Synchrotron Self-Compton Model for PKS 2155–304

H.E.S.S. observed TeV blazar PKS 2155-304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2008-08, Vol.682 (2), p.784-788
Main Authors: Kusunose, Masaaki, Takahara, Fumio
Format: Article
Language:English
Subjects:
Astronomy
Earth, ocean, space
Exact sciences and technology
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63
cites cdi_FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63
container_end_page 788
container_issue 2
container_start_page 784
container_title The Astrophysical journal
container_volume 682
creator Kusunose, Masaaki
Takahara, Fumio
description H.E.S.S. observed TeV blazar PKS 2155-304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz factor [image]100, the size of the emission region [image]10 super(15) cm, and magnetic field [image]0.1 G explain the observed spectral energy distribution and the flare timescale of [image]a few minutes. This model with a large value of Gamma accounts for the emission spectrum not only in the TeV band but also in the X-ray band. The major cooling process of electrons/positrons in the jet is inverse Compton scattering off synchrotron photons. The energy content of the jet is highly dominated by particle kinetic energy over magnetic energy.
doi_str_mv 10.1086/589233
format article
fullrecord <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_crossref_primary_10_1086_589233</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>19311401</sourcerecordid><originalsourceid>FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63</originalsourceid><addsrcrecordid>eNp90ctKxDAUBuAgCo6jPkNdqCBUk5zcupTBGyoKo-AuxDTBSqepSWcxO9_BN_RJbJlBF6Krw4GPH85_ENol-JhgJU64KijAGhoRDipnwOU6GmGMWS5APm2irZReh5UWxQiR6aKxLzF0MTTZ1NU-n4RZ2_XLbShdnfkQs_vraUYJ55_vH4DZNtrwpk5uZzXH6PH87GFymd_cXVxNTm9yyyTvcss54FIooFg6aSQALblxgnjsvJRMEcWfgWFTCKWsMJJI5xwrDS7LHgoYo8NlbhvD29ylTs-qZF1dm8aFedKSAStUf2wvD_6VpABCGCY_0MaQUnRet7GambjQBOuhO73srof7q0STrKl9NI2t0remmDMJBe_d3tJVof076-i3GfrXwzu0UFRTLRXTbenhC2bhgfs</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>19311401</pqid></control><display><type>article</type><title>Synchrotron Self-Compton Model for PKS 2155–304</title><source>EZB Free E-Journals</source><creator>Kusunose, Masaaki ; Takahara, Fumio</creator><creatorcontrib>Kusunose, Masaaki ; Takahara, Fumio</creatorcontrib><description>H.E.S.S. observed TeV blazar PKS 2155-304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz factor [image]100, the size of the emission region [image]10 super(15) cm, and magnetic field [image]0.1 G explain the observed spectral energy distribution and the flare timescale of [image]a few minutes. This model with a large value of Gamma accounts for the emission spectrum not only in the TeV band but also in the X-ray band. The major cooling process of electrons/positrons in the jet is inverse Compton scattering off synchrotron photons. The energy content of the jet is highly dominated by particle kinetic energy over magnetic energy.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/589233</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Chicago, IL: IOP Publishing</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology</subject><ispartof>The Astrophysical journal, 2008-08, Vol.682 (2), p.784-788</ispartof><rights>2008 INIST-CNRS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63</citedby><cites>FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&amp;idt=20547395$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Kusunose, Masaaki</creatorcontrib><creatorcontrib>Takahara, Fumio</creatorcontrib><title>Synchrotron Self-Compton Model for PKS 2155–304</title><title>The Astrophysical journal</title><description>H.E.S.S. observed TeV blazar PKS 2155-304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz factor [image]100, the size of the emission region [image]10 super(15) cm, and magnetic field [image]0.1 G explain the observed spectral energy distribution and the flare timescale of [image]a few minutes. This model with a large value of Gamma accounts for the emission spectrum not only in the TeV band but also in the X-ray band. The major cooling process of electrons/positrons in the jet is inverse Compton scattering off synchrotron photons. The energy content of the jet is highly dominated by particle kinetic energy over magnetic energy.