of 3 total) You must be logged in to reply to this topic.


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What does KISM mean in Geology?
This page is about the meanings of the acronym/abbreviation/shorthand KISM in the Academic & Science field in general and in the Geology terminology in particular.
Find a translation for KISM in other languages:
Select another language:
Discuss this KISM abbreviation with the community:
Use the citation below to add this abbreviation to your bibliography:
"KISM." Abbreviations.com. STANDS4 LLC, 2015. Web. 5 Mar. 2015. <http://www.abbreviations.com/term/330972>.
KISM also stands for:
- Kenya Institute of Supplies Management
- Kigezi International School of Medicine
- Kumpulan Ikhtisas Sains Malaysia
... see them all »
Nearby & related abbreviations:
Alternative search:
- Search Kenya Institute of Surveying and Mapping on Amazon
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Pulse Profiles, Spectra, and Polarization Characteristics of Nonthermal Emissions from the Crab-like Pulsars
ABSTRACT We discuss nonthermal emission mechanisms of the Crab-like pulsars with both a two-dimensional electrodynamic study and a three-dimensional model. We investigate the emission process in the outer gap accelerator. In the two-dimensional electrodynamic study, we solve the Poisson equation of the accelerating electric field in the outer gap and the equation of motion of the primary particles with the synchrotron and the curvature radiation processes and the pair-creation process. We show a solved gap structure that produces a gamma-ray spectrum consistent with EGRET observations. Based on the two-dimensional model, we construct a three-dimensional emission model to calculate the synchrotron and the inverse Compton processes of the secondary pairs produced outside the outer gap. We calculate the pulse profiles, the phase-resolved spectra, and the polarization characteristics in optical through gamma-ray bands for comparison with the observation of the Crab pulsar and PSR B0540-69. For the Crab pulsar, we find that the outer gap geometry extending from near the stellar surface to near the light cylinder produces a complex morphology change of the pulse profiles as a function of the photon energy. This predicted morphology change is quite similar to that of the observations. The calculated phase-resolved spectra are consistent with the data from the optical to the gamma-ray bands. We demonstrate that the 10%-20% of the polarization degree in the optical emissions from the Crab pulsar and the Vela pulsar is explained by the synchrotron emissions from the particle gyration motion. For PSR B0540-69, the observed pulse profile with a single broad pulse is reproduced for an emission region thicker and an inclination angle between the rotational axis and the magnetic axis smaller than the Crab pulsar.
- [Show abstract] [Hide abstract]
ABSTRACT: {\it Fermi}-LAT has detected pulsed gamma-ray emissions with high confidences from more than 40 millisecond pulsars (MSPs). Here we study the phase-averaged gamma-ray properties of MSPs by using revised version of a self-consistent outer gap model. In this model, a strong multipole magnetic field near the stellar surface for a MSP is assumed and such a field will be close to the surface magnetic fields ($\sim 10^{11}- 10^{12}$ G) of young ulsars; the outer gap of a MSP is controlled by photon-photon pair production process, where the effects of magnetic inclination angle ($\alpha$) and magnetic geometry have been taken into account, therefore the fractional size of the outer gap is a function of not only pulsar's period and magnetic field strength but also magnetic inclination angle and radial distance to the neutron star, the inner boundary of the outer gap can be estimated by the pair production process of the gamma-ray photons which are produced by the back-flowing particles through the null charge surface; inside the outer gap, a Gaussian distribution of the parallel electric field along the trans-field thickness is assumed, and the gamma-ray emission is represented by the emission from the average radial distance along the central field lines of the outer gap. Using this model, the phase-averaged gamma-ray spectra are calculated and compared with the observed spectra of 37 MSPs given by the second {\it Fermi}-LAT catalog of gamma-ray pulsars, our results show that the {\it Fermi}-LAT results can be well explained by this model. The thermal X-ray emission properties from MSPs are also investigated.11/2013; - SourceAvailable from: P. Caraveo
Article: On the puzzling high-energy pulsations of the energetic radio-quiet $\gamma$-ray pulsar J1813$-$1246
M. Marelli, A. Harding, D. Pizzocaro, A. De Luca, K. S. Wood, P. Caraveo, D. Salvetti, P. M. Saz Parkinson, F. Acero[Show abstract] [Hide abstract]
ABSTRACT: We have analyzed the new deep {\it XMM-Newton} and {\it Chandra} observations of the energetic radio-quiet pulsar J1813$-$1246. The X-ray spectrum is non-thermal, very hard and absorbed. Based on spectral considerations, we propose that J1813 is located at a distance further than 2.5 kpc. J1813 is highly pulsed in the X-ray domain, with a light curve characterized by two sharp, asymmetrical peaks, separated by 0.5 in phase. We detected no significant X-ray spectral changes during the pulsar phase. We extended the available {\it Fermi} ephemeris to five years. We found two glitches. The $\gamma$-ray lightcurve is characterized by two peaks, separated by 0.5 in phase, with a bridge in between and no off-pulse emission. The spectrum shows clear evolution in phase, being softer at the peaks and hardenning towards the bridge. The X-ray peaks lag the $\gamma$-ray ones by 0.25 in phase. We found a hint of detection in the 30-500 keV band with {\it INTEGRAL} IBIS/ISGRI, that is consistent with the extrapolation of both the soft X-ray and $\gamma$-ray emission of J1813. The peculiar X and $\gamma$-ray phasing suggests a singular emission geometry. We discuss some possibilities within the current pulsar emission models. Finally, we develop an alternative geometrical model where the X-ray emission comes from polar cap pair cascades.The Astrophysical Journal 07/2014; 795(2). · 6.28 Impact Factor - [Show abstract] [Hide abstract]
ABSTRACT: We study the phase-averaged spectra and luminosities of γ-ray emissions from young, isolated pulsars within a revised outer gap model. In the revised version of the outer gap, there are two possible cases for the outer gaps: the fractional size of the outer gap is estimated through the photon-photon pair process in the first case (Case I), and is limited by the critical field lines in the second case (Case II). The fractional size is described by Case I if the fractional size at the null charge surface in Case I is smaller than that in Case II, and vice versa. Such an outer gap can extend from the inner boundary, whose radial distance to the neutron star is less than that of the null charge surface to the light cylinder for a γ-ray pulsar with a given magnetic inclination. When the shape of the outer gap is determined, assuming that high-energy emission at an averaged radius of the field line in the center of the outer gap, with a Gaussian distribution of the parallel electric field along the gap height, represents typical emission, the phase-averaged γ-ray spectrum for a given pulsar can be estimated in the revised model with three model parameters. We apply the model to explain the phase-averaged spectra of the Vela (Case I) and Geminga (Case II) pulsars. We also use the model to fit the phase-averaged spectra of 54 young, isolated γ-ray pulsars, and then calculate the γ-ray luminosities and compare them with the observed data from Fermi-LAT.The Astrophysical Journal 02/2013; 765(2):124. · 6.28 Impact Factor
Page 1
arXiv:0707.3301v1 [astro-ph] 23 Jul 2007
Not to appear in Nonlearned J., 45.
