File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Afterglow emission from highly collimated jets with flat electron spectra: Application to the GRB 010222 case?

TitleAfterglow emission from highly collimated jets with flat electron spectra: Application to the GRB 010222 case?
Authors
KeywordsGamma rays: Bursts
Relativity
Shock waves
Issue Date2001
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2001, v. 558 n. 2 PART 2, p. L109-L112 How to Cite?
AbstractWe derive light curves of the afterglow emission from highly collimated jets if the power-law index (p) of the electron energy distribution is above 1 but below 2. We find the following: (1) Below the characteristic synchrotron frequency, the light-curve index depends generally on p. (2) As long as the jet expansion is spherical, the light-curve index above the characteristic frequency increases slowly as the spectral index of the emission increases. (3) Once the jet enters the spreading phase, the high-frequency emission flux decays as proportional to t -(p+6)/4 rather than proportional to t -p. All these results differ from those in the case of p > 2. We compare our analytical results with the observations on the GRB 010222 afterglow and conclude that the jet model may be unable to explain the observed data. Thus, a more promising explanation for this afterglow seems to be the expansion of a relativistic fireball or a mildly collimated jet in a dense medium.
Persistent Identifierhttp://hdl.handle.net/10722/43332
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorDai, ZGen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2007-03-23T04:43:44Z-
dc.date.available2007-03-23T04:43:44Z-
dc.date.issued2001en_HK
dc.identifier.citationAstrophysical Journal Letters, 2001, v. 558 n. 2 PART 2, p. L109-L112en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43332-
dc.description.abstractWe derive light curves of the afterglow emission from highly collimated jets if the power-law index (p) of the electron energy distribution is above 1 but below 2. We find the following: (1) Below the characteristic synchrotron frequency, the light-curve index depends generally on p. (2) As long as the jet expansion is spherical, the light-curve index above the characteristic frequency increases slowly as the spectral index of the emission increases. (3) Once the jet enters the spreading phase, the high-frequency emission flux decays as proportional to t -(p+6)/4 rather than proportional to t -p. All these results differ from those in the case of p > 2. We compare our analytical results with the observations on the GRB 010222 afterglow and conclude that the jet model may be unable to explain the observed data. Thus, a more promising explanation for this afterglow seems to be the expansion of a relativistic fireball or a mildly collimated jet in a dense medium.en_HK
dc.format.extent73091 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectGamma rays: Burstsen_HK
dc.subjectRelativityen_HK
dc.subjectShock wavesen_HK
dc.titleAfterglow emission from highly collimated jets with flat electron spectra: Application to the GRB 010222 case?en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=558&issue=pt 2&spage=L109&epage=L112&date=2001&atitle=Afterglow+Emission+from+Highly+Collimated+Jets+with+Flat+Electron+Spectra:+Application+to+the+GRB+010222+Case?en_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/323566en_HK
dc.identifier.scopuseid_2-s2.0-0035840523en_HK
dc.identifier.hkuros64924-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0035840523&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume558en_HK
dc.identifier.issue2 PART 2en_HK
dc.identifier.spageL109en_HK
dc.identifier.epageL112en_HK
dc.identifier.isiWOS:000171002700009-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridDai, ZG=7201387760en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats