The Rumpus Room was everyone's dysfunctional home away from home. With the décor scheme of your parents' 1980s rec room, The Rumpus Room was decked out with knickknacks that usually take a lifetime of garage sale scouring to acquire. The menu at the Rumpus Room was a fun and kitchy mix of deep-fried pickles, freshly baked apple pie and delicious breakfast poutine. Sadly, the Rumpus Room closed in 2014 when its location was slotted for redevelopment. We are currently hunting for a new location.


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redpajama_set_name: RedPajamaCommonCrawl


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Rochester stifles Post 72
By Mike WhaleyAssistant Sports Editor
Jun 27, 2007 at 7:25 AM Jun 27, 2007 at 1:52 PM
ROCHESTER — After surrendering 25 runs in a pair of District A losses last week, Rochester Post 7 used a weekend trip to a wooden-bat tournament in Burlington, Vt., to get its mojo back.
Post 7 won all five games it played during its Vermont swing, using the Green Mountain momentum as a springboard to its first district win Tuesday over Alton Post 72, 14-1 in seven innings via the mercy rule, at Bert George Field.
Rochester scored eight runs in the first four innings and closed out the game with a six-run sixth. Post 7 (1-2) pounded out 15 hits off three Alton pitchers, while Post 72, which stranded nine base runners, managed just six hits off Rochester starter and winner, Eric LaBatte, who fanned five and walked two.
"Coach (Sean) Evans worked with me over the weekend and gave me some confidence, and showed me a few minor adjustments," said LaBatte, who had struggled with his control in recent outings. "I went out there and stayed relaxed and just tried to throw strikes. Sometimes I try (to) overpower kids and it just doesn't work. So I just put it down the middle, worked my spots and let them hit it and let the defense make some plays."
"This is the worse loss that we've had," said Alton coach Jim Grant, whose team had lost 6-5 on Sunday to district leader, Portsmouth, and 7-5 on Saturday to a strong Salem club. "Four of our losses have been by two runs or less. Tonight was disappointing. We've been right there, right there, but tonight wasn't the night. Something wasn't clicking for us. And Rochester hit the ball well."
LaBatte's RBI single plated the first Post 7 run in the first, and Jamie Ferullo's home run over the fence in left field made it 2-0 in the second. A four-run third featured Will Fisher's three-run homer off Alton starter Alex Bourdeau. An error and LaBatte's sacrifice fly widened the gap to 8-0 in the fourth.
A pivotal inning for Alton (0-7) proved to be the third. Trailing 2-0, Alton's first two batters reached: Nate Gonya on an error and Jim Grant on a bunt single. However, the three, four, five batters in the lineup went in order on harmless balls in the air and Alton's one serious chance to get back in the game was gone.
"I don't know if that home run (by Ferullo) set us back," Coach Grant added. "It seemed to take some of the gas out of it. Alex (Bourdeau), we had to pull him off the mound, he just wasn't feeling well, struggling with a fever. That didn't help any. Little things just ate us up tonight. Rochester did a good job of running the bases and getting guys going. They were going to steal until we threw them out. So they played a good game on the bases."
Alton scored its only run in the fifth when Gonya reached on a fielder's choice, moved to second on a base hit by Grant (two of Alton's six hits), and then third on a throwing error. Gonya scored on Alex Bourdeau's groundout.
Rochester, which had all nine starters collect at least one hit, wrapped the game up in the sixth with six runs on six hits. Chris Campbell (2 for 4, 2 runs, 2 RBIs) and Mark Wiggins collected RBI doubles, while LaBatte (2 for 2, 2 runs, 3 RBIs) knocked in one run with a single and Matt Warren stroked a sacrifice fly. Leadoff hitter J.R. Santaniello (3 for 4, 4 runs, 2 RBIs, 2 SBs) closed out the scoring with a two-run single to center.
In the seventh, LaBatte got the first out, and then issued back-to-back walks, his first two of the night, to Gonya and Jeff Feeny. However, LaBatte regained his composure and ended the game with a strikeout and groundout.
"(LaBatte) needed a good outing. He pitched well enough to win, I don't care who we play," said Post 7 coach Dave Hoyt. "The only time he struggled was that last inning when he walked two."
Rochester hosts Sweeney tonight, while Alton plays in Manchester Friday against Post 79.
In its five games over the weekend in Burlington, Vt., Rochester beat Colchester, Vt., 6-4; Albany, N.Y., 4-1; Champlain Valley, Vt., 5-2; Newark, Del., 3-2, and Delaware, 6-0.
Kyle Davis, J.R. Santaniello and Chris Tebo were complete-game winners, while Will Fisher and Andrew Riotto combined in the win over Newark and Riotto and Mark Wiggins combined in the win over Colchester.
In the win over Colchester, Santaniello, Jeff Richardson and Cam Chasse had two hits.
Davis fanned eight over the final three innings against Albany, and whiffed the final six batters he faced. He struck out 11 in all, allowing three hits and one walk. LaBatte and Campbell had two hits and two RBIs each.
Santaniello allowed two hits, walked three and whiffed six against Champlain Valley. Warren had three hits, while Campbell, LaBatte and Wiggins had two hits each.
In the win over Newark, Riotto came into save the game for Fisher, retiring all six batters he faced in the final two innings. Santaniello, Wiggins and Robbie Jenkins each had an RBI.
In the final game against Newark, Del., Tebo tossed a three-hitter, walking one and striking out three. Campbell (run, RBI) and Davis (3 RBIs) each had two hits.
Rochester, 14-1 (7 inns.)
Alton (0-7) 000 010 0 — 1 6 4
Rochester (1-2) 114 206 x — 14 15 3
Batteries: A-A. Bourdeau, N. Funk (4), Knight (6) and M. Bourdeau and Gonya (6); R-LaBatte and Warren. WP-LaBatte; LP-A. Bourdeau. Home runs: R-2 (Ferullo, 2nd, none on; Fisher, 3rd, two on); LOB: A-9, R-6.


The third question is related to the twelfth chapter of Daniel where the prophet Daniel was given many end time prophecies which he did not understand. When he asked the Lord to explain them, he was told that they would not be understood until the time came for them to be fulfilled. Are we in that period of time today when we are understanding end time prophecies that no one has ever understood before? And if so, does that mean we are living in the season of the Lord's return?
#3. Are we finally understanding prophecies we've never understood before?
Yes, we are. One of the opening prophetic chapters of Daniel is chapter 2 where Daniel interprets the dream of King Nebuchadnezzar concerning the successive Gentile empires that would rule over Israel. In that interpretation given to Daniel, God told him only initially that the first empire would be the Babylonian Empire. God didn't really explain to him what the other empires would actually turn out to be.
Later on in chapter 8 in the vision of the ram and he-goat, God reveals to Daniel the next two empires, which were the Medo-Persian Empire and the Greek Empire. But, the fourth empire — the one that Daniel was most interested in and asked about, God does not specifically say it's the Roman Empire. Later in Daniel 9, it's revealed to Daniel that the people of that fourth empire would destroy Jerusalem, and from history we know that it was the Romans who destroyed Jerusalem in 70 AD. Because of that destruction, we now know that the people of the Antichrist accordingly were from the Roman Empire, as the Antichrist will be.
I'm not sure if Daniel really understood who that fourth empire was, but God then begins to give him many other details about that coming Roman Empire, including that last stage or last phase of it represented by the feet of the statue in Nebuchadnezzar's dream which is not made of solid iron but iron that has been mixed with clay. This imagery indicates a kind of weakness that would be in that last stage of the Revived Roman Empire. Even then, I don't think that Daniel fully understood that last empire. From where we are in history, obviously we can look back at Rome. Having now gone beyond 70 AD, we can understand Daniel's prophecies much better and we can see today that the Roman Empire has revived in the form of the European Union. That's one example of the many prophecies that Daniel probably did not fully understand, and there are probably others.
Daniel is told in chapter 12 to close up the book and seal it because it was meant for the times in many days to come. Those prophecies were not all for his time. I think that Daniel could accept that and realized that he was merely the recorder, the messenger. He was not the one who would need to be able to explain all of it to everybody in his day.
One of the examples that comes to mind is Daniel 7:23. There the passage talks about the final empire that would exist before the Second Advent of Jesus. It is the fourth beast and Daniel says it's going to subdue. The language is very specific about that. The final empire is going to subdue the whole world. That's talking about a one-world government.
I don't think Daniel in his time period could have ever seen something like a one-world government with his own eyes. He was prophesying during the days of Neo-Babylonia which was a localized government, and yet he's revealing some entity that would have jurisdiction over the entire world according to Daniel 7:23.
Just look at what's happening today. Look at the plans in store for a one-world government. Look how these politicians no matter what party they are in can't even get through a speech without mentioning globalism in some way. Clearly we are living in the time period where we have caught up to Daniel's prophecy of globalism.
Within the prophecies of Daniel, especially in the issue of the four empires and the final ruler of the fourth empire who is the Antichrist, there are lots of gaps in the information. You could not just take the book of Daniel and develop a full-scale chronological sequence of events. Daniel is told to seal the book, for it would not be fully understood in his time. Not that nothing could be understood, but a lot couldn't be understood.
When John finishes Revelation, he is told the opposite, to not seal the book because the missing pieces of information in Daniel were then provided in Revelation. When you combine the two books, you can get a good study of the sequence of events. And so, the reason that Daniel is told his prophecies wouldn't be fully understood is because there are gaps in the information, and those gaps we now have filled in Revelation.
Daniel 12:4 says that, "Many shall run to and fro and knowledge shall be increased." I believe we are seeing that knowledge being increased today in the 21st Century. I have no doubt in my mind that Daniel longed to want to understand these prophecies, but he could just not understand them in his day. But, in the Last Days, those who will seek to understand and read these prophecies will be able to do so.
I tried reading the Bible before I became a born again Christian and it was like trying to read Chinese. I couldn't understand one iota of that book. But, when I got saved, then the Holy Spirit of God came to reside within me. That's the last days ministry of the Holy Spirit as explained in John chapters 14-16 which tell us that the Holy Spirit will enlighten us to understand these very prophecies. Psalm 119:18 is fulfilled, "Open thou my eyes that I may behold wondrous things out of thy law." So, it's the Holy Spirit of God that illuminates us to understand these very prophecies.
God told Daniel, "Daniel, you are going to seal the book, and these prophecies are not going to happen in your lifetime." And yet, God tells John in Revelation 22:10, "Seal not the sayings or the prophecy of this book, for the time is at hand." That's talking about the imminency of the coming of the Lord Jesus Christ which could happen at any moment and at any time. Until the return happens, knowledge will be increased and so too our understanding of these last days prophecies.
In Daniel 2, it's recorded that Nebuchadnezzar lay in his bed one night and he had a dream. Nebuchadnezzar was the King of Babylon and so a very powerful man of a very powerful empire. He saw a statue that was composed of four different kinds of metals. He didn't understand what this statue meant, so Daniel was called in eventually and he interpreted this dream for Nebuchadnezzar.
Nebuchadnezzar was wondering what was going to happen in the last days and later years. After he was gone, what would life be like? Who's going to be running things? Daniel's interpretation of that dream is the answer to Nebuchadnezzar's question about what is going to happen in later days. Specifically, Daniel talked about the four empires: the Babylonian Empire which Nebuchadnezzar was a part of, then the Medo-Persian, then the Greek, and then the Roman Empire.
Very, very interesting is the part of the interpretation that just grabs my attention which is that dream ends with a stone that is cut out of this mountain without human hands. That stone becomes the dominant, the premiere kingdom, over all the earth. It crushes even any memory of the original four. That could not be understood until the days in which we are living right now, and that's the Kingdom of Jesus Christ.
In the eighth part of this series on the book of Daniel, the remaining members of our panel of Bible prophecy experts will continue to answer, "Are we finally understanding prophecies we've never understood before?"