Institute of Astronomy and Astrophysics, Academia Sinica; and Theoretical Institute for
Advanced Research in Astrophysics, Academia Sinica and National Tsing Hua University,
Taipei Taiwan
Department of Physics and Institute of Astronomy, National Tsing Hua University,
Hsinchu, Taiwan
We discuss non-thermal emission mechanism of the Crab-like pulsars with
both a two-dimensional electrodynamical study and a three-dimensional model.
We investigate the emission process in the outer gap accelerator. In the two-
dimensional electrodynamical study, we solve the Poisson equation of the accel-
erating electric field in the outer gap and the equation of motion of the primary
particles with the synchrotron and the curvature radiation process and the pair-
creation process. We show a solved gap structure which produces a consistent
gamma-ray spectrum with EGRET observation. Based on the two-dimensional
model, we conduct a three-dimensional emission model to calculate the syn-
chrotron and the inverse-Compton processes of the secondary pairs produced
outside the outer gap. We calculate the pulse profiles, the phase-resolved spec-
tra and the polarization characteristics in optical to γ-ray bands to compare the
observation of the Crab pulsar and PSR B0540-69. For the Crab pulsar, we find
that the outer gap geometry extending from near the stellar surface to near the
light cylinder produces a complex morphology change of the pulse profiles as a
function of the photon energy. This predicted morphology change is quite similar
with that of the observations. The calculated phase-resolved spectra are consis-
tent with the data through optical to the γ-ray bands. We demonstrate that
Page 2
– 2 –
the 10∼20 % of the polarization degree in the optical emissions from the Crab
pulsar and the Vela pulsar are explained by the synchrotron emissions with the
particle gyration motion. For PSR B0540-69, the observed pulse profile with a
single broad pulse is reproduced with a thicker emission region and a smaller in-
clination angle between the rotational axis and the magnetic axis than the Crab
Subject headings: optical-X ray-gamma rays:theory-pulsars:Crab like -radiation
The observed strong γ-ray emissions from the seven young pulsars (Thompson 2003)
show that electrons and positrons are accelerated up to ultra-relativistic regime in the pulsar
magnetosphere. The Crab pulsar (PSR B0531+21), which is one of the brightest and the
youngest γ-ray emitting pulsar, shows the non-thermal emission properties in optical to γ-
ray bands. The observed spectrum of the pulsed photons emitted from the Crab pulsar
extends continuously from optical to γ-ray bands with the spectral index αν, defined as
Iν∝ ν−αν, varying from αν∼ 0 in optical wavelengths, αν∼ 0.5 in X-ray bands, to αν∼ 2
in γ-ray bands. The pulse profile has two peaks in a single period, and the positions of
the pulse peaks across the wide energy range are approximately all in phase (Kuiper et
al. 2001). Interestingly, the pulse profile morphology changes significantly as a function of
the photon energy. The first peak (denoted Peak 1 in the following) dominates in optical
wavelengths. However, the second peak (Peak 2) becomes more and more pronounced for
increasing energies and eventually the Peak 2 emission dominates in soft γ-ray bands. Above
10 MeV photon energy, Peak 1 again dominates Peak 2. The electromagnetic spectrum of
the non-thermal emissions also changes with pulse phases. In the future, the phase-resolved
spectra above 10 MeV will be measured with a sensitivity better than that of the Energetic
Gamma-Ray Experiment Telescope on board the Compton Gamma-ray Observatory by, for
example, GLAST LAT. These observed detail properties for the pulse profiles and the phase-
resolved spectra will be useful to discriminate the proposed emission models.
In addition to the pulse profiles, Kanbach et al.(2005) measured the polarization char-
acteristics of the pulsed photons from the Crab pulsar in the optical wavelengths. The
observation revealed that the degree of the polarization at each pulse peak is lower than
10 % and a large swing of the position angle of the electric-vector of the radiation appears at
each pulse peak. The polarization measurements provide two additional observed properties,
namely, the degree and the position angle of the polarization. In the future, the polarization
Page 3
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of X-ray and soft γ-ray emissions from the pulsar will probably be able to be measured
by ongoing projects such as PoGO (Kataoka et al. 2005) and NCT (Chang et al. 2007)
projects. Therefore, a theoretical study, particularly on the polarization characteristics, is
not only desired, but also timely for the understanding the non-thermal emission process in
the pulsar magnetospheres.
The polar cap accelerator (Ruderman and Sutherland 1975; Daugherty and Harding
1996) and the outer magnetospheric accelerator, the so called outer gap model (Cheng et
al. 1986a,b; Romani 1996), were proposed as the possible acceleration sites in the pulsar
magnetospheres. The traditional polar cap model assumes an acceleration region expanding
several stellar radii from the stellar surface around the magnetic pole. On the other hand,
the traditional outer gap assumes an acceleration region extending beyond the null surface
of the Goldreich-Julian charge density at the outer magnetosphere. The Goldreich-Julian
charge density is given by ρGJ∼ −Ω · B/2πc (Goldreich and Julian 1969) with Ω being the
rotational frequency of the star, B the magnetic field, and c the speed of light. Both models
assume the particle acceleration by an electric field parallel to the magnetic field line. In
the pulsar magnetosphere, the accelerating electric field arises in the region where the local
charge density differs from the Goldreich-Julian charge density.
The slot gap model (Muslimov & Harding 2004), which is an extended polar cap model,
predicts that the acceleration region extends up to near the light cylinder around the last-
open field lines because the pair-formation front, which screens the accelerating electric field,
occurs at higher altitude around there. Two-dimensional electrodynamical studies (Takata
et al. 2004, 2006; Hirotani 2006) suggested that the inner boundary of the outer gap locates
near (or at) the stellar surface because of the current through the outer gap. Although the
recent polar-slot gap and outer gap models both predict similar geometry of the acceleration
region, an important difference between the two models is the electric field configuration in
the accelerator. For the slot gap accelerator, the electric field is stronger nearer the stellar
surface and smaller at higher altitude. On the other hand, the outer gap model predicts a
stronger electric field beyond the null surface and a smaller one below the null surface due
to the screening effect of electron and positron pairs. This difference in the electric field
configuration, and the resultant difference in the acceleration and the emission structures
will appear as a difference in the predicted pulse profiles, the phase-resolved spectra and the
polarization characteristics, which can be examined by a three-dimensional model.
Within the framework of the traditional outer gap model, Romani & Yadigaroglu (1995)
considered a three-dimensional geometry and explained the general features of the observed
pulse profile such as two-peaks in a single period. Subsequently, Cheng et al. (2000, here-
after CRZ00) developed the three-dimensional outer gap model, in which the gap is sustained
Page 4
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self-consistently by the pair-creation process between the primary photons emitted via the
curvature process and the surface X-ray photons. CRZ00 calculated the phase-resolved
spectrum in γ-ray region for the Crab pulsar with the synchrotron radiation and the inverse
Compton scattering of the electron and positron pairs produced outside the gap. Zhang &
Cheng (2002) reconsidered the CRZ00 model to examine the phase-resolved spectra in X-ray
region. However, it has been difficult to explain the detail features of the observed pulse
profiles and phase-resolved spectra with the traditional model. Furthermore, the previous
studies have not discussed the complex features of the observed pulse profiles from optical
to γ-ray bands. Recently, Takata et al. (2007) explained the observed polarization charac-
teristics in the optical wavelengths (Kanbach et al 2005) with the new outer gap geometry.