</description><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2008</creationdate><recordtype>article</recordtype><recordid>eNp90ctKxDAUBuAgCo6jPkNdqCBUk5zcupTBGyoKo-AuxDTBSqepSWcxO9_BN_RJbJlBF6Krw4GPH85_ENol-JhgJU64KijAGhoRDipnwOU6GmGMWS5APm2irZReh5UWxQiR6aKxLzF0MTTZ1NU-n4RZ2_XLbShdnfkQs_vraUYJ55_vH4DZNtrwpk5uZzXH6PH87GFymd_cXVxNTm9yyyTvcss54FIooFg6aSQALblxgnjsvJRMEcWfgWFTCKWsMJJI5xwrDS7LHgoYo8NlbhvD29ylTs-qZF1dm8aFedKSAStUf2wvD_6VpABCGCY_0MaQUnRet7GambjQBOuhO73srof7q0STrKl9NI2t0remmDMJBe_d3tJVof076-i3GfrXwzu0UFRTLRXTbenhC2bhgfs</recordid><startdate>20080801</startdate><enddate>20080801</enddate><creator>Kusunose, Masaaki</creator><creator>Takahara, Fumio</creator><general>IOP Publishing</general><general>University of Chicago Press</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20080801</creationdate><title>Synchrotron Self-Compton Model for PKS 2155–304</title><author>Kusunose, Masaaki ; Takahara, Fumio</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2008</creationdate><topic>Astronomy</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kusunose, Masaaki</creatorcontrib><creatorcontrib>Takahara, Fumio</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kusunose, Masaaki</au><au>Takahara, Fumio</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Synchrotron Self-Compton Model for PKS 2155–304</atitle><jtitle>The Astrophysical journal</jtitle><date>2008-08-01</date><risdate>2008</risdate><volume>682</volume><issue>2</issue><spage>784</spage><epage>788</epage><pages>784-788</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>H.E.S.S. observed TeV blazar PKS 2155-304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz factor [image]100, the size of the emission region [image]10 super(15) cm, and magnetic field [image]0.1 G explain the observed spectral energy distribution and the flare timescale of [image]a few minutes. This model with a large value of Gamma accounts for the emission spectrum not only in the TeV band but also in the X-ray band. The major cooling process of electrons/positrons in the jet is inverse Compton scattering off synchrotron photons. The energy content of the jet is highly dominated by particle kinetic energy over magnetic energy.</abstract><cop>Chicago, IL</cop><pub>IOP Publishing</pub><doi>10.1086/589233</doi><tpages>5</tpages><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 0004-637X
ispartof The Astrophysical journal, 2008-08, Vol.682 (2), p.784-788
issn 0004-637X
1538-4357
language eng
recordid cdi_crossref_primary_10_1086_589233
source EZB Free E-Journals
subjects Astronomy
Earth, ocean, space
Exact sciences and technology
title Synchrotron Self-Compton Model for PKS 2155–304
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-04T03%3A03%3A12IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Synchrotron%20Self-Compton%20Model%20for%20PKS%202155%E2%80%93304&rft.jtitle=The%20Astrophysical%20journal&rft.au=Kusunose,%20Masaaki&rft.date=2008-08-01&rft.volume=682&rft.issue=2&rft.spage=784&rft.epage=788&rft.pages=784-788&rft.issn=0004-637X&rft.eissn=1538-4357&rft.coden=ASJOAB&rft_id=info:doi/10.1086/589233&rft_dat=%3Cproquest_cross%3E19311401%3C/proquest_cross%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c475t-c5530d683207e7a7332d5ae61f0ef7748185b340a9688c6a717eee4da0ddd5a63%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=19311401&rft_id=info:pmid/&rfr_iscdi=true