Our Rockinfreak-a-meets 1999- 2004, pictures, running commentaries and stories: It's all here again! As I find the time, I will put up all photos of old fan and fanclub meetings on this site, you're welcome to contribute to complete our album - (4x Paris, 1 HQ meet are already up now - Enjoy! Follow this link to the Rockinrfeak-a-family album.
We are MTV UK's 'Fansite Insight'!
"Sibél's fansite is so userfriendly, even a monkey could log on! Here at mtv.co.uk we think the design is cool and simple. Check out the extensive discography and extremely detailed equipment section. This is a must for any Chili fan!"
20.02.04- Listen to John's Demo & Acoustic versions for free online!
11.12.03 - Slane Live Photos & Slane Streaming video samples!
3 full length Slane Live video samples!
09.12.03 - New European Tour Dates for 2004!
Greatest Hits CD/DVD AND Live at Slane DVD!
28.04.03- Win RHCP Tickets with the Your Player !
Win tickets ,watch behind the scenes Can't Stop footage,listen to the album and get dates!
Stills form the official By The Way Promotion Photo session - Enjoy!
17.12.02- THE ChiliChat is back!
By The Way.. All about the album and its singles!
12.4.02-Flea Chat on Ninemsn for National Youth Week 2002!
Flea chats with fans about the new album, life, music- and we have the full transcript!
Previously unpublished live and backstage photos by one of the best pros!
21.7.02- Hear tracks from the album+ band commentary!
21.01.03- Tribute To The Ramones finally released!
Troublekids in.. Update - Log = Find out what's new since your last visit!
06.11.02-New interview with Flea - donated by Ladybug. In between plenty of updates (see news) and put most of the John in Paris show online for download here!
15.08.02- A brandnew interview with John on his 4th album!
09.08.02- A new photo of John in Paris and the review to suit! Also new Tatoo pictures.
08.08.02- An excellent in depth interview with Anthony Flea and John + a Total Guitar interview with John.. enjoy!
24.07.02- Watch the Paris show online + video interviews with the whole band, and win RHCP gear - it's all up in the main news section! Also added a brand new concert review of the Talanta show by Brian Huff (Thank You Brian!! ) In Reviews section and good news about John in the John Tour Diary pages don't miss it! Actually there were dozens of updates between the last one logged here from May and now, but too much to write a new log for all of them.
17.05.02 - Books have been added to the Media pages - some interesting treats like Anthony's diary from his Borneo expedition(extracts will be added soon) - New Cali Promo pics are coming up tonight and a tattoo section is in under construction.
13.-16.05.02- It's been a long time but now Troublekids is back full blast: A big bunch of updates from new album to Tour and special competitons - And the main picture page is finally getting its much needed overhaul (picture files at 80kb or more each? *Shudders)At over 700 pics creating thumbnails by hand and redesigning the pages can take a while as you may understand .. To sweeten waiting time I've added 6 new pics to the Cali and "Private" pics sections and more are to follow soon, so it's well worth checking out the new pages!
24.02.02- A long overdue update for the news! Sorry but work doesn't leave me the time.
13.11.01- "Listen & Watch" - Troublekids' new multimedia page featuring delicious rare eye and ear candy treats.
1./7.11.01- Peppers will finally release their much rumoured Live DVD and Troublekids is proud to be the first site on the web to give you the full details! + More details on release date for the new album in our Updated tour & album section.
3.10.01- The best Christmas present ever: Red Hot Chili Peppers + John Frusciante live gigs in L.A. and Flea's new music Conservatory where the master himself will teach!
24.8.01 - A vivid first hand account of the Red Hot Chili Peppers live at V2001 Festival.
18.8.01 - 5 New Promotion Pictures of John -smiling, sulking, in bed.. + The Pictures sections are all gradually getting refurbished-Since loading the pix pages takes forever and a day, I'm turning all pics on this site into thumbnails by hand (not photoshop auto)and reducing filesize wherever possible -at several hundred pics, said refurbishing takes forever and ten days, argh!
17.8.01- Unfortunately things were happening in Pepperland sooner than expected: The Israel show has been axed last minute- A full report, all the media headlines and press links can be found in the Special report. Updated with news continuously.
13.8.01- Nothing happening in Pepperland? Getting the shakes from lack of Pepperfix? Troublekids has the remedy: The Robb Cohen Gallery -featuring mouth watering pics from legendary live gigs, both on and backstage, dressed in clothes or tattoos only - And updated weekly just when the craves set in again.. Very special thanks to Robb Cohen, longstading professional concert photographer and photojournalist, who kindly donated these exclusive pics to us!
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Pea Island Life-Saving Station was located on the Outer Banks in North Carolina. It was the first life-saving station in the country to have an all-#black crew, and it was the first in the nation to have a black man, Richard Etheridge, as the commanding officer. Richard Etheridge was born into #slavery on January 16, 1842, and was the property of John B. Etheridge on the Outer Banks of North Carolina. On the Outer Banks slavery was limited and there were no plantations. Most slave men who lived on the banks learned to work the sea, fish, and pilot boats, Etheridge was one of those slaves. Even though it was illegal to teach slaves to read, master Etheridge taught Richard how to read.
After the fighting between the states began in 1842, the Outer Banks became the site for Northern invasions. General Ambrose Burnside, the Union commander, needed Black labor men to build fortifications for his armies. The island was also a safe refugee camp for fugitive slaves. The union was not blind to the fact that they needed Southern black forces to add to their forces, not only by bolstering the Union ranks but by simultaneously diminishing the opposition's labor supply.
Black troops were enlisted by the summer of 1863; Richard Etheridge joined on August 28 of that year. Etheridge spent much of his first year of active duty like most of the other black units in the Union Army but playing secondary roles. After limited anti-guerilla actions in North Carolina, the soldiers of the 36th served as guards at the prisoner-of-war camp at Point Lookout, Maryland, occasionally raiding into neighboring Virginia for goods: such as horses, tools, supplies, cattle and slaves.
Etheridge left the service and returned home on the Outer Banks. He married and became a fisherman while serving in the newly formed Life-Saving Service. Since Etheridge was the first Black to be commander, under the racial standards of the times, the crew who worked under his command had to be black. Although other black men served as surfmen at Pea Island and other stations, the station was operated by an entirely black keeper and crew. Etheridge and his all-black crew had to deal with discrimination, and their station was burned to the ground right from the beginning. But, the crew did not let that stop them. He went on to serve twenty years. Etheridge died in 1900. Pea Island continued to be manned by an all-black crew through the Second World War. The station was decommissioned in 1947.
Very interesting I had read about these men before. There's always room to learn more, I didn't realize those men, were to become the buffalo soldiers of the Texas Calvary. Thanks for this site.


New Delhi : In a shocking revelation it has come to fore Police inspector Subodh Kumar Singh, who was killed during violence over alleged cow slaughter in Bulandshahr on December 3, had his thumb chopped off and sustained head injuries in an axe attack before being shot dead, police said.
These startling facts came to light during interrogation of prime accused Prashant Nat, who was arrested on Thursday, and recreation of the crime scene on Thursday evening.
Senior superintendent of police, Bulandshahr, Prabhakar Chaudhary said the villagers had felled a roadside tree to block the Bulandshahr-Garhmukteshwar road during their protest against alleged cow slaughter in Mahaw village in Syana area of Bulandshahr.
Not absconding Bajrang Dal member Yogesh Raj but a 30-yearold petty criminal named Prashant Natt, whose name did not figure in the first information report, has emerged as the prime suspect in the killing of inspector Subodh Kumar Singh in Bulandshahr earlier this month, according to a senior Uttar Pradesh Police officer.
"Inspector Subodh Singh reached the spot with police force and tried to pacify the mob. A villager, identified as Kalwa of village Chingrawathi, attacked the inspector with an axe in a fit of rage and chopped off his thumb. The injured inspector snatched the rifle of a policeman and tried to disperse the violent mob but he was again attacked with the axe sustaining an injury on his skull," he said.
The SSP said villagers also started pelting the policemen with stones. "The injured inspector ran towards an open field to save himself but the mob chased him and shot him dead. Other policemen also fled the spot to protect themselves," he added.
Kalwa is still on the run.Nat, a taxi driver, was on Thursday arrested from Noida for allegedly killing the police inspector.Police said Nat had confessed to shooting the inspector with the policeman's own weapon in a fit of rage.
Bulandhshahr's additional police superintendent, crime, Shiv Ram Yadav said Nat told interrogators that he caught hold of Singh when the mob cornered him in an open field after local youth Sumit was shot. He said Nat then allegedly shot Singh dead after snatching the inspector's pistol.
Nat's arrest came over a week after Singh's family blamed political pressure for the police's failure to arrest the main accused in the case.
Earlier, six of the 27 accused named in the case were arrested. As many as 19 others have been held after they were caught on video footage of the violence.
Three key accused, Bajrang Dal's Yogesh Raj, Bharatiya Janata Party leader Shikhar Agarwal, and Vishwa Hindu Parishad activist Upendra Raghav, remain on the run.
Hate extremists blinded by rage destroying the people who are protecting the nation!
What to say about a people to whom a cow matters more than a human being!!