Jia et al. (2007) examined the phase-resolved spectra by taking account of the emissions
below null charge surface. However, these studies also did not consider the pulse profile,
the phase-resolved spectra and the polarization characteristics in optical to γ-ray bands,
In this paper, we study the emission process of the Crab-like pulsars with the outer
gap accelerator model from both a two-dimensional electrodynamical model and a three-
dimensional emission model point of views. In first part (section 2) of this paper, we will
summarize the results of the two-dimensional electrodynamical study, in which the outer
gap structure for the Crab pulsar is solved with the Poisson equation, the particle motion,
the radiation process and the pair-creation process in meridional plane, following Takata
et al (2004, 2006) and Hirotani (2006). We will show a result which has a consistent GeV
spectrum with the observed phase-averaged spectrum of the Crab pulsar. In the second
part (sections 3 and 4), we will conduct a three-dimensional outer gap model based on the
results of the two-dimensional electrodynamical study. In the three-dimensional study, the
main purpose is to discuss the emission process of optical to γ-ray photons by examining the
morphology change of the pulse profile as a function of the photon energy and the phase-
resolved spectra for the Crab pulsar with the outer gap accelerator model. We will predict
the polarization characteristics through optical to γ-ray bands. We also apply the model
to a Crab-like pulsar, PSR B0540-69. The Crab pulsar and PSR B0540-69 are sometimes
called twin pulsars, because their pulsar parameters are very similar to each other. However,
the observed shapes of pulse profiles are very different to each other. This pair will give an
unique opportunity to examine the model capability.
Important differences between present and previous three-dimensional studies are as
follows. First, we take into account the emissions both below and beyond the null surface as
the electrodynamical study has predicted, while only the emissions beyond the null surface
were taken into account in CRZ00. Secondary we discuss the morphology change of the
pules profile by calculating local emissivity as a function of the photon energy, while the
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previous studies did not discuss the morphology change because they assumed a constant
emissivity when the pulse profiles were calculated. We deal the gyration motion of the pairs
because the gyration motion causes the depolarization for the synchrotron radiation. We
adopt the rotating dipole field in the observer frame, while the previous studies adopted it
in the co-rotating frame. Though these effects were considered in Takata et al. (2007), they
calculated only the synchrotron emission process and presented the phase-averaged spectrum
below MeV energy. In this paper, we extend the model spectrum up to γ-ray bands by
computing also the inverse Compton scattering. Finally, we calculate the collision angle of
the inverse Compton scattering between the pairs and the background synchrotron photons
by tracing the three-dimensional trajectory of the synchrotron photons, while the isotropic
distribution of the back ground photons was assumed in the previous studies (CRZ00). The
collision angle greatly affects to the emissivity of and the polarization characteristics of the
inverse Compton scattering. By including all these effects, we examine the pulse profiles,
the phase-resolved spectra and the polarization characteristics in optical to γ-ray bands,
2. Results of Two-dimensional Electrodynamical Model
In this section, we summarize the results of the two-dimensional electrodynamical study
for the Crab pulsar. Following Takata et al (2004, 2006) and Hirotani (2006) we calculate
the spectrum of the synchrotron and curvature radiation processes of the primary particles
with the electric structure by solving the Poisson equation [∇2Φ = −4π(ρ − ρGJ)], the
equation of motion for the particles, the pair-creation process and the radiation process. As
discussed in Takata el al. (2004, 2006), the electric structure depends on the current and
the gap size, which are model parameters in their studies. In this section, we show a result,
which produces a consistent GeV spectrum with the observations. We ignore the effect of
the gravity which is not important for the dynamics of the outer gap accelerator. We adopt
static dipole field, while in the later section of the three-dimensional study, we apply the
rotating dipole field. The obtained electric structure with the static and the rotating dipole
field did not change very much, because the radial distances to the null charge points, that
is, to the gap position are similar to each other. For the pair-creation process in the gap, we
consider the thermal soft-photons coming from the stellar surface. We adopt kT = 170 eV
for the Crab pulsar (Yakovlev & Pethick 2004). The inclination angle is assumed as α = 50◦.
Thick solid line in Figure 1 shows the solved accelerating electric field along the field line
locating at 50 % of the trans-field thickness from the lower boundary (last-open field line).
Here, we assume 0.1Rlcof the gap thickness at the light cylinder and the outer boundary is
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putted at near the light cylinder. We also assume that 5% of the Goldreich-Julian current,
0.05ΩB/2π, is injected at the outer boundary.
The position of the inner boundary is solved with the current, for which about 22 % of the
Goldreich-Julian current runs through the outer gap in the present case. From Figure 1, we
can see that the inner boundary (r ∼ 0.18Rlc) is inside of the null charge point (r ∼ 0.29Rlc).
As suggested by Takata et al. (2004), the inner boundary is located at the position, on which
jg+j2−j1∼ Bz/B is satisfies, where jgis non-dimensional current created in the gap, j1and
j2are non-dimensional current injected at the inner and the outer boundaries, respectively.
For example, for no injection currents, j1= j2= 0, the inner boundary is located at the
null charge surface, where Bz = 0, if no current is created inside of the gap (jg = 0) as
the vacuum case. On the other hands, if jg ∼ cosα, where α is the inclination angle, is
created, the inner boundary is located at the stellar surface on which Bz/B ∼ cosα is
satisfied around the magnetic pole. In the present case, the inner boundary is located at the
position of about 65 % of the radial distance to the null point with the current components
(jg, j1, j2) = (0.17, 0, 0.05).
Figure 2 shows the calculated synchrotron-curvature spectrum and compares with the
observed phase-averaged spectrum. Sold-line shows spectrum of the intrinsic radiation from
the outer gap, while the dashed-line represents the appearance spectrum after attenuation
of the photons via pair-creation process outside of the gap with the soft photon-field emitted
by the synchrotron process of the secondary pairs. We calculate the initial pitch angle of
the pairs from the propagating direction of the curvature photons and the magnetic field
direction at the pair-creation position. For obtaining the luminosity, we assume the gap
opening angle ∼ 250 degree in the azimuthal direction (see section 3.1).
As dashed-line shows the large amount of the curvature photons above 500 MeV are
converted into the secondary pairs outside of the gap via the pair creation process with
the X-ray photons from the secondary pairs. We find from Figure 2 that the shape of
the spectral energy distribution after absorption becomes relatively flat and explains the
observation above 100 MeV.
The inverse-Compton process of the primary particles in the gap is a possible mech-
anism for TeV emissions. However, the present model predicts the TeV flux for the Crab
pulsar is too low to detect the present Cherenkov telescopes. The soft-photons emitted by
secondary pairs above the gap may not be able to illuminate the gap due to the curvature
of the field lines, and only thermal photons from the stellar surface may be scattered by
the primary particles. In such a case, we found that the intrinsic flux on the Earth be-
comes ∼ 10−15erg/cm2s , which is much small compared with the sensitivity of the present
Cherenkov telescope. On the other hand, some soft-photons emitted by secondary pairs may
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illuminate the outer gap because of the effects of the pith angle. In such a case, we obtained
intrinsic TeV flux which is easily detected by present instruments. However, the optical
depth of the pair-creation for TeV photons is much larger than unity in the magnetosphere,
and the residual TeV photons are a very few, which is difficult to detect with the present
From Figure 2, we can see that the synchrotron and curvature radiations of the primary
particles in the outer-gap does not explain the observed flux below 100 MeV. We consider that
the secondary pairs created outside gap produce below 100 MeV photons via the synchrotron
and the inverse-Compton process. Furthermore, the present two-dimensional model can
compare with only the phase-averaged spectrum. More detailed observation such like the
pulse profile, the phase-resolved spectra and the polarization require a three-dimensional
model. Following sections, therefore, we calculate the emission process of the secondary
pairs and conduct a three-dimensional model.
3.A Three-Dimensional Emission Model
In the following, we conduct a three-dimensional emission model. We anticipate that
the emission direction is coincide with the particle motion in the observer frame. In the
present paper, we adopt the rotating dipole field in the observer frame while it was assumed
in the co-rotating frame in the previous studies (Romani & Yadigaroglu 1995; Cheng et al
2000; Dyks et al 2004). As a results, the magnetic field configurations and resultant the
morphology of emission pattern in the observer frame are different between the present and
the previous studies, but the difference becomes to be important only near the light cylinder.
In the present study, furthermore, we discuss the model in the observer frame only, and we
do not introduce the co-rotating frame.
3.1.Electric field
We have to describe the accelerating electric field into the three-dimensional from. Based
on the result (Figure 1) of the two-dimensional electrodynamical study, we adopt the fol-
lowing three-dimensional form. First, we use the vacuum solution obtained by Cheng et al.
E||(r) =ΩB(r)f2(r)R2
, (1)
beyond the null charge surface, where s(r) is the curvature radius of the magnetic field line
and f(r) is the fractional gap thickness. We can calculate the electric field at each point
Page 8
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having a three-dimensional radial distance, r. Below null surface, we assume 50 % of the
strength of the electric field at the null point given by equation (1). The dashed-line in
Figure 1 shows the electric field strength of the approximation form in the meridional plane.
We can see that the typical strength of the electric field by the two-dimensional electro-
dynamical study (solid-line) in the meridional plane is in general described by the present
simple form (dashed-line). In fact, as long as the gap is geometrically thin in the trans-field
direction and the magnitude of the current is smaller than the Goldreich-Julian value, the
vacuum solution beyond the null charge surface approximately describes the typical strength
of the accelerating field in the meridional plane. Now, we assume that this simple form can
describe also the typical strength of the three-dimensional distribution of the accelerating
electric field.
At each point, the maximum Lorentz factor of the particles are determined by the
force balance between the acceleration by the electric and curvature radiation back re-
action, Γp(r) = [3s2(r)E||/2e]1/4, where Ω2 = Ω/100s−1.
high-energy photons as the curvature radiation process, whose typical energy is Ecurv(r) =
The primary particle emits
p(r)c/4πs(r), and the local power of the curvature radiation is given by lcurv= eE||c.
It is important to estimate the polar cap opening angle of the active region of the outer
gap accelerator. When we consider an open-field line through the outer gap, the pair-creation
process between the primary curvature photons and the surface X-rays mainly occurs near
and below the null charge surface. Therefore, we may be able to relate the opening angle with
the pair-creation mean free path, which is estimated as l(r) ∼ [2s(r)f(r)Rlc] ∼ 2f1/2(Rlc/2)r,
at the null surface. In the present paper, we constrain the width of the polar cap angle of the
active gap by the condition that the mean-free path at the null charge point on the magnetic
field line becomes shorter than the light radius. This condition produces the width of the
polar cap angle of ∼ 250◦.
3.2.Distribution and motion of the secondary pairs
As we demonstrated in section 2, a significant amount of the curvature photons above
∼500 MeV convert into secondary pairs outside the gap via the photon-photon pair-creation
process with the soft-photons emitted by the synchrotron radiation of the secondary pairs.
From Figure 2, furthermore, we can read that the spectrum of the intrinsic emissions has the
photon index of about −1. Therefore, we may approximately describe the local curvature
spectrum with Fcurv ∼ lcurvjnGJ/EcurvEγ, where j represent the current in units of the
Goldreich-Julian value. Using the steady loss equation, d[˙Eedn/dEe]/dEe = Q(Ee), we
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obtain the distribution of the secondary pairs as
lcurvjnGJln(Ecurv/500 MeV)/˙EeEcurv
for 500 MeV < 2Ee< Ecurv
for 2Ee< 500 MeV
where˙Ee= 2e4B2(r)sin2θp(r)Γ2
of the secondary pairs, θp is the pitch angle, and Γe is the Lorentz factor of the pairs.
The local pitch angle will be expressed as sinθp(r) ∝
f(Rlc)(r/Rlc)3/2and s(r) ∼
sinθp(r) = (r/Rlc)1/2sinθp(Rlc) between the pitch angle of the local point and the light
cylinder along the field lines. Outside the gap, the pairs loose most of their energy via the
synchrotron process. Because the synchrotron loss rate˙Eeis proportional to square of the
particle energy, the power law index of the distribution given by equation (2) becomes p ∼ 2,
which produces a synchrotron spectrum with the spectral index of αν∼ 0.5.
In the observer frame, we may describe the particle motion outside the gap with
ec3is the energy loss rate of the synchrotron radiation
?2f(r)RL/s(r). Because f(r) =
√rRlc are satisfied for the dipole field, we may relate with
β = β0cosθpb + β0sinθpb⊥+ βcoeφ,(3)
where the first term and the second term in the right hand side represent, respectively,
the particle motion parallel to the magnetic field and gyration motion, and the third term
represents the co-rotational motion with the non-dimensional velocity βco= ̟/Rlc, where
̟ is the axial distance. The vector b is the unit vector along the field line and b⊥represents
the unit vector perpendicular to the magnetic field line, b⊥≡ ±(cosδφK + sinδφK × b),
where the sign + (or −) corresponds to gyration of the positrons (or electrons), K =
(b · ∇)b/|(b · ∇)b| is the unit vector of the curvature of the magnetic field line, and δφ
represents the phase of gyration around the magnetic field.
ultra-relativistic speed, we determine the value of the coefficient β0from the condition that
|β| = 1. We anticipate that the photons are emitted in the direction of the particle motion
of equation (3).
Because the pairs have an
We note that the synchrotron radiation after collecting of the photons is greatly depo-
larized due to the gyration motion of the pairs, although the intrinsic radiation is highly
polarized. Therefore, the observed small polarization degree ∼ 10 % at the optical bands
for not only the Crab pulsar, but also for the Vela pulsar (Mignami et al. 2007) are easily
reproduced by the synchrotron emission model (Takata et al. 2007).