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Working with Benode Bihari Mukherjee
Organising an exhibition in Delhi
KG Subramanyan	Artist
21. Organising an exhibition in Delhi 47 09:28
22. Working with Benode Bihari Mukherjee 54 03:25
23. Interest in Italian painting 42 04:03
24. Satyajit Ray 83 02:36
25. Leaving Santiniketan for Baroda 39 01:51
26. The partition of Indian and going to Baroda University 36 04:11
27. Life at Baroda 55 04:06
28. From Baroda to writing and the Slade School of Art, London 46 02:52
29. My wife, Susheela 71 07:13
30. London, language, tradition and the various influences on my art 69 05:22
A few months after joining Kala Bhavan, one of my friends who had the enthusiasm to exhibit works of these people in UP in one of the exhibitions, thought that he should get them to agree to exhibit in Delhi. They hadn't had an exhibit in Delhi. So he said that he, and he had an uncle almost his own sort of age, and he planned the whole thing and persuaded them that they would lend their works. Then he talked to me, since you can talk in English a little better than I, why don't you come with me? So I went with him to Delhi with his exhibition, and in planning the whole exhibition, getting together all the works, I came a little closer to them, and I saw their works much more than most other people saw. Of course our experience in Delhi was also very educative. In 1945 there wasn't much of an art activity in Delhi. In Delhi at that time the Old Delhi and New Delhi, you have to reach by horse carts, tongas, this sort of thing, and it seemed quite far. And then the culture of New Delhi and Old Delhi were also different, very official, very... and then the main art exhibition in those days was the art exhibitions that the different societies had, which was mostly academic work. The other people who had Sudhir Khastagir at that time was Sharada Ukil, who had an Ukil School of Art, and Amrita Shergil. In fact, Amrita Shergil charmed Sarada Ukil's brother, Baruda Ukil, to go along with her, and they used to have a few exhibitions together. So in her letters, she laughs at the kind of things he had to do to do that. Anyway, she was known and the other artist known at that time was a product of Kala Bhavan but who used to be in the Doon School as an art teacher. That is, Sudhir Khastgir. These are the people who were familiar at that time. So, when Benode Bihari and Ramkinar's work went there, Benode Bihari had said that time you see, I don't know many people anywhere but I know Nirad Chaudhuri, and you can go and meet him. So we went and met Nirad Chaudhuri. He was then the script writer in the All India Radio, especially news and other items and things of that kind. We went and met him, we said, 'Look, we are going to have this exhibition, Benode Bihari apparently knows you, will you be helpful to us?' He was very forthcoming. He said, 'I will write a small note for your leaflet'. Then he even took us to dinner, to his house, in Kashmiri Gate, then showed us his library of art books and things of that kind. Well, he had not become the man he became later as a sort of all-knowing sort, but he was very nice.
Is that before he wrote The Autobiography of an Unknown Indian?
That's right, that's much before, yeah. So then he said this kind of work, you can't just show like that here. No exhibition sort of attracts people unless it is opened by somebody. So we were wondering who would do that. Then he himself suggested Zakir Hussain, who at that time was the vice chancellor of the Jamia Millia Islamia. He is sort of a man with a lot of knowledge about the world, and also interested in art, so why don't you go and ask him? So we tried to contact Zakir Hussain, and Zakir Hussain said, 'I ought to see the paintings, I will be very happy, I have heard about artists but I haven't seen any of their work'. So we had to go in a tanga all the way, so many kilometres to his place to show him, and in the meanwhile, we had to find a place where to show them. The only two sort of not gallery spaces there were was one owned by the All India Fine Arts and Craft Society, and then there was a smaller placed called Freemasons Hall at that time. But in the All India Fine Arts and Craft Society, they didn't approve of the work. They said that we can't show that work. So we were quite...
So there was no Lalit Kala?
No, no Lalit Kala, nothing. This was in '45. Lalit Kala came into being about 7 or 8 years later. So, while walking along, we saw the YMCA which had a big hall, and I went in and then it was the administrator of the whole thing was a man from Kerala. So I talked to him and said that this is the thing, is there any space where we can...? So he said we have a kind of hall, but nobody exhibits works here, but I can give you on a certain date, yes, you can fix the date, but then you cannot put any nails on the wall, and it had too many windows. So I said look, we will have to put some kind of batons and nails at the end and have jute canvas so that it looks like a proper exhibition. He agreed to that. So the dates were fixed. So we went and told Zakir Hussain can he come and open. He saw that paintings and he was quite favourably impressed and he said, 'I would very much like to do it, but I am not there on that day, I am going to Germany'. So then I said, 'If you are going away, does he have any suggestions of who?' He said I don't know who is interested in art these days and things of that kind, and especially if you can, then he suddenly said, 'There is a person called, I think Edward Benthall, I think Edward Benthall', who then was the member secretary of the Railway Board . He said, 'He may not know anything about art, but he is a perfect gentleman, and he is well thought of by everyone in Delhi, so why don't you call him'. So we went to Edward Benthall. He was very nice. He was a tall Englishman, very proper, and he said, 'I will agree, I know nothing about art, but all the same, I am sure that when you have come all the way to show these works, these works should be of some importance'. Then there was the opening and because Edward Benthall opened them, well, a lot of people came to see it, and especially the people from the then Delhi Art School, which was not an art school at that time. It was a Delhi polytechnic where it had an art department. And then The Statesman sent its critic over, that was Charles Fabri was the critic, and it had a kind of a good reception. Now, this is how I came close to them, through these things. Of course those days, I mean we just made money we spent on it by selling two paintings each and that was bought of the art department of the yay [sic], otherwise, there was nothing else.
The art department of the yay [sic]?
The art department of the yay [sic], you said.
The art department of the Delhi Polytechnic. In fact, what is now called Delhi College of Art, was at that time the art department of Delhi Polytechnic.
KG Subramanyan (1924-2016) was an Indian artist. A graduate of the renowned art college of Kala Bhavana in Santiniketan, Subramanyan was both a theoretician and an art historian whose writings formed the basis for the study of contemporary Indian art. His own work, which broke down the barrier between artist and artisan, was executed in a wide range of media and drew upon myth and tradition for its inspiration.
Title: Organising an exhibition in Delhi
Listeners: Timothy Hyman
Timothy Hyman is a graduate of Slade School of Fine Art, London, in which he has also taught. In 1980 and 1982, he was Visiting Professor in Baroda, India. Timothy Hyman has curated many significant art exhibitions and has published articles and monographs on both European and Indian artists.
Date story recorded: 2008


text:
The Global LEI Initiative: Unfinished Business and the Hail Mary Pass
Posted on Thu, Mar 25, 2021 @ 7:00
By Allan D. Grody, Financial InterGroup
Originally published on the Financial InterGroup site
Below is a research note from Allan D. Grody of Financial InterGroup that explores the efforts of legal entity identifiers (LEIs) on a global basis.
LEI Statistics and Comparisons
The Global Legal Entity Identification Foundation (GLEIF) has been reporting statistics on registration of the Legal Entity Identifier (LEI) since January, 2016 and on the collection of LEI's Relationship data since May, 2017. We are pleased to bring you this Research Note on annual, month-end and year-to-date LEI issuance based on GLEIF's March 5, 2021 Global LEI Data Quality Report and FIG's historical LEI database, now accumulating data into its sixth year.
Registered LEIs this month reached 1.817 million vs last month's 1.797 million. Newly issued LEIs this month was 19,491 vs. last month's 19,485, about equal to the monthly average of last year of 19,364. This month's non-renewal (lapsed) LEIs were 15,688, much lower than last month's 22,270 and somewhat lower than last year's monthly average of 18,778. An overall lapsed rate comparing total non-renewed LEIs to total issued LEIs is 32.5% this month vs. last month's 32.8%. For the first time in five months the number of newly issued LEIs has exceed non-renewed LEIs.
Relationship data is following past patterns: the recording of permitted exceptions to opt-out of identifying a LEI for either or both parents is consistently growing at approximately twice the number of monthly newly issued LEIs; and the recording of LEIs with 'complete' parent data is consistently growing at about the monthly new LEI issuance rate. The 'complete' statistic includes no LEI recorded for one or both parents plus those LEIs recorded for its parents.
Active LEIs, Renewed LEIs and the Lapsed Rate
GLEIF this year began reporting total Active LEs in their statistics dashboard. As of February, 2021 month, end it totaled 1,744,868. This statistic results from subtracting from total issued LEIs: retired LEIs 52,028; merged LEIs 14,452; duplicate LEIs 4,729; annulled LEIs 833; LEIs pending archives 833; and LEIs pending transfers 256. If we calculate the non-renewal rate on active LEIs, it results in a rate of 33.8% vs. 32.5% calculating it based on total issued LEIs.
With one-third of the LEIs not renewed, little impetus is present for renewing such LEIs. There are two views, it is vital and the opposite, it is inconsequential. Even the CFTC which was the first regulator to champion the LEI has made renewing LEIs mandatory for only the largest firms under their jurisdiction, 153 swaps counterparties. The answer is that both views are correct, however, it is a matter of timing.
Right now, GLEIF is attempting to maximize adoption of the LEI. Championing a broad mandate for regulators to adopt mandatory renewal would most likely impede this objective. However, at some point issues will arise, hopefully nothing of consequence, in using non-renewed data. However, users of the LEIs and those who administer to the Global LEI initiative should be aware of and make sure renewals of LEIs becomes mandatory and plan for it before it becomes consequential.
First, non-renewed LEIs are allowed to be used in reporting to trade repositories in the EU. This presents potential default issues should a financial firm collapse or file for bankruptcy and its legal identity or its parent identity had been changed but without updating this information in the LEI record. A second scenario is that of renewing a LEI with corporate reorganization data such as mergers or acquisitions or spinoffs (legal actions). If LEI data is to be relied upon and such information is not accurate, not timely, nor does not match up with existing LEI data that may not have been renewed, exposure to losses can result (trading in the wrong company; mistiming dividend cash flows; missed voting of rights or warrants; etc.).
A Closer Look at the Validation Agent Concept
Most recently a Validation Agent (VA), a new category of intermediaries in the global LEI initiative, was introduced to the GLEIF's Globally Important Financial Institutions (GIFI) Relationship Group. These large financial institutions are being solicited for their willingness to validate on-boarding credentials of their clients and introduce them to a LOU for obtaining an LEI. The first to step up as a VA is JPMorgan Chase & Co.
The Validation Agent is not a new concept, it was first used by Avox, a private company that maintained a legal entity data base, to build its population of legal entities. Avox had most of the larger financial institutions submitting their onboarding data to them. They would then compare this to external second source databases. Where other financial institutions had provided data on the same entity, and there where many, it was compared it to those other submissions.
DTCC bought Avox in 2012, around the time the ground rules for the LEI were being contemplated. DTCC subsequently sold Avox to Reuters. It can now be found at Refinitiv which was acquired by the London Stock Exchange from Reuters. The "AVID" was their "LEI" identifier. It is still a major identifier in use today.
There are 3.5 million issued AVIDs. There are two major ways in which the LEI data is updated – from existing legal entities and from newly formed legal entities. The former has dominated the buildup of the 1.8 million LEIs. This has predominately been from converting existing information in financial institutions internal data bases into inputs to LOUs. The later will come to be the focus of the Validation Agents – new data from acquired clients' account onboarding documentation. This information is reviewed by legal staff at the financial institution opening the account. This information is also reviewed by auditors at the submitting legal entity at audit time.
JPM chose to work with an existing LOU, DTCC, because if JPM themselves became an LOU their identity would be associated with the client, thus advertising to all that this entity is a JPM client. While this is true to some extent, not all clients are exclusive to only one financial institution. Many clients shop for best-in-class financial institutions using different parameters of service and cost per function or product.
There is considerable cost/time savings if a VA could complete the entire process themselves as a VA and a LOU. In fact, having the original documentation in hand would negate having to access secondary sources of this information which at the time of onboarding probably does not yet exist do to timing issues of updating these secondary sources, especially the business registries, if this is a new legal entity. Having auditors' assurance of documentation submitted would provide a financial institution with the necessary adherence to its know-your-customer obligations.
To me this suggests multiple VA's sponsor a LOU Utility so that anonymity of clients and cost/time savings can be realized.
The vLEI Hail Mary
The vLEI is a digitally verifiable credential containing the LEI. The vLEI service to be offered by GLEIF will enable automated identity verification between counterparties operating across all industry sectors, globally. It will be supported by a credentialing governance framework and technical support infrastructure. By embedding new and existing LEIs in verifiable credentials, the vLEI will create a cryptographically secure chain of trust. It is intended to replaces today's manual processes required to access and confirm an entity's LEI data.
While the vLEI effort is laudable as another use case for adoption of the LEI, its extension to all industry sectors globally may deflect from the LEIs primary mission of its use for cost reduction and risk management in the financial services sector.
GLEIF is now looking to engage with the pharmaceutical, healthcare, telecom, and automotive sectors through the vLEI. The need to increase the adoption rate of LEIs is, of course, paramount but moving far afield of its mandated and exclusive focus on the financial services sector might be a stretch. This is especially the case as so much has yet to be done in the single sector of finance: increasing LEI registrations for parent hierarchical relationship data; implementing legal actions for timely maintenance of the GLEIS; onboarding government entities participating in financial transactions; implementing the Validation Agent concept; onboarding fund families; resolving the accumulating Provisional Node Identifier (PNI) codes recorded in the GLEIS for registered legal entities not registering a LEI for a known parent; and implementing a mapping service for data vendors.
By itself this is an ambitious agenda. At the same time a commitment to drive the cost of a LEI to zero is compelling the GLEIF and its direct government overseer, the Regulatory Oversight Committee (ROC), to look beyond the financial sector to other uses of the LEI, particularly with the vLEI. Both have set a 2027 goal of 20 million LEIs issued, from its current 1.8 million. That is a tenfold increase in seven years, when it took nearly a decade to reach the current total. Notwithstanding that awareness and momentum of the Global LEI initiative has built up over the past decade, this goal might be a bridge too far.
This column does not necessarily reflect the views or opinions of FinReg Alert or Tradeweb Markets LLC.
Allan D. GrodyFinancial InterGroupGLEIFJPMorganLEIs