We assume that the emission region of the secondary pairs extends just above the outer
gap with thickness of the mean free path of the pair-creation λ ∼ 107cm∼ 0.1Rlcfor the
Crab pulsar. Some secondary high-energy photons via the inverse Compton scattering may
convert into the tertiary pairs. The tertiary pairs will be produced above the emission region
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of the secondary pairs, and its initial Lorentz factor will be smaller than that of the secondary
pairs. We also take into account the effects of the emissions from the tertiary pairs.
3.3.Emission process of the secondary pairs and polarization
We consider that the synchrotron radiation and the inverse Compton scattering of
the secondary pairs are major emission mechanisms for the observed non-thermal radia-
tion through optical to γ-ray bands for the Crab-like pulsars. If we estimate the radiation
powers of the synchrotron radiation and the inverse Compton scattering, we obtain
∼ 10
5 · 107erg/cm3
with Uph being the energy density of the synchrotron photons. The estimated value will
explain the observed flux ratio of 1 MeV and 100 MeV emissions of the Crab pulsar. We
calculate only the outward emissions, because the inward emissions are expected to be much
fainter than the outward emissions.
In the calculation, we firstly compute the volume emissivity of the synchrotron radia-
tion and its emitting direction for each radiating point (section 3.3.1). Then, we trace the
propagation of the synchrotron beam to simulate the scattering process by the pairs (sec-
tion 3.3.2). On each scattering point, we calculate the volume emissivity and the polarization
of the inverse Compton scattering for a specific viewing angle of the observer. We perform
this procedure for all calculation points to obtain the total radiation for the specific observer.
This procedure is equivalent with computing the radiation transfer,
= js(k1,ǫ1) + ji(k1,ǫ1),(5)
where I(k1,ǫ1) is the total intensity of the beam propagating in the direction of k1, ǫ1is the
energy of photons in units of the electron rest mass energy, js(k1,ǫ1) is the volume emissivity
of the synchrotron radiation, and ji(k1,ǫ1) represents the amount of the scattered photons
into the direction k1and to the energy ǫ1. We neglect the effects of the absorption, because
the synchrotron self-absorption is not important above optical photon energy, where we are
now interested in. Also, we ignore the effects of the scattering off from the direction k1of
the synchrotron photons, because the scattered photons are tiny amounts of total number
of the synchrotron photons.
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3.3.1.Synchrotron radiation
Assuming that all the synchrotron photons are radiated toward the particle motion
direction, k1= β, the volume emissivity of the synchrotron radiation is calculated from
js(ǫ1) ≡dIs
where δΩ is the solid angle of the radiation, and Fsynis the photon spectrum described by
Fsyn(ǫ1) =31/2e3B(r)sinθp(r)
? ?dne(r)
where ǫsyn(r) = 3heΓ2
units of the electron rest mass energy, Γerepresents the Lorentz factor of the secondary pairs
and F(x) = x?∞
When we calculate the polarization of the synchrotron radiation, we anticipate that
direction of the electric vector of the electro-magnetic wave propagating toward the observer
is parallel to the projected direction of the acceleration of the particle on the sky, Eem∝
a−(k1·a)k1, (Blaskiewicz et al. 1991), where the acceleration vector a derived from equation
(3) is approximately written by a ∼ ±β0ωBsinθp(−sinδφK + cosδφK × b), where ωBis
the gyration frequency. We assume that the radiation at each point is linearly polarized
with degree of Πsyn = (p + 1)/(p + 7/2), where p is the power law index of the particle
distribution. Because the observed radiation is consist of the radiations from the different
particles with the different pitch angle, we assume that the circular polarization will cancel
out and become zero in the observed radiation. The Stokes parameters Qsynand Usynare,
respectively, calculated from dQsyn(k1,ǫ1)/ds = js(k1,ǫ1)cos2ηs(r) and dUsyn(k1,ǫ1)/ds =
js(k1,ǫ1)sin2ηs(r), where ηs(r) is the position angle defined by the angle between the electric
vector of the wave and the projected direction of the rotation axis on the sky, Ωp= Ω −
(k1· Ω)k1.
ec3is the typical photon energy of the pairs in
xK5/3(y)dy with K5/3being the modified Bessel function of order 5/3.
3.3.2. Inverse Compton scattering
To simulate the scattering process, we trace the three-dimensional trajectory of the syn-
chrotron photons. When we trace the trajectory of the synchrotron photons, we define the
Cartesian coordinate such that z-axis is along the rotation axis and the x-axis is in the merid-
ional plane. By ignoring bending of the trajectory due to the gravity, the position of the pho-
tons after traveling distance δs is x(δs) = (x0+kx0δs)cos(δs/Rlc)+(y0+ky0δs)sin(δs/Rlc),
y(δs) = −(x0+kx0δs)sin(δs/Rlc)+(y0+ky0δs)cos(δs/Rlc) and z(δs) = z0+kz0δs, where the
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coordinates (x0, y0, z0) are the radiating point of the synchrotron photon, and (kx0, ky0, kz0)
represents the emission direction at (x0, y0, z0). The emission direction of the background
synchrotron radiation is calculated from equation 3, which takes account the aberration due
to the corotating motion.
Because the mean free path of a synchrotron photon of the scattering is much longer than
the light radius, one can consider that the scattering rate is constant along the path of the
synchrotron photons in the magnetosphere as the first order approximation. We determine
the scattering points at regular interval, which is much shorter than the gap size, along the
path of the synchrotron photons. In the calculation, we first compute the Stokes parameter
of the Compton process in the electron rest frame, and then we transform it to the observer
frame. In the following, the prime and 'non'-prime quantities represent the quantities in the
electron rest frame and the observer frame, respectively. A detail derivation of equations of
the Stokes parameters (8) and (10) are seen in Appendix A.
We denote the specific intensity of the synchrotron radiation propagating to the direction
k0in the observer frame with I0(k0,ǫ0), where ǫ0represents the energy of the background
photons in units of the electron rest mass energy. In the electron rest frame, the background
radiation becomes I′
Doppler factor, β is the velocity of the scattering particles in units of the speed of light,
and Γe = 1/?1 − β2. The polar angle θ0 is defined by the angle between the directions
of the particle motion and of the propagation of the background radiation, which becomes
θ0∼ 0.1 − 0.3 radian in numerically. For the particles with the Lorentz factor 103∼ 104,
optical to X-ray photons are mainly scattered. In this photon energy bands, the synchrotron
photons are distributed with a spectral index of αν∼ 0.5 because the cut-off energy of the
synchrotron spectrum is ∼ 1 MeV and because the particles are distributed with the index
p ∼ 2 (section 3.2). Because the synchrotron beam from each position is strongly collimated,
we approximately describe the background beam, in which the center of the beam is direct to
the polar angle θ0measured from the electron motion direction and the azimuthal direction
φ0, as I0(k0,ǫ)= C0ǫ−0.5δ(θ − θ0)δ(φ − φ0), where C0is evaluated from equation (6).
We are interested in the inverse Compton scattering with the background synchrotron
radiation, which is partially polarized with Πsyn∼ 70%. With unpolarized components of
the background radiation propagating to the direction k0, the volume emissivity juand the
Stoke parameter Quand Uuof the scattered radiation propagating to the direction k1are
calculated from (see appendix A)
1I0(k0,ǫ0), where D1 = ǫ′
0/ǫ0 = Γ−1
e(1 + β cosθ′
0) is a
ju(k1,ǫ1) ≡ dIu(k1,ǫ1)/ds
= (1 − Πsyn)3σT
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(1 − β cosθ1)2(1 + β cosθ′
ucos2ζ − u′
usin2ζ + u′
0− sin2w′
= sin2w′
= sin2w′
where the Stokes parameters are measured from the rotation axis of the pulsar projected
on the sky, and ζ is defined by the angle between the directions of the rotation axis and
the particle motion projected on the sky (Figures 11). The polar angle θ1represents the
propagating direction of the scattered photons measured from the particle motion direction,
wsis the scattering angle defined by cosws= k0· k1and the azimuthal angle η is the angle
between the orthogonal direction to the scattering plane and the direction of the particle
motion projected on the sky.
For the polarized component of the background radiation, the volume emissivity and
the Stokes parameters are calculated from
jp(k1,ǫ1) ≡ dIp(k1,ǫ1)/ds
= Πsyn3σT
(1 − β cosθ1)2(1 + β cosθ′
pcos2ζ − u,psin2ζ
psin2ζ + u′
0− sin2w′
s− (1 + cos2w′
s− (1 + cos2w′
?cos2η′− 2cosw′
?sin2η′− 2cosw′
where λpis the angle between the polarization plane of the background radiation and the
plane of the scattering. By exploring the additive property of the Stokes parameters, the
total volume emissivity and Stokes parameters are, respectively, given by ji = ju+ jp,
dQi/ds = dQu/ds + dQp/ds and dUi/ds = dUu/ds + dUp/ds.
After collecting all photons from the possible points for each rotation phase Φ and a view-
ing angle ξ, the degree of the radiation and the position angle of the electric vector of the radi-
ation are, respectively, calculated from P(ξ,Φ,ǫ1) =
?Q2(ξ,Φ,ǫ1) + U2(ξ,Φ,ǫ1)/I(ξ,Φ,ǫ1)
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and χ(ξ,Φ,ǫ1) = 0.5atan[U(ξ,Φ,ǫ1)/Q(ξ,Φ,ǫ1)], where I(ξ,Φ,ǫ1), Q(ξ,Φ,ǫ1) and U(ξ,Φ,ǫ1)
are the Stokes parameters after collecting photons emitted via both synchrotron radiation
and the inverse Compton scattering. The position angle χ(ξ,Φ,ǫ1) is measured anticlockwise
from the axis of the rotation projected on the sky (Figure 11).
3.4.Model parameter
The inclination angle of the pulsars has been constrained by the polarization measure-
ments of the radio pulsed emissions. However, it has not been strongly constrained the
inclination angle for the Crab pulsar and PSR B0540-69. Therefore, we treat the inclina-
tion angle as a model parameter. The viewing angles ξ of the observer measured from the
rotational axis is also a model parameter. For this local model in the magnetosphere, the
current should be dealt as a model parameter and the position of the inner boundary de-
pends on the assumed current (Hirotani et al. 2003; Takata et al. 2004, 2006; Hirotani
2006). Instead of the current, however, the ratio of the radial distance to the inner boundary
and distance to the the null surface rnis parameterized and is assumed to be constant for
each field line, that is, rin(φ)/rn(φ)=constant, such that the inner boundary locates far away
from the stellar surface if the null surface locates far away. For example, from Figure 1, the
outer gap accelerator with the non-dimensional current j ∼ 0.22 has the inner boundary
at rin(φ)/rφ(φ) ∼ 0.65 in the meridional plane. The altitude of the emission region of the
secondary pairs is also model parameter, because the magnetic field will be modified by rota-
tional and plasma effects near the light cylinder and because the last-open field lines may be
different from the traditional magnetic file lines that are tangent to the light cylinder in the
vacuum case. To specify the upper surface of the outer gap, it is convenient to refer to the
footpoint of the magnetic surface on the star and to parameterize the fractional polar angle
af= θu/θlc, where θuand θlcare the polar angle of the footpoints of the magnetic surfaces
for the gap upper surface and the last-open field line in the vacuum case, respectively. We
constrain the boundary of the radial distance to the emission region to r = Rlc. In this
paper, we apply the model to the Crab pulsar in section 4.1 and to a Crab-like pulsar, PSR
0540-69, in section 4.2.
Page 15
– 15 –
4.Model results
4.1. The Crab pulsar
For the Crab pulsar, we adopt the inclination angle of α = 50◦, the viewing angle of
ξ = 100◦and the position of the inner boundary described by rin(φ)/rn(φ) = 0.67, which
were chosen in Takata et al. (2007). In this paper we chose the fractional angle of af= 1
to explain the phase-resolved spectra, that is, we assume the gap upper surface with the
magnetic field lines that are the conventional last-open field lines in vacuum. The opening
angle of the active outer gap in the azimuthal direction is set at δφ = 250◦, which as assume
in section 3.1.
Figure 3 is the photon mapping of the outwardly propagating photons, where the emis-
sion direction tangent to the local field lines, which is described by af= 1, were temporary
assumed. Figure 4 shows the variations of the typical radial distance to the emission points
of the photons measured by the observer with the viewing angle ξ = 100◦. The dashed-line
in Figure 4 represents the radial distance to the emission points that locate beyond the null
surface on the magnetic field lines coming from the north pole. And, the dotted-lines show
the distance to the points that locate below the null surface on the magnetic field from the
south pole. In the traditional study, only the emission beyond the null surface (dashed-line)
have been considered. We will see that the emission component below null surface is required
to explain the phase-resolved spectrum of Peak 1 (Figure 8). To calculate the phase-resolved
spectra, we define the phase intervals of Peak 1, Bridge, and Peak 2 as 0.06−0.16, 0.29−0.4,
and 0.49 − 0.6 (Figure 4).
4.1.1. Pulse profile and Polarization
Figures 5 and 6 show the predicted variations of the intensity (upper), the position angle
of the electric vector of the radiation (middle) and the degree of the polarization (lower) as a
function of the pulse phase from optical to γ-ray bands. To compare with the observed pulse
profiles in Kuiper et al. (2001), the results were calculated by integrating the photons within
the energy interval 1−10 eV, 0.1−2.4 keV, 20−100 keV, 100−315 keV, 0.75−10 MeV and
30−100 MeV. In the figure, we define the rotation phase Φ = 0 in abscissa axis as lying the
south pole, and the zero degree in the position angle of the bottom panel is corresponding
to the direction of the rotation axis projected on the sky.