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4/09/2014�� The CVV number is a fraud prevention tool, providing a layer of security when the card is not present during a transaction. These numbers will be phased out as �... Card features � your credit card is printed with a security code (CVV) and is protected with a PIN � both help us to verify the card is in your possession when you make transactions. No liability ? You will not be liable for fraudulent transactions online or on the high street (including contactless transactions).
Card security Protect your card and PIN from fraud HSBC UK . Security centre The fraudsters telephone customers on their landline claiming that their debit or credit card has been used fraudulently. In order to gain customers trust the fraudsters tell them to ring their bank on the telephone number printed on the reverse of their card to ensure the call is genuine. The fraudster pretends... Your best option would be to call your credit card company and get them to help you. That code is the �card verification code,� and without it, online retailers cannot confirm that you are the cardholder.
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26/08/2015�� There's a hidden mathematical pattern in your credit card (also works for debit cards or ATM cards). In this video I will teach you a mathematical magic trick based on the pattern.
Your best option would be to call your credit card company and get them to help you. That code is the �card verification code,� and without it, online retailers cannot confirm that you are the cardholder.
Card features � your credit card is printed with a security code (CVV) and is protected with a PIN � both help us to verify the card is in your possession when you make transactions. No liability ? You will not be liable for fraudulent transactions online or on the high street (including contactless transactions).


text:
\section{Introduction}

The nonthermal X-ray emission detected from a number of young
shell-type SNRs (for a review see e.g. Vink \cite{Vink2006}) is
generally interpreted as synchrotron radiation of relativistic
electrons accelerated diffusively by shock waves to multi-TeV
energies (see e.g. Drury et al. \cite{Druryetal2001}). Two
other (alternative) radiation mechanisms - the bremsstrahlung of
subrelativistic electrons and the inverse Compton (IC) scattering
of  moderately relativistic electrons  - are not sufficiently effective to explain
the observed X-ray fluxes.  The  discovery of TeV gamma-rays from
young SNRs, in particular from Cas A  (Aharonian et al.
\cite{Aharonian2001}), RX J1713.7-3946 (Enomoto et al.
\cite{Enomoto2002}; Aharonian et al. \cite{Aharonian2004}) and  RX
J0852.0-4622  (Katagiri et al \cite{Katagiri2005}; Aharonian et
al. \cite{Aharonian2005}) provides unambiguous evidence of
acceleration of particles (electrons and/or protons) to energies
100 TeV and beyond. Unfortunately even the very high quality
morphological and spectrometric studies of young SNRS in TeV
gamma-rays performed with the HESS array of  imaging atmospheric
Cherenkov telescopes do not allow robust conclusions concerning
the origin of gamma-rays.  For example,   in the case of the best
studied gamma-ray emitting SNR, RX  J1713.7-3946, the hadronic
model  can explain satisfactorily  both the overall energetics
and the spectral features of TeV gamma-ray emission.
Nevertheless,  the inverse Compton origin of gamma-rays
remains an alternative option, provided that the
magnetic field in the gamma-ray production region  does not
exceed $10 \mu \rm G$ (Aharonian  et al. \cite{Aharonian2006}).

Power-law distributions of relativistic particles are readily
formed at astrophysical shocks, in particular in young shell type
SNRs, through  the so-called diffusive shock acceleration (DSA)
mechanism (Krymsky \cite{krymsky77}, Bell \cite{bell78}, Axford et
al. \cite{axford77}). The maximum energy of accelerated particles
and the shape of the spectrum around and beyond the maximum energy
(the so-called "cutoff region") is  determined by the competition
between the acceleration  and escape rates, as well as, in the
case of electrons, by radiative (synchrotron and inverse Compton)
energy losses. In this regard, the most important information
about the accelerator is contained in the energy distribution of
particles in the cutoff region.  The spectrum of relativistic
electrons in the cutoff region is formed under conditions when
particles gain energy during the shock crossing and lose energy
simultaneously. In young SNRs,  the radiative cooling of electrons
results in formation of highest energy tails of synchrotron X-rays
and inverse Compton  gamma-rays, at $\geq 1$ keV and $\geq 10$
TeV, respectively. Thus, the comparison of  hard X-ray and TeV
gamma-ray observations with the spectral features predicted by the
DSA model in these energy bands gives direct information about the
key parameters characterizing the process of particle
acceleration. In this regard,  analytical presentations of the
energy  distributions  of high energy electrons and the spectra of
their synchrotron and IC radiation components provide effective
tools for   studies of nonthermal processes in SNRs.

So far,  analytical solutions for the electron spectra at the
plane  shock have been derived  only for a special case of
\textit{energy-independent} diffusion coefficient (Bulanov \&
Dogiel \cite{bulanov79}, Webb et al. \cite{webb84}, Heavens \&
Meisenheimer \cite{heavens87}).  At the same time, for
typical shock speeds of several thousand km/s
in young SNRs, the particles, in particular electrons, have a chance to be
boosted  to multi-TeV energies only if the acceleration proceeds
in the most effective  way, the so-called Bohm diffusion limit.
This implies strong\textit{
energy-dependence} of the diffusion coefficient, $D(E) \propto E$.
Therefore,  it is important to derive analytical solutions for the
electron spectra  for a more realistic case of diffusion.

In this paper we present exact asymptotic solutions  for the
high-energy tails of  distributions of electrons formed at the
plane shock,  assuming arbitrary energy-dependencies of both the
diffusion coefficient and the energy lose rate of electrons.  The
spectrum of electrons in the low-energy domain where the radiative
cooling can be neglected,  is well known from the solution of the
transport equation characterizing the acceleration at the shock
without losses.  On the other hand, assuming that the cooling of
electrons at very high energies is dominated by synchrotron
losses, we obtained simple analytical expressions for the exact
asymptotic solutions in the high energy domain. In order to extend
the  analytic presentations to a broader  energy range, we  should
"glue"  the asymptotic solutions  applicable at very low and very
high energies, using numerical calculations performed at
intermediate energies. We treat separately the electron
distributions at the shock, as well as downstream and upstream of
the shock, and calculate the spectra of  synchrotron and IC
radiation in these regions. We present these spectra in forms of
simple analytical approximations which appear significantly
different from ones often used in the literature for the fits of
spectral measurements  and subsequent interpretations  of the
X-ray and TeV gamma-ray observations of SNRs in terms of
synchrotron and IC radiation of multi-TeV electrons.

\begin{figure}[t]
\includegraphics[width=8.0cm]{fig1.eps}
\caption{The shock speeds  in the
upstream and downstream regions (solid lines) and  the spatial distributions of
electrons (dashed lines), accelerated at the plane shock.  }
\end{figure}

\section{Asymptotic form of the electron spectra}

Below we consider  acceleration of electrons by the plane shock.
The upstream plasma moves with a speed  $u=u_1$ towards the shock
from $-\infty $ of the $x$ axis (see Fig.1). Then, the downstream
speed is $u_2=u_1/\sigma$,  where $\sigma $ is the shock
compression ratio. The electron momentum distribution $N(p,x)$
obey the following equation written in the shock frame upstream
and downstream of the shock:
\begin{equation}
\frac \partial {\partial x}D\frac {\partial N}{\partial x}-
u\frac {\partial N}{\partial x}+\frac 1{p^2}\frac {\partial }{\partial p}
p^2b(p)N=0
\end{equation}
Here $b(p)$  is the energy lose rate of particles ($b  > 0$).  Hereafter we
assume that the synchrotron losses dominate  over the escape of
electrons from the system.  The electron momentum distribution
$N(p)$ is normalized to  $n=4\pi \int p^2dpN(p)$, where $n$ is the
number density of accelerated particles.

Boundary condition at the shock front, $x=0$,  can be written as
\begin{equation}
u_1\frac p{\gamma _s}\frac {\partial N_0}{\partial p}= \left.
D_2\frac {\partial N}{\partial x}\right| _{x=+0}- \left. D_1\frac
{\partial N}{\partial x}\right| _{x=-0} \ ,
\end{equation}
where $\gamma _s=3\sigma /(\sigma -1)$ is the power-law index of
particles accelerated at the absence of  energy losses, $N_0(p)$
is the electron distribution at the shock front, $D_1$ and $D_2$
are the diffusion coefficients upstream and downstream of the
shock, respectively.

Analytical solutions of  Eqs.(1) and (2)  can be obtained  for
simplified conditions, e.g. at  low energies when  the radiative
energy losses can be neglected, or in the case of
energy-independent diffusion-coefficient.  On the other hand, it
is possible to derive asymptotic solutions for an arbitrary
diffusion coefficient in the very high energy regime,  where  the
energy losses of particles dominate over their acceleration.
In this regime, it is
convenient to present the solution for the steady-state energy
distribution of electrons  in the following form:
\begin{equation}
N_{1,2}= K_{1,2}(x,p)\exp[S_{1,2}(x,p)] \ ,
\end{equation}
where indices  $1,2$ correspond to the upstream and downstream
regions, respectively. In the asymptotic regime, when losses
dominate over the acceleration, the function $S(x,p)$ obtains large
negative values. According to the standard asymptotic method we assume
that $S(x,p)$ is proportional to $b(x,p)$. After substitution of
Eq. (3) into Eq. (1) and keeping all  terms which are proportional
to $b^2$ and $b$, one finds

\begin{equation}
D_{1,2}\left( \frac {\partial S_{1,2}}{\partial x}\right) ^2
+b_{1,2}\frac {\partial S_{1,2}}{\partial p}=0
\end{equation}
\[
D_{1,2}K_{1,2}\frac {\partial ^2S_{1,2}}{\partial x^2}+
2D_{1,2}\frac {\partial K_{1,2}}{\partial x} \frac {\partial
S_{1,2}}{\partial x}
\]
\begin{equation}
-u_{1,2}K_{1,2}
\frac {\partial S_{1,2}}{\partial x}+
\frac 1{p^2}\frac {\partial }{\partial p}p^2b_{1,2}K_{1,2}=0 \ .
\end{equation}
Denoting by
\begin{equation}
S_0(p)=\left. S_1(p)\right| _{x=0}=\left. S_2(p)\right| _{x=0} \ ,
\end{equation}
\begin{equation}
K_0(p)=\left. K_1(p)\right| _{x=0}=\left. K_2(p)\right| _{x=0} \ ,
\end{equation}
and  performing the same expansion for the boundary condition
given by  Eq.(2),  we obtain
\begin{equation}
\frac {u_1p}{\gamma _s}\frac {\partial S_0}{\partial p}= {D_2}
\left. \frac {\partial S_2}{\partial x}\right| _{x=0}- {D_1}
\left. \frac {\partial S_1}{\partial x}\right| _{x=0} \ ,
\end{equation}
\begin{equation}
\frac {u_1p}{\gamma _s}\frac {\partial K_0}{\partial p}= {D_2}
\left. \frac {\partial K_2}{\partial x}\right| _{x=0}- {D_1}
\left. \frac {\partial K_1}{\partial x}\right| _{x=0} \ .
\end{equation}

The derivatives of functions $S_1$ and $S_2$ on $x$ and the
derivative $\partial S_0/\partial p$ can be found from Eqs.(4) and
(8):
\begin{equation}
\left. \frac {\partial S_1}{\partial x}\right| _{x=0}= \frac
{\gamma _s}{u_1p}\sqrt{\frac {b_1}{D_1}} \left(
\sqrt{b_1D_1}+\sqrt{b_2D_2}\right),
\end{equation}

\begin{equation}
\left. \frac {\partial S_2}{\partial x}\right| _{x=0}= -\frac
{\gamma _s}{u_1p}\sqrt{\frac {b_2}{D_2}} \left(
\sqrt{b_1D_1}+\sqrt{b_2D_2}\right) \ .
\end{equation}

\begin{equation}
\frac {\partial S_0}{\partial p}=-\frac {\gamma ^2_s}{u_1^2p^2}
\left( \sqrt{b_1D_1}+\sqrt{b_2D_2}\right) ^2
\end{equation}
The  solution of the last equation is
\begin{equation}
S_0=-\frac {\gamma ^2_s}{u^2}\int ^p_0\frac {dp'}{p'^2}
\left( \sqrt{b_1(p')D_1(p')}+\sqrt{b_2(p')D_2(p')}\right)^2.
\end{equation}
Taking the first derivative of Eq.(4) on $x$,  and using Eqs (10)
and (11) we find
\begin{equation}
\left. \frac {\partial ^2S_1}{\partial x^2}\right| _{x=0}= -\frac
{b_1}{2D_1}\frac {\partial }{\partial p}\ln{\sqrt{\frac
{b_1}{p^2D_1}} \left( \sqrt{b_1D_1}+\sqrt{b_2D_2}\right) },
\end{equation}

\begin{equation}
\left. \frac {\partial ^2S_2}{\partial x^2}\right| _{x=0}= -\frac
{b_2}{2D_2}\frac {\partial }{\partial p}\ln{\sqrt{\frac
{b_2}{p^2D_2}} \left( \sqrt{b_1D_1}+\sqrt{b_2D_2}\right) } \ .
\end{equation}

After  substitution of
these  functions  into Eq. (5), and using Eq. (9),  we  arrive at the
following ordinary differential equation
\begin{equation}
p\frac {\partial K_0}{\partial p}K^{-1}_0=-\frac 12+
 \frac {\sqrt{D_2}p\frac {\partial
}{\partial p}\sqrt{b_2} +\sqrt{D_1}p\frac {\partial }{\partial
p}\sqrt{b_1}} {\sqrt{b_1D_1}+\sqrt{b_2D_2}} ,
\end{equation}
the solution of which can be written in the following form:
\begin{equation}
K_0(p)\propto p^{-1/2}\exp{\int dp\frac {\sqrt{D_2}\frac {\partial
}{\partial p}\sqrt{b_2} +\sqrt{D_1}\frac {\partial }{\partial
p}\sqrt{b_1}} {\sqrt{b_1D_1}+\sqrt{b_2D_2}}} \ .
\end{equation}
Eqs. (3),(13) and (17) determine the asymptotic form of the
electron spectrum at the shock front $N_0(p)$ for an arbitrary
diffusion coefficient. In the case of an energy-independent
diffusion, it coincides  with the exact solution  derived by Webb
et al. (\cite{webb84}).

These expressions can be significantly simplified in the case of
the same energy-dependence of the diffusion coefficient and the
energy lose rate  upstream and downstream: $b_2=b=\xi b_1$,
$D_2=D=\kappa D_1$. In this case

\begin{equation}
K_0(p)\propto \sqrt{b/p}   \ ,
\end{equation}
and Eq. (3) is reduced to
\begin{equation}
N_0\propto \sqrt{\frac bp}\exp \left[ -\frac {\gamma ^2_s}{u_1^2}
\left( 1+\frac 1{\sqrt{\xi \kappa }}\right) ^2 \int ^p_0\frac
{dp'}{p'^2}b(p')D(p')\right] \ .
\end{equation}

The integrations of $F_1=\int ^0_{-\infty }dxN(x,p)$ and $F_2=\int
_0^{\infty }dxN(x,p)$   give   the integrated electron spectra
$F_1(p)$ and $F_2(p)$ in the upstream and downstream regions,
respectively. They are of great practical interest in many
astrophysical situations. At large momenta they are
determined by the ratios of the electron spectrum at the shock
front to the absolute values of derivatives given by Eqs.(10) and
(11):
\begin{equation}
F_1(p)=\frac {\xi }{1+\sqrt{\kappa \xi }}\frac {u_1p}{\gamma
_sb(p)}N_0(p) \ ,
\end{equation}
\begin{equation}
F_2(p)=\frac {\sqrt{\kappa \xi }}{1+\sqrt{\kappa \xi }}\frac
{u_1p}{\gamma _sb(p)}N_0(p) \ .
\end{equation}

Eqs. (19)-(21) describe the form of the spectrum at large
energies. At small energies the losses are negligible and the
electron  spectrum is power-law with an index $\gamma _s$. In order
to describe  the transition between this two extreme regimes,
Eq.(1)  has been solved numerically using  an implicit
finite-difference scheme.

\subsection{The case of Bohm diffusion}

Below we consider the most interesting  case which assumes that
the diffusion of electrons proceeds in the  so-called Bohm
diffusion regime and the energy losses of electrons are dominated
by synchrotron radiation. We present the diffusion coefficient  in
the form  $D=\eta cr_g/3$, where $r_g=pc/qB$ is the gyroradius of
particles, $B$ is the magnetic field strength, $q$ and $m$ are the
electric charge and mass of the electron, respectively. The factor
$\eta\geq 1 $  allows deviation of the diffusion coefficient from
its minimum value $\eta =1$ (the nominal Bohm diffusion). The
synchrotron loss rate  averaged over the pitch angles is
$b(p)=4q^4B^2p^2/9m^4c^6$. Since the Bohm diffusion and
synchrotron losses are determined by the magnetic field strength,
the parameter $\xi =\kappa ^{-2}$, where $\kappa $ is the ratio of
the magnetic field upstream to the magnetic field downstream,
$\kappa =B_1/B_2$. Eq. (19)  shows that in the high energy cut-off
region the spectrum has a "Gaussian" type behavior, $N_0 \propto
\exp (-p^2/p^2_0)$, where
\[
\frac {p_0}{mc}=(1+\kappa ^{1/2})^{-1}\frac {mcu_1}{\gamma
_s\sqrt{2\eta q^3B/27}}=
\]
\begin{equation}
\frac {2.86\cdot 10^8}{\gamma _s\eta ^{1/2}(1+\kappa
^{1/2})} \left( \frac {u_1}{3000\ \mathrm{km\ s}^{-1}} \right)
\left( \frac {B}{100\ \mu \mathrm{G} }\right) ^{-1/2} \ .
\end{equation}
Here the shock speed $u_1$ and the magnetic field in the
downstream region $B_2=B$ are normalized to ${3000\ \mathrm{km\
s}^{-1}}$, and $100 \ \mu \mathrm{G}$, which are quite typical for
shells of young SNRs.

At $p=p_0$, the characteristic  lifetime  of electrons  due to  the
synchrotron cooling  is
\[
\tau =p_0/b(p_0)=8.6  \gamma _s(1+\kappa ^{1/2})\eta ^{1/2}\times
\]
\begin{equation}
\left( \frac
{u_1}{3000\ \mathrm{km\ s}^{-1}} \right) ^{-1}\left( \frac {B}{100\ \mu
\mathrm{G} }\right) ^{-3/2} \ \mathrm{yr}\ .
\end{equation}
The synchrotron losses have a strong impact on formation of
the energy spectrum of electrons at energies for which this time
is small compared to the characteristic dynamical times of  the
source, e.g.  the age of the accelerator. If this condition is
fulfilled, the electrons with such energies are concentrated in
the shock vicinity,  and therefore the plane shock approximation is well
justified.

In the case of  standard shock acceleration in the Bohm diffusion
regime  with $\kappa =1$ and $\gamma _s=4$,  we combined  the
asymptotic analytical solutions, obtained at low and very high
energies,  with numerical calculations performed in the transition
region. This allows  a simple analytical presentation of the
electron spectrum at the shock  over the entire energy range:
\begin{equation}
N_0(p)\propto p^{-4}[1+0.66(p/p_0)^{5/2}]^{9/5}\exp
(-p^2/p^2_0) \ .
\end{equation}
The spectrum of electrons given by Eq.(24) is shown in Fig. 2. At
low and large energies  Eq. (24) coincides with the exact
asymptotic solutions:  $N_0(p) \propto p^{-4}$ and  $N_0(p)
\propto p^{1/2} \exp(-p^2/p^2_0)$, respectively. In the cutoff
region, the spectrum  is proportional to the product of two terms
--  a power-law term with a positive slop ($p^{1/2}$) and  an
exponential term, $\exp(-p^2/p^2_0)$. While  the first term can be
interpreted as a pile-up\footnote{The possible appearance of a
pile-ups in the electron spectra within the so-called "box" model
of shock acceleration has been noticed by Drury et al.
(\cite{Drury99}).},  it in fact does not sow-up because  the
second (exponential) term effectively cancels this feature. As a
result,  an almost perfect power-law ($p^{-4}$  type) spectrum is
formed up to $p \sim p_0$, with a super-exponential cutoff
afterwards (see Fig.2).

It is easy to relate, using Eq. (1)  and boundary condition given by Eq. (2)
the integrated spectra in
downstream, upstream and the spectrum at the shock:

\begin{equation}
F_2+\kappa ^2F_1=l\frac {p_0}{p}N_0(p), \ \mathrm{and} \ l=\frac
{u_1p^2}{\gamma _sbp_0}.
\end{equation}
 This relation is valid for all energies. It
implies  that for $\kappa =1$ (i.e. equal magnetic field strengths
upstream and downstream)  the integrated spectrum $F=F_1+F_2
\propto N_0p^{-1}$.

The case of different magnetic fields in the
downstream and upstream regions,
more specifically, for the scenario when  the magnetic field downstream
is stronger than magnetic field upstream by a factor of $\kappa
^{-1} =\sqrt{11}$, is of practical interest, in particular
for nonthermal emission of young supernova remnants.   This case,
which  corresponds to the increase of the  isotropic random
B-field at the shock with the "standard" compression factor
$\sigma =4$, can be described by the following analytical
approximations for the electron distributions at the shock front:
\begin{equation}
N_0(p)\propto (p/p_0)^{-4}[1+0.523(p/p_0)^{9/4}]^{2}\exp
(-p^2/p^2_0) \ ,
\end{equation}
and in the upstream region
\begin{equation}
F_1(p)\propto 0.70l(p/p_0)^{-3}[1+1.7(p/p_0)^{3}]^{5/6}\exp
(-p^2/p^2_0) \ .
\end{equation}
For the downstream,  the integrated energy spectrum of electrons can
be found from Eq. (25):

\begin{equation}
F_2(p)=N_0(p)l\frac {p_0}{p}-0.09F_1(p) \ .
\end{equation}

Note that the spectrum integrated over the upstream region, at
small energies  is very flat, $F_1 \propto p N_0(p) \propto p^{-3}
$. This has a simple explanation  related to the spatial scale of
the electron distribution; in the upstream region it is
proportional to the diffusion coefficient.

The integrated spectra of electrons in the upstream and downstream
regions given by Eqs. (26)-(28) as well as results obtained
numerically are shown in Fig.3.

The dependence of the spectra given by Eqs. (24), (26)-(28)
on the factor $\eta $ is expressed through the momentum $p_0$.