In Figures 5 and 6, we see that the calculated pulse profile morphology changes signifi-
cantly as a function of the photon energy likewise the observational pulse profiles (see figure 5
View other sources
Hide other sources
- Available from Jumpei Takata · May 20, 2014
- Available from ArXiv


text:
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Binary Options and signals
February 27, 2015 Working From Home
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For Stretch Fabrics
Designed for stretch woven & knit fabrics with the stretch on crosswise grain. Suggested fabrics: stretch twill, stretch poplin, stretch denim, double knit
Misses' very close fitting slim leg pants have fly zipper, waistband with button or snap closure, and optional pockets and belt loops. View A are full length. View B are cropped and have hemline slits.
German Translations:
Item shipped worldwide.
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Burned out lite bulb Judy T. • Renton, WA • August 28, 2014 Appliance: Model INSIDE DOOR My Repair & Advice Changed it to a new bulb, specifically for Whirlpool appliances. Was this review helpful to you?
Water filter needed replaced Darrell R. • Broken Arrow, OK • July 16, 2014 My Repair & Advice Replace water filter Was this review helpful to you?
Broken pan slide Jose V. • Hayward, CA • March 19, 2014 My Repair & Advice Just insert in the support and done. Was this review helpful to you?
My ice maker was not gettin water so it couldn't make ice the videos and information on this web site show me how to troubleshoot and find out what the problem was ans how to fix it Mary O. • League City, TX • June 21, 2014 My Repair & Advice Test showed it was the infrared sensor, so I ordered the replacement parts, which arrived with standard shipping in just a couple of day. The video on the site show exactly what to do. The fix and installation of the replacement part was quick and easy. My ice maker is producing ice like bran knew. I could not be happier with the service and information provided by this site. Great job guys, really great job. Was this review helpful to you?
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Pronunciation: Yolande Moreau
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Results: 1Comments by: Arcalight |
File: Redtuzk UI04-21-14 |
redtusk UI profile
Posted By: Arcalight
I've installed everything and going from your video everything seems to be in order until I try to set up the UI. When I go to set the profile to RedtuzkUI as shown in the instillation video, that option isn't available. Just has my character name, the server name, class name and "default" as options on the pulldown menu. This goes f...


text:
AC Milan Football Club
- Nickname:Rossoneri
- Founded:1899
- Manager:Filippo Inzaghi
- Ground:Guiseppe Meazza, San Siro
- Capacity:85700
- Last Game: 28-Mar-2012 19:45
- AC Milan
Ambrosini to stay with Milan
12 May 2009 - 10:30:35
AC Milan midfielder Massimo Ambrosini is staying at the San Siro, according to his agent.
Earlier in the season, Ambrosini had cast doubt on his future with the Rossoneri after growing frustrated at a lack of new contract talks and had been linked with a move to Fiorentina.
However, the situation has now improved, according to agent Moreno Roggi, who told Radio Blu: "I'm pretty sure that Max will renew with Milan once again.
"I believe that the Rossoneri will not let go of a player like him. It's true that his contract was short, but every time we find the conditions to renew it.
"I don't think his transfer to Fiorentina this summer is plausible, the conditions do not exist."
Ambrosini, who has made over 350 appearances in his 14 years with the club, is contracted to Milan until the end of next season.
Related AC Milan News
Related AC Milan News


text:
Start learning with our library of video tutorials taught by experts. Get started
Learn how to apply strategic innovation to build better products and services for your company.
Discover nine simple tips to boost your creativity and think about problems in new ways.
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"This has blossomed into a really big thing because now we know it's out there. That's why you see this avalanche now to try and stop it."
Rep. Arthenia Joyner
"Love is the flower of life, and blossoms unexpectedly and without law, and must be plucked where it is found, and enjoyed for the brief hour of its duration."
D.H. Lawrence
"Big. Big, ... We were just starting to blossom with that concept of having Steven in there. We've had visions of some bigger and better things with him. That's going to hurt us."
Bobby Johnson
"Mentally, it took a while. It was a big step back. The team was blossoming and coming together while I was out and to come back and try and fit in with the chemistry they had, it took a while to adjust."
Kristen Newlin
"(Benson) gave us a big lift. He's a great athlete. He's really started to blossom."
Dale Mabrey
"And the day came when the risk to remain tight in a bud was more painful than the risk it took to blossom."
Anais Nin
"A thorn defends the rose, harming only those who would steal the blossom."
Chinese Proverbs


text:
The Big Taste Grill is 20 feet tall, a whopping 65 feet long and 6 feet in diameter. Just to park it you need a space that is at least 20 feet by 90 feet!
The 6,000 pound lid with an 8-foot handle is opened using a hydraulic system, giving access to 440,000 BTUs, which is needed to grill the 1/2 ton of Johnsonville Brats held in the onboard fridge.
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To give the chefs plenty of room to move about as they grill the flavorful sausage...the grill has a 4 foot aluminum walkway along its border.
Johnsonville created the original Big Taste Grill in 1995 to celebrate the company's 50th anniversary. The Big Taste Grill operates at special events like community festivals, major sporting events and retail locations all over the country. Whenever you create something this big and this unique, it attracts a great deal of attention. The Big Taste Grill allows Johnsonville to introduce the great taste of Johnsonville brats to millions of folks in a fun way … all while benefiting deserving non-profit organizations in the communities we visit. Johnsonville donates a portion of its brat sale proceeds to a local charity at each event it serves. Johnsonville asks the benefiting charity to bring their volunteers to the Big Taste Grill to cook and serve the brats.
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3 Stocks to Sell, 2 Excellent Strategies
NEW YORK ( TheStreet) -- At the ripe old age of 36, I scoff at the notion of "sitting in cash." You hear so many people say that in all different types of market environments.
The market rallies. And the worriers "sit in cash" because they expect a pullback, crash or correction.
The market moves wildly. Uncertainty breeds anxiety. Anxiety hates uncertainty. Time to sit in cash.
The market crashes. It's just too much to stomach. I'm in cash.
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Live show from Defcon, including important announcements regarding the future of BinRev and its awesome community. Show notes were lost due to a stupid problem with Lattera's mouse in OSX. Show notes will appear later on. We said during the show we would write in the show notes who won oCTF. Vand won and received a few great prizes.
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Time Warner Cable Enters Partnership With World Golf Champion Ian Poulter
Time Warner Cable announced today that it has partnered with World Golf Champion, Ian James Poulter, in support of its Enjoy Sports Better initiative that helps customers enjoy the sports and teams they love even more. Poulter is an English professional golfer who is a member of the world's top two professional golf tours, the U.S.-based PGA Tour and the European Tour. He has previously been ranked as high as number 5 in the world rankings. The partnership will feature Poulter in a national advertising campaign as well as appearances at golf tournaments and exclusive opportunities with customers in Time Warner Cable markets.
"We're tremendously pleased to have Ian partner with us in support of our Enjoy Sports Better campaign," said Jeffrey A. Hirsch, EVP, Chief Marketing Officer, Residential Services of Time Warner Cable. "He is widely regarded as one of the best putters in the game and without a doubt will also serve as an important voice for our customers who are passionate about all things golf."
In the next few months, Time Warner Cable customers across its footprint can view a new Enjoy Sports Better commercial featuring Poulter and other top athletes. Additionally, customers will have the chance to meet and greet Poulter at golf tournaments where he will be competing.