\section{Synchrotron  radiation}

The synchrotron emissivity of electrons
is determined  as
\begin{equation}
\epsilon (\omega )=\frac {\sqrt{3}Bq^3}{2\pi mc^2}
\int p^2dpN(p)R(\omega /\omega _c)
\end{equation}
where $\omega _c$ is the characteristic frequency of synchrotron
radiation $\omega _c=1.5\ qBp^2/m^3c^3$. The function $R$
describes synchrotron radiation of a single electron in magnetic
field with chaotic directions.  Crusius \& Schlickeiser
(\cite{crusius86}) derived an exact expression for  $R(\omega
/\omega _c)$ in terms of Whittaker's function. With an accuracy of
several percent $R(\omega /\omega _c)$ can be presented in a
simple analytical form
\begin{equation}
R(\omega /\omega _c)= \frac {1.81\exp (-\omega /\omega _c)}
{\sqrt{(\omega _c/\omega )^{2/3}+(3.62/\pi )^2}} \ .
\end{equation}

These functions are compared in Fig.4.

 The energy flux
($J(\omega)=\omega {\rm d}N_{\mathrm{rad}}/{\rm d}\omega$) of
synchrotron radiation produced at the shock is determined by the
integral of the emissivity along the line of sight $l$ and over
the solid angle  $\Omega $ $J(\omega )=\int dld\Omega
\epsilon $. This means that it is determined by the integrated
spectrum $F(p)$.

The integration of  Eq. (29), using Eqs. (24) and (30),
results in the energy flux of radiation $J(\omega )=\int
dpa(p,\omega )\exp (-g(p,\omega ))$, where $g(p,\omega )=\omega
/\omega _c+p^2/p^2_0$,  $a(p,\omega )\propto p^2F(p)R(\omega
/\omega _c)\exp (g(p,\omega ))$. At large frequencies, when the
argument of the exponent is large this integral is mostly
determined by the momentum interval around the momentum $p_*$
which minimizes the function $g(p,\omega )$. Thus at large
frequencies the energy flux of radiation can be written as
$J(\omega )=a(p_*,\omega )\exp (-g(p_*,\omega ))\sqrt{2\pi
/g''(p_*,\omega )}$. Here $g''$ is the second derivative of $g$ on
$p$. The momentum $p_*$ is given by the expression:
\[
\frac {p_*}{mc}=\left( 9\frac {\omega m^3c^3u_1^2}{\eta \gamma
_s^2q^4B^2}\right) ^{1/4}\frac {1}{\sqrt {1+\kappa ^{1/2}}}=8.3
\times 10^7 \times
\]
\begin{equation}
\frac { (\hbar \omega /1 \rm  \ keV)^{1/4}} {\gamma _s^{1/2}  \eta
^{1/4} \sqrt {1+\kappa ^{1/2}} } \left( \frac {u_1}{3000
\mathrm{km/s}} \right)^{1/2} \left(\frac {B}{100\ \mu \mathrm{G}
}\right)^{-1/2} \ .
\end{equation}
Note that  at the fixed $\omega$, the characteristic
frequency of the synchrotron radiation $\omega_c $ corresponding
to  $p_*$,  is smaller than $\omega$.

In the regime of Bohm diffusion the energy
flux of synchrotron radiation has an asymptotic form
\begin{equation}
J \propto \omega ^{3/8}\exp (-\sqrt{\omega /\omega _0}) \ ,
\end{equation}
where
\begin{equation}
\omega _0=\frac {81}{16\left( 1+\kappa ^{1/2}\right) ^2} \frac
{u_1^2mc}{\eta \gamma ^2_sq^2} \ ,
\end{equation}
or for the  corresponding energy of  synchrotron photons
\begin{equation}
\epsilon _0= \hbar \omega _0= \frac {\mathrm{2.2\ keV}}{\eta
(1+\kappa ^{1/2})^2}\left( \frac {u_1}{\mathrm{3000\ km\ }s^{-1}}
\right) ^2\frac {16}{\gamma _s^2} \ .
\end{equation}

At small energies the integrated downstream synchrotron spectrum
is proportional to $\omega ^{-{\frac {\gamma _s-2}{2}}}$. In order to
describe analytically the  synchrotron spectrum over
the entire energy range, which should  coincide  with the  exact
asymptotic spectra  at low and high energies,  we use
numerical calculations  performed in the intermediate energy range. In
particular, in the  case of $\gamma _s=4$ and $\kappa
=1$, we suggest  the following approximate formula
\begin{equation}
J(\omega )\propto \frac {\omega _0}{\omega }\left[ 1+ 0.46\left(
\frac {\omega }{\omega _0} \right) ^{0.6}\right] ^{11/4.8} \exp
(-\sqrt{\omega /\omega _0} \ ) \ ,
\end{equation}
which provides an accuracy  better than 10 percent.

The energy spectrum of electrons at the shock $N_0(p)$ (see Eqs.
(24)), is shown in Fig.2. Because the cooling length of electrons
downstream the shock is inversely proportional to the momentum,
the spatially integrated electron spectrum appears steeper, in
particular, in the case of $\kappa=1$, $F(p)=F_1(p)+F_2(p) \propto
N_0(p)/p$. Note that below the cutoff region $F(p) \propto
p^{-5}$. The corresponding spectrum of synchrotron radiation of
these electrons is shown in Fig.2. At small frequencies, $J(\omega
)\propto \omega ^{-1}$.

The synchrotron spectrum obtained using the so-called $\delta
$-function approximation is also shown in Fig.2. It is assumed,
that the synchrotron emission of the  electron is concentrated at
the frequency $\omega =0.29\omega _c$. This corresponds to the
function $R(\omega /\omega _c)\propto \delta (0.29-\omega /\omega
_c)$. Obviously this approximation does not provide a satisfactory fit.

\begin{figure}[t]
\includegraphics[width=8.5cm]{fig2.eps}
\caption{The electron distribution at the shock front (solid line)
and the spatially integrated spectrum of synchrotron radiation
(dashed line) produced by  electrons  accelerated at the shock
with compression ratio $\sigma =4$ and equal upstream and
downstream magnetic fields ($\kappa =1$). The spectrum of
synchrotron radiation obtained using the $\delta $-function
approximation is also shown (dotted line). }
\end{figure}

In the  case of $\gamma _s=4$, $\kappa =1/\sqrt{11}$ we
found the following spectra produced upstream and downstream the
shock:
\begin{equation}
J_1(\omega )\propto 0.175\left[ 1+ 1.27\left( \frac {\omega
}{\omega _0}\right)^{3/4}  \right]^{1/2} \exp \left
(-\sqrt{3.32\frac {\omega }{\omega _0}}  \right) ,
\end{equation}
\begin{equation}
J_2(\omega )\propto \frac {\omega _0}{\omega }\left[ 1+
0.38\sqrt{\frac {\omega }{\omega _0}}  \right]^{11/4} \exp
\left( -\sqrt{\frac {\omega }{\omega _0}}  \right) .
\end{equation}
Note that the spectrum of synchrotron radiation produced upstream the shock at small
frequencies is very flat, $J(\omega)=\mathrm{const}$, which
reflects the  hard electron spectrum  in that region (see Eq.(27) and Fig.3).

The  spectra of synchrotron radiation in the upstream and
downstream regions  given by Eqs.(36) and (37) are shown in Fig.5.
The synchrotron flux in the downstream region is significantly
enhanced because of the  larger (compressed)  magnetic field.
The corresponding spectra obtained numerically are also shown.

We should note that the exponential terms in Eqs. (35),(36) and
(37) are relatively slow functions (proportional to $\exp
[-(\omega/\omega_0)^{1/2}]$). Moreover,  these exponential terms
are multiplied to  power-law terms $(\omega/\omega_0)^s$ with
positive indices, $s \ge 0$,  which effectively compensate the
exponential terms at  frequencies $\omega \sim \omega_0$. For that
reason the parameter $\omega_0$  only formally can be  treated
as a cutoff  frequency.  In reality,  the breaks (cutoffs) in
the synchrotron spectra  appear at much higher frequencies,
namely at $\omega \geq 10 \omega_0$.

\begin{figure}[t]
\includegraphics[width=8.5cm]{fig3.eps}
\caption{The integrated upstream ($F_1$; dotted line) and
downstream ($F_2$; dashed line) electron spectra given by Eqs.
(27), (28), as well as the overall $F=F_1+F_2$ spectrum (solid
line) for the shock with compression ratio $\sigma =4$ and the
ratio of the magnetic fields downstream and upstream
$k^{-1}=\sqrt{11}$. The spectra $F_1$ and $F_2$ obtained
numerically are also shown (thin solid lines). }
\end{figure}

\begin{figure}[t]
\includegraphics[width=8.5cm]{fig4.eps}
\caption{Comparison of the function $R(\omega /\omega _c)$
tabulated by Crusius and Schlickeiser (\cite{crusius86}) (dotted
line) and the function given by the approximate expression (30)
(solid line).  }
\end{figure}

\begin{figure}[t]
\includegraphics[width=8.5cm]{fig5.eps}
\caption{The energy spectra  of synchrotron radiation given by
Eqs. (36),(37) and produced by electrons  in downstream (dashed
line) and upstream (dotted line) regions of the shock with
compression ratio $\sigma =4$ and the ratio of the magnetic fields
downstream and upstream $\kappa ^{-1}=\sqrt{11}$. The
corresponding spectra obtained numerically are also shown (solid
lines).}
\end{figure}

The integrated downstream electron spectrum $F_2$ in Fig.3 and the
corresponding synchrotron spectrum $J_2$ in Fig.5 may be applied
to the supernova remnants with ages  lager than the cooling time given by
Eq.(23), i.e.  when the electron spectrum in the cut-off region
is determined by the energy losses of
electrons. Electrons with energies below cut-off energy are
accelerated with power-law spectrum and  advected downstream. It
was also assumed that these electrons lose all their energy
downstream that is of course valid for energies larger than the
energy of the electron which has the  cooling time comparable with
the age of the remnant. For smaller energies a three-dimensional
geometry of the shock wave should be taken into account.  Consequently,
the integrated downstream electron spectrum and the
corresponding  synchrotron radiation spectrum  appear  flatter
compared to the  ones shown in Figs.3,5.

\subsection{The radiation  zones}

The asymptotic solutions derived in Sec.2 can be used for study of
coordinate-dependence of electron distributions. Near the shock
front, the spatial distribution of electrons  has an exponential
dependence.  The inverse exponential lengths in the upstream and
downstream regions are given by Eqs. (10) and (11). Since the
synchrotron radiation is produced mainly by electrons with
momentum $p_*$, the exponential lengths  of emissivity (29) in the
upstream $l_u$ and downstream $l_d$ regions of the shock can be
found from Eqs. (10),(11) and (31):

\begin{equation}
l_d=\frac {9}{4\sqrt{3(1+\kappa ^{1/2})}} \left( \frac {
m^9c^{17}u_1^2\eta }{\omega q^{12}B^6\gamma _s^2}\right) ^{1/4} \
,
\end{equation}
and
\begin{equation}
l_u=l_d\kappa ^{-5/4} \ .
\end{equation}
In particular, for $\gamma _s=4$ we have
\[
l_d=\frac {1.4\cdot 10^{17}\ \mathrm{\ cm}}{\sqrt{1+\kappa
^{1/2}}} \eta ^{1/4}\left( \frac {u_1}{\mathrm{3000\ km\ }s^{-1}}
\right) ^{1/2}\times
\]
\begin{equation}
\left( \frac B{100\ \mu \mathrm{G}}\right) ^{-3/2} \left( \frac
{\hbar \ \omega }{\mathrm{1\ keV\ }} \right) ^{-1/4} \ ,
\end{equation}
for the radiation width in downstream, and a factor of  $\kappa
^{-5/4}$ larger in upstream. Note that the above  equations are
correct only for  large frequencies, $\omega >\omega _0$.

The radiation width in downstream (40) is relatively small. This
permits to explain the  narrow X-ray filaments observed in SNRs
and to estimate the magnetic field strength (see e.g. Berezhko et
al. \cite{berezhko02}, V\"olk et al. \cite{voelk05}).

\section{Inverse Compton scattering}

In the isotropic photon field,  the emissivity of the inverse
Compton  radiation of an electron with  Lorentz factor $\gamma$  is
described as  (Blumenthal \& Gould \cite{blumenthal70})
\[
\epsilon _{\mathrm{IC}}(\omega )=2\hbar cr_e^2\int \limits ^\infty _{\frac
{\omega }{4\gamma ^2\left( 1-\frac {\hbar \omega }{\gamma
mc^2}\right)}} d\omega 'n(\omega ') \frac {\omega }{4\gamma
^2\omega '} \left[ 1-2\frac {\omega ^2}{\omega _c^2}+\right.
\]
\begin{equation}
\left. \frac {\omega }{\omega _c }\left( 1+2\ln \frac
{\omega }{\omega _c}\right)
+\frac {\hbar ^2\omega ^2}{2m^2c^4\gamma ^2
\left( 1-\frac {\hbar \omega }{\gamma mc^2}\right)}\left( 1-\frac {\omega
}{\omega _c}\right) \right] .
\end{equation}
Here $\omega _c=4\omega '\gamma ^2\left( 1-\frac {\hbar \omega
}{\gamma mc^2}\right) $ , $r_e=q^2/mc^2$ is the classical electron
radius and $n(\omega)$ is the energy distribution of  the target
photons. Hereafter we assume that the target photons are described by
a Planckian  distribution
\begin{equation}
n(\omega )=\frac {\omega ^2/(c^3\pi ^2)}{\exp (\hbar \omega
/\kappa_{\mathrm{B}}T)-1} \ ,
\end{equation}
where $T$ is the temperature of radiation {and $\kappa
_{\mathrm{B}}$ is the Boltzman constant}. It is easy to show,
using Eqs. (41) and (42),  that   at large frequencies $\omega
>> \gamma ^2\kappa _{\mathrm{B}}T/\hbar $ the IC  emissivity in the Thompson regime
behaves as   $\epsilon _{\mathrm{IC}}(\omega) \propto \omega \exp
(-\hbar \omega /4\gamma ^2\kappa _{\mathrm{B}}T)$. At very high
energies  the integration over the electron energy distribution at
the shock and the use of the method described in the Section
3,  give the following asymptotic form  of the IC spectrum in the
Thompson limit:
\begin{equation}
J^{\mathrm{IC}}\propto \omega ^{7/8}\exp (-\sqrt{\omega /\omega _b}) \ ,
\end{equation}
with
\begin{equation}
\omega _b=\frac {27}{2\eta \left( 1+\kappa^{1/2}\right) ^2} \frac
{\kappa _{\mathrm{B}}Tu_1^2m^2c^2}{\hbar \gamma ^2_sq^3B} \ ,
\end{equation}
or, in terms of energy of gamma-rays,
$\epsilon _b=\hbar \omega _b$, we have:
\begin{equation}
\epsilon _b=\frac {\mathrm{1.2\ TeV}}{\eta
(1+\kappa^{1/2})^2}\left( \frac {u_1}{\mathrm{3000\ km\ }s^{-1}}
\right) ^2 \frac {100\ \mu \mathrm{G}}{B}\frac {T}{2.7\
\mathrm{K}} \frac {16}{\gamma _s^2} .
\end{equation}
As before, it is  assumed that synchrotron losses dominate over IC losses,
i.e.  the energy density of the background radiation
$U_{\mathrm{rad}}<<B^2/8\pi $. In the case of 2.7 K CMBR this
implies $B \ge  3 \mu \rm G$.

Using the exact asymptotic spectra at low and high energies,
and  the results of numerical calculations at  intermediate energies,
we can describe the broad-band energy flux of the
inverse Compton  (Thompson) scattering  by simple analytical
expressions.   In particular, for $\kappa=1$ one has
\begin{equation}
J^{\mathrm{IC}}(\omega )\propto \frac {\omega _b}{\omega }\left[ 1+
0.36\left( \frac {\omega }{\omega _b} \right) ^{0.7}\right]
^{15/5.6} \exp \left(-\sqrt{\frac {\omega }{\omega _b}} \ \right)
\end{equation}

\begin{figure}[t]
\includegraphics[width=8.5cm]{fig6.eps}
\caption{The spectrum of IC radiation given by Eqs. (47),(48) and
produced by electrons accelerated downstream (dashed line) and
upstream (dotted line) the shock with compression ratio $\sigma
=4$ and the ratio of the magnetic strength downstream and upstream
$\sqrt{11}$. The sum
$J^{\mathrm{IC}}=J^{\mathrm{IC}}_1+J^{\mathrm{IC}}_2$ is shown by
the solid line. It is assumed that IC scattering proceeds in the
Thompson limit,  $b_{\rm KN}=0$, and that synchrotron losses
dominate over the IC loses. The corresponding spectra obtained
numerically are also shown (thin solid lines).}
\end{figure}

For the "standard" scenario of shock acceleration
with  $\gamma _s=4$ and  $\kappa=1/\sqrt{11}$,  we obtain  the
following IC spectra produced upstream and downstream
the shock:
\begin{equation}
J^{\mathrm{IC}}_1(\omega )\propto 0.20\left[ 1+ 0.75\left( \frac {\omega
}{\omega _b}\right) ^{7/8} \right] \exp \left (-\sqrt{\frac
{\omega }{\omega _b}} \ \right) ,
\end{equation}
\begin{equation}
J^{\mathrm{IC}}_2(\omega )\propto \frac {\omega _b}{\omega }\left[ 1+
0.31\left( \frac {\omega }{\omega _b}\right) ^{0.6} \right]
^{25/8} \exp \left( -\sqrt{\frac {\omega }{\omega _b}} \ \right) .
\end{equation}
The spectra given by Eqs. (47) and (48) are shown in Fig.6. They are
derived under the assumption that the Compton
scattering occurs  in the Thompson regime. However,  in many cases
one  should take into account the Klein-Nishina effect. The
importance of this effect in the case of black-body radiation
field is determined by the  parameter
\[
b_{KN}=4\frac {\kappa _{\mathrm{B}}Tp_0}{m^2c^3}= \frac
{0.52}{\gamma _s\eta ^{1/2}(1+\kappa^{1/2})} \times
\]
\begin{equation}
\left( \frac
{u_1}{3000\ \mathrm{km\ s}^{-1}} \right) \left( \frac {B}{100\ \mu
\mathrm{G} }\right) ^{-1/2}\frac {T}{2.7\ \mathrm{K}} \ .
\end{equation}
The Thompson limit corresponds to $b_{KN}<<1$, while the
Klein-Nishina effect becomes significant  already at $b_{KN} \geq
0.1$.  The IC spectra of electrons calculated for different values
of the parameter $b_{KN}$ are shown in Fig.7.

\begin{figure}[t]
\includegraphics[width=9.0cm]{fig7.eps}
\caption{The spectra of IC radiation produced by electrons
accelerated at the shock with compression ratio $\sigma =4$ and
the ratio of the magnetic strength downstream and upstream
$\sqrt{11}$ for different values of $b_{KN}$: $b_{KN}=0$ (solid
line), $b_{KN}=0.1$ (dashed line), $b_{KN}=0.3$ (dotted line),
$b_{KN}=1.0$ (thin solid line), $b_{KN}=3.0$ (thing dashed line)
and $b_{KN}=10.0$ (thin dotted line). The case of dominating
synchrotron losses is considered. }
\end{figure}

As long as the energy losses of electrons are dominated by
synchrotron radiation, the  Klein-Nishina effect  makes steeper
the spectrum of IC gamma-rays.
In particular,  it moves the region of the spectral cutoff to lower
energies.  Below the cutoff region,  the energy spectrum
of  IC gamma-rays  still can be described by a  (quasi) power-law.
The Klein-Nishina effect changes the slope of the gamma-ray
spectrum  significantly,  even for relatively small values of the
parameter $b_{KN}$.

\section{Discussion}

The detection of nonthermal X-ray emission of synchrotron origin
clearly demonstrates the existence of multi-TeV electrons in
different astrophysical source populations like shell type SNRs --
pulsar wind nebulae, microquasars,  small and large scale jets in AGN,  \textit{etc.}
Given the severe synchrotron  losses of electrons, which increase with
energy as $dE/dt \propto E^2$, the acceleration efficiency
in these objects  should be very high in order to boost the electrons
to energies well beyond 1 TeV.
In particular, in young SNRs with  typical shock speeds
$u_1 \sim 2000-3000 \ \rm km/s$, which are established
as prominant nonthermal X-ray emitters,  the diffusive shock
acceleration of electrons should proceed in the regime close to
the Bohm diffusion limit,  otherwise the synchrotron spectrum  would
break before achieving the X-ray domain.

Although the basic concepts
of diffusive shock acceleration are  deeply studied and well understood
(see e.g. Malkov and Drury \cite{malkov01}), many  important
details remain   unexplored. This concerns, in particular the radiation features
of the shock accelerated electrons.  Over  the recent years,
several numerical calculations of high energy radiation by
particles accelerated in young SNRs have been performed
with emphasis on the non-linear effects caused by protons and
nuclei on  the shock structure (see e.g.
Ellison et al. \cite{Ellison2000}, Berezhko and V\"olk \cite{berezhko04}).

The shock accelerated electron spectra have been studied analytically
(e.g. by  Webb et al. \cite{webb84}), but  only for the
case of energy-independent  diffusion coefficient. Therefore
the results of these early works  generally cannot be applied to the most interesting
sources with synchrotron X-ray emission.  These sources, as noticed above,
require diffusive shock acceleration of electrons in the regime
close to the Bohm diffusion which is characterized by a
diffusion coefficient  $D(E) \propto E$.

The aim of this paper  was  a fully analytical treatment of  the energy
spectra  of shock-accelerated electrons and their  synchrotron and inverse
Compton radiation for  an arbitrary  energy-dependent
diffusion coefficient.  In particular, under the assumption
of dominance of synchrotron losses, we derived exact  asymptotic
solutions in the  high  energy  region.  For the energy-dependent diffusion
coefficient written in a rather general form $D\propto p^\alpha$,
the electron spectrum contains an exponential  term
$\exp [-(p/p_0)^\beta]$ with $\beta=\alpha+1$ (see Eq.(19)).
Thus,  only in the  case of energy-independent diffusion ($\alpha=0$) the
electron spectrum is characterized by an exponential cutoff. In the
most interesting case of  Bohm diffusion,
the spectral cut-off is of Gaussian type,  $\exp [-(p/p_0)^2]$.
The corresponding cutoff in the spectrum of syncrotron radiation
appears much smoother (see also Fritz
\cite{fritz89} for discussion of this effect).  It is described
by an exponential term
$\exp[-(\omega/\omega_0)^{\beta/(2+\beta)}]
=\exp [-(\omega/\omega_0)^{(\alpha +1)/(\alpha +3)}]$.
For the energy independent diffusion coefficient we have
$J(\omega) \propto \exp[-(\omega/\omega_0)^{1/3}]$,
while in the case of Bohm diffusion
$J(\omega) \propto \exp[-(\omega/\omega_0)^{1/2}]$.