"I am thrilled to begin the 2013 season with Time Warner Cable as my newest partner," said Poulter. "We both value entertainment as a key component of life! I am looking forward to a long relationship with Time Warner Cable!"
Along with the advertising campaign, Poulter will connect with Time Warner Cable customers via online media including Time Warner Cable's YouTube channel, Twitter and Facebook page, www.facebook.com/twc , where fans will be able to enjoy Facebook chats during PGA Tour events and regular status updates. About Time Warner Cable Time Warner Cable Inc. (NYSE: TWC) is among the largest providers of video, high‐speed data and voice services in the United States, connecting more than 15 million customers to entertainment, information and each other. Time Warner Cable Business Class offers data, video and voice services to businesses of all sizes, cell tower backhaul services to wireless carriers and, through its NaviSite subsidiary, managed and outsourced information technology solutions and cloud services. Time Warner Cable Media, the advertising arm of Time Warner Cable, offers national, regional and local companies innovative advertising solutions. More information about the services of Time Warner Cable is available at www.timewarnercable.com, www.twcbc.com, www.navisite.com, and www.twcmedia.com.Check Out Our Best Services for Investors
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Best Western Olde Maritime Motor Inn - Warrnambool
Corner of Banyan Street & Merri Street - Warrnambool
1-877-662-6988Searching for convenient motel rates in Warrnambool? Take a look at Best Western Olde Maritime Motor Inn!
Wake up to a nice breakfast or enjoy an evening meal at this 3 star Warrnambool motel as it has its own restaurant. You can find a fitness center on site so you will be able to take some time out to de-stress. Guests wishing to relax with a drink will surely want to visit the bar/lounge.
Multilingual staff can provide express check-in. Enjoy complimentary newspapers and a TV in front of the fire in the lobby area, as well as having a safe deposit box at the front desk. Free Wi-Fi is provided. This motel has a business center. Other amenities include dry cleaning/laundry and laundry facilities.
We show TripAdvisor reviews for new Venere hotels that haven't been reviewed yet
Check Availability at Best Western Olde Maritime Motor Inn
Breakfast at Best Western Olde Maritime Motor Inn
A full breakfast is served between 7 AM and 9 AM for a fee.
Facilities at Olde Maritime Motor Inn
- Business Center
- Bar
- Restaurant/Dining
- Laundry service
- Entire property is non-smoking
- Laundry room
- Gym
- Multilingual staff
- Newspapers
- Front desk - safety deposit box
- Luggage room
- Internet/Email services
- TV Lounge
- Free parking
Know before you go
Check-in: after 2 PM.
Check-out: before 10 AM.
Extra-person charges may apply and vary depending on hotel policy.Government-issued photo identification and a credit card or cash deposit are required at check-in for incidental charges.
Special requests are subject to availability upon check-in and may incur additional charges. Special requests cannot be guaranteed.
City tax and/or any other fees charged by the hotel
The following fees and deposits are charged by the property at time of service, check-in, or check-out.
- Breakfast fee: AUD 19 per person (approximately)
- Late check-out fee: AUD 25.00
- Crib (infant bed) fee: AUD 10.00 per night
- Rollaway bed fee: AUD 15.00 per night
The above list may not be comprehensive. Fees and deposits may not include tax and are subject to change.
Best Western Olde Maritime Motor Inn is also known as
Olde Maritime Motor Inn
BEST WESTERN Olde Maritime Motor Inn
Best Western Warrnambool
Warrnambool Best Western
Olde Maritime Motor Inn reviews by TripAdvisor
Room Details
Best Western Olde Maritime Motor Inn has 43 guest rooms, all with iPod docking stations and climate control. Guests can kick back at the end of a busy day and enjoy 32-inch LCD televisions with digital channels. Corporate travelers visiting the Warrnambool area will benefit from free wireless high-speed Internet access as well as phones. A good night's sleep in comfortable beds with premium bedding will have visitors waking up refreshed and well-rested throughout their vacation or business trip.
Private bathrooms are outfitted with showers. Irons/ironing boards, minibars, coffee/tea makers and hair dryers are supplied in each room to facilitate basic travel needs. Additional comforts include air conditioning.
Accommodation Services
- Telephone
- Air conditioning
- Mini bar
- Extra beds
- Coffee and tea maker
- Baby cots/cribs available
- Hairdryer in each room
- In-room ironing facilities
- Individually controlled air conditioning
- LCD flat screen TV
- Wireless Internet access
Distances from Olde Maritime Motor Inn
Flagstaff Hill Maritime Village - 0.2 km / 0.1 miWarrnambool Beach - 0.5 km / 0.3 mi
Warrnambool Botanical Gardens - 1.6 km / 1 mi
Warrnambool Golf Club - 2 km / 1.3 mi
Tower Hill Wildlife Reserve - 11.9 km / 7.4 mi
Port Fairy to Warrnambool Rail Trail - 15.2 km / 9.4 mi
Port Fairy Golf Club - 18.1 km / 11.2 mi
Griffiths Island Lighthouse - 19.9 km / 12.4 mi
Bay of Islands Coastal Park - 27.3 km / 16.9 mi
Port Campbell Foreshores - 51.4 km / 31.9 mi
Port Campbell Visitor Information Centre - 51.4 km / 31.9 mi
Wreck Beach - 75.4 km / 46.8 mi
Johanna Beach - 88.2 km / 54.8 mi
Great Otway National Park - 107.9 km / 67 mi
Apollo Bay Harbour - 111.6 km / 69.4 mi
The preferred airport for Best Western Olde Maritime Motor Inn is Melbourne, VIC (MEL-Tullamarine) - 222 km / 138 mi.
Distances are calculated in a straight line from the property's location to the point of interest or airport and may not reflect actual travel distance.
Distances are displayed to the nearest 0.1 mile and kilometer.
Transportation services Best Western Olde Maritime Motor Inn
- Free parking
We have the accommodation you need, all over the world
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Posts tagged rockstar presents table tennis
TGS: Today's Marketplace content, 9/21 [update 1]
Another day, another batch of content. TGS rolls on, and Microsoft gives us more to drool over. Now, without further ado, today's content: Vista Game Montage Fusion Frenzy 2 trailer (Weren't we just talking about this?) Kingdom Under Fire: Circle of Doom trailer Team Fortress 2 trailer Table Tennis...
Get your Table Tennis (demo) on
As many of you have already pointed out, the Table Tennis demo has hit Marketplace (even in Europe). If you'd like a description of the game, please see the above picture. That's really all there is to it. Clean, simple fun. If you haven't tried it out, give it a spin and tell us what you think. No...
Airborne is online
A trailer for Medal of Honor Airborne is now available on marketplace. I have not had the luxury of checking it out yet so, somebody get busy describing it in the comments. Why haven't I gotten it yet, you say? I was doing my patriotic duty, or jury duty to be more specific. In other news, expect a...
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Off the Grid: The Witcher Adventure Game and Star Wars Imperial Assault
Posted on Feb 3rd 2015 2:15PM