We should note that the  $\exp [-(\omega/\omega_0)^{1/2}]$ type behavior
of the synchrotron spectrum in the cutoff region
\textit{formally} is similar to the one derived
for the  generally  assumed  "power-law with
exponential cutoff" electron spectrum,
$N_0(p) \propto p^{-\Gamma} \exp(-p/p_0)$,
and using the $\delta $-function approximation for
calculation of the synchrotron radiation
(see e.g. Reynolds \cite{Reynolds98}).  However, this is
simply a coincidence.  First of all, the $\delta$-functional
approximation leads to a wrong synchrotron spectrum;
the exponential cut-off in the electron spectrum
results in the synchrotron spectrum
with a $\exp (-\omega ^{1/3})$ type cut-off.
More importantly, the spectra  of shock accelerated electrons
given by  Eq.(26)-(28)
are quite different from the simplified  "power-law with
exponential cutoff"  assumption. Correspondingly, because of the
dependence $\omega_c \propto p^2 B$, the effect on
the spectrum  of  synchrotron radiation appears
even more pronounced (see Fig.2).

Exact  solutions for electrons are possible only at low and high
energies, namely in the energy intervals where (\textit{i}) the
radiative losses of electrons are negligible,  and  (\textit{ii})
the radiative energy loss rate exceeds the acceleration rate. The
indices  of the  power-law factors in the asymptotic solutions
(19),(32) and (43)  significantly  differ from the power-law
indices of the electrons, as well as the synchrotron and IC
spectra below the cut-off regions.  In order to connect these
solutions we performed numerical  calculations in the intermediate
energy intervals. This  allowed us to obtain, within accuracy
better than 10 percent, simple analytical presentations for  the
spectra  of electrons and their synchrotron and inverse Compton
radiation components.

Eqs. (35)-(37) and Eqs. (46)-(48) properly  describe the  relative
contributions of radiation from  the regions upstream and
downstream the shock. At the same time,  they do not allow  direct
calculations of  the absolute synchrotron and inverse Compton
luminosities. However, the normalisation constants  can be easily
calculated  from the total energy release through the synchrotron
and inverse Compton channels.

It should be  noted  that in this paper the momentum $p_0$ in the
electron spectrum, and the corresponding frequencies $\omega _0$
and $\omega _b$ which characterize the positions of cut-offs in
the spectra of synchrotron and IC radiation components, are found
from the exact asymptotic solutions of kinetic equations.
Interestingly, the results appear quite close, within a factor of
2,  to   the estimates  derived from the condition "acceleration
rate = synchrotron cooling rate". However, as it follows  from
Fig. 2-6, the real cut-offs  appear, in fact, at much higher
frequencies.  In the case of synchrotron radiation, the spectrum
continues without an indication of a break or a cutoff up to  $20
\omega _0$. The spectrum of  inverse Compton gamma-rays turns down
also at $\omega \sim 20 \omega _b$ (in the case of constant
magnetic field), or it continues up to $\sim 50 \omega _b$ (in the
case of different magnetic fields upstream
 and downstream).  The more effective extension of
the hard spectrum of IC radiation  is explained by  the larger
spatial scale of electron distribution upstream the shock. This is
not  important  for the synchrotron radiation the contribution of
which from the upstream region is suppressed by an order of
magnitude.  On the other hand, because of the homogeneous
distribution of the target radiation field, 2.7 K CMBR, the IC
gamma-ray contribution at highest energies from  the upstream
region dominates over the contribution from the downstream region.

The results obtained in this paper can be used to fit the  X-ray
spectra observed from young supernova remnants. The value of the
parameter $\omega _0$ found from the fitting procedure should be
compared with the theoretical value given by Eq.(33). For the
known shock velocity of a given supernova remnant, this would
allow an important estimate of deviation of the diffusion regime
from the extreme Bohm limit. The dependence of the energy spectra
 on the factor $\eta $ is expressed via parameters $p_0$,
$\omega _0$, $\omega _b$. If the width of X-ray
filaments is known, the magnetic field strength may be found from
Eq. (40). All this in turn would provide reliable estimates of the
maximum energy of protons and nuclei accelerated in supernova
remnants.

Finally, we  note  that the results of this paper
are applicable for  nonrelativistic shocks with
velocities   up to  $u_1 \sim  (0.1-0.3) c$. The derived
analytical approximations do not  take into account
possible nonlinear effects which
can somewhat modify the spectra of electrons at low and high energies.

\acknowledgement{VNZ acknowledges the hospitality of the
Max-Planck-Institut f\"ur Kernphysik, where this work was carried
out. We thank the anonymous referee for many valuable comments. }

redpajama_set_name: RedPajamaArXiv


text:
Q: Deleting node without deleting root node This is my xml :
<?xml version="1.0" encoding="utf-8"?>
<Videos>
    <Playlist>
    </Playlist>
</Videos>

xml i want :
<?xml version="1.0" encoding="utf-8"?>
<Videos>
</Videos>

I tried something like :
List<XNode> t = xmlDoc.Element("Videos").DescendantNodes().ToList();
  foreach (XNode a in t)
   {
     if (((System.Xml.Linq.XElement)a).Value == "")
                a.Remove();
  }

But i get this result :
<?xml version="1.0" encoding="utf-8"?>
<Videos />

Can somebody help ? :/

A: <Videos>
</Videos>

and
<Videos />

is the same thing. So, Where is the problem ?

redpajama_set_name: RedPajamaStackExchange


EVEREST is Anjali's story, a young girl who aspires to conquer her own personal EVEREST - of getting her father's love and respect. At the age of 21, she is faced with the biggest conflict of her life and is forced to question her very own existence. To redeem herself and find a place in her father's heart she decides to fulfill her father's unfulfilled dream - to summit the greatest and highest of all mountains, Mt Everest.
EVEREST FINALE - An Inspiring Show, story of Anjali-Akash-Arjun!
The epic saga 'Naagarjun' confirms another ENTRY!


text:
Q: Creating a mobile app based on the ASP.NET Core website Coming from Desktop development, I'm in the middle of my very first web project (as a small side/learning-project). I'm using ASP.NET Core 2. I'm already thinking about going mobile too.
What are my best options here?
First thing that comes to my mind is separating logic and data interactions into web API, which will run along side the website frontend. Website will consume logic via REST. As for a mobile, I could use Xamarin and consume, logic, data persistence and authentication from API as well. I'll have to build UI twice, for web and mobile.. but I guess I can't avoid that.
Is it the way to go?
Thanks for suggestions,

A: My experience with xamarin is that its a bit of a jack of all trades.
If you are keen to keep with a single tech stack then yes, .net core/framework apis + xamarin + azure is great. You can quickly get an app out on iPhone, Android and Windows
But, if you want a very polished app, which uses the UI specific to each platform to ita best advantages you may find that xamarin lets you down a bit.
Your other option would be to make a web app designed for mobile.

A: I would add to the previous answer above to avoid Xamarin Forms if you really want good UI. And use instead Xamarin Native which means you would need to create 2 separate UI, one for Android and one for IOS. The only disadvantage is that you need Mac for the IOS


text:
Home News Scottish News Former Prince Charming panto star misses out on "Porn Oscar"
Former Prince Charming panto star misses out on "Porn Oscar"
By Jenny Kane -
A FORMER panto star, sacked from his role as Prince Charming after it emerged he appeared in adult movies, has missed out on a porn 'Oscar'.
Craig Chalmers, who performs under the name Ryan Ryder, shot to fame after making it to the finals of a BBC talent show Any Dream Will Do.
But 32-year-old was axed from a Dunfermline production of Cinderella after an anonymous tip off from a member of the public.
Craig Chalmers shot to fame after making it to the finals of a BBC talent show Any Dream Will Do
The Scot was nominated for the for the Best Foreign Male award at the AVN Awards – known as the Oscars of porn.
Mr Chalmers, who films include Hotel Voyeur and Fade Into You, had previously said: he was "delighted with the nomination."
His wife Jennifer Smith, who performs under the name Jasmine Jae, was also up for Best Foreign female.
But at a glitzy ceremony in Las Vegas at the weekend it was revealed both had lost out on the gong.
The Scot was nominated for the for the Best Foreign Male award at the AVN Awards – known as the Oscars of porn
Craig lost out to Italian porn veteran Rocco Siffredi who has starred in more than 1,300 films.
Meanwhile his wife was pipped to the post by French star of Ultimate French Girls 3, Anissa Kate.
The AVN Awards are sponsored by the adult video industry trade magazine AVN and is aired on American TV.
It was two years ago when Mr Chalmers lost his leading role in Cinderella with his X-rated revelation also seeing him axed by his talent agency.
Thr 32-year-old was axed from a Dunfermline production of Cinderella after an anonymous tip off
The Alhambra Theatre in Dunfermline even removed his face from the poster for the show and replaced him with CBBC star James Mackenzie.
Now Edinburgh-born Chalmers, who was also part of the short-lived boyband No Reason and an all-male strip group G-Force, is also turning his hand to producing adult movies.
Craig Chalmers
Alhambre Theatre
Previous articleIain Banks inspiring space travel
Next articleEdinburgh researchers find sugar solution reduces the risk of osteoarthritis
Jenny Kane
http://www.deadlinenews.co.uk/2015/01/26/former-prince-charming-panto-star-misses-out-on-porn-oscar/


text:
sportsRangers
Rangers agree to deals with international prospects Anthony Gutierrez, Jose de Jesus
The Rangers announced deals with 17 players on Saturday.
Texas Rangers President Jon Daniels talks with media at Globe Life Field in Arlington on Monday Jan. 10, 2022. Six players previously spoke after the Texas Rangers Player Development Camp.(Staff Photographer)
By Evan Grant
1:27 PM on Jan 15, 2022 CST
Update: This story has been updated.
While everything involving major league players remains ground to a standstill due to the lockout, the Rangers did agree to plunk down more than $3 million on a pair of Latin American teenagers as the international free agent signing period began Saturday.
The Rangers announced deals with 17 players on Saturday, headed by the outfield duo of Anthony Gutierrez (Venezuela) and Jose de Jesus (Dominican Republic). According to sources, Gutierrez, who was ranked as the 13th best international prospect by Baseball America, received $2 million, while de Jesus, ranked 35th, received a $1.2 million bonus. Both signed Saturday
The Rangers have a total of $5,179,700 to use on international free agents for the 2021-2022 signing period, which technically began Saturday. Players signed for less than $10,000 do not count against the cap.
The Rangers also signed shortstops Daniel Bruzual, Echedry Vargas, Luis Marquez, Esteban Meijia, Kleimer Lemos and Jaiker Garcia, outfielders Roni Cabrera, Yeremy Cabrera, Oliver Yan, and Erik Valbuena and catchers Jesus Lopez and Alfredo Espinoza. None of the large signing class, however, were pitchers. All of the teens came from Venezuela and the Dominican Republic.
Gutierrez, 17, was the highest rated prospect among the deals. He was linked initially to the Washington Nationals, but had switched over to the Rangers in the last few months. According to Baseball America he is one of the better power bats in the class. He reportedly has the athleticism to play center field, but at 6-3, 185, he is expected to grow into a corner outfielder.
Breaking the ice: With MLB in deep freeze, Rangers are planting seeds of leadership with prospects
Find more Rangers coverage from The Dallas Morning News here.
Evan Grant, Rangers beat writer/insider. Evan has covered the Rangers since 1997. He has twice been named one of the top 10 beat writers in the country by the AP Sports Editors. His passions outside of covering baseball are his wife, Gina, his two step kids, two crazy dogs & barbecue. Let's not discuss the cat. Evan graduated from Georgia State University, but oddly is a Georgia fan.
egrant@dallasnews.com @Evan_P_Grant
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