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Article: Gamma-ray bursts: Optical afterglows in the deep Newtonian phase

TitleGamma-ray bursts: Optical afterglows in the deep Newtonian phase
Authors
KeywordsGamma-rays: bursts
ISM: jets and outflows
Radiation mechanisms: non-thermal
Stars: neutron
Issue Date2003
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2003, v. 341 n. 1, p. 263-269 How to Cite?
AbstractGamma-ray burst remnants become trans-relativistic typically in days to tens of days, and they enter the deep Newtonian phase in tens of days to months, during which the majority of shock-accelerated electrons will no longer be highly relativistic. However, a small portion of electrons are still accelerated to ultra-relativistic speeds and are capable of emitting synchrotron radiation. The distribution function for electrons is re-derived here so that synchrotron emission from these relativistic electrons can be calculated. Based on the revised model, optical afterglows from both isotropic fireballs and highly collimated jets are studied numerically, and compared to analytical results. In the beamed cases, it is found that, in addition to the steepening due to the edge effect and the lateral expansion effect, the light curves are universally characterized by a flattening during the deep Newtonian phase.
Persistent Identifierhttp://hdl.handle.net/10722/80752
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHuang, YFen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2010-09-06T08:09:53Z-
dc.date.available2010-09-06T08:09:53Z-
dc.date.issued2003en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2003, v. 341 n. 1, p. 263-269en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80752-
dc.description.abstractGamma-ray burst remnants become trans-relativistic typically in days to tens of days, and they enter the deep Newtonian phase in tens of days to months, during which the majority of shock-accelerated electrons will no longer be highly relativistic. However, a small portion of electrons are still accelerated to ultra-relativistic speeds and are capable of emitting synchrotron radiation. The distribution function for electrons is re-derived here so that synchrotron emission from these relativistic electrons can be calculated. Based on the revised model, optical afterglows from both isotropic fireballs and highly collimated jets are studied numerically, and compared to analytical results. In the beamed cases, it is found that, in addition to the steepening due to the edge effect and the lateral expansion effect, the light curves are universally characterized by a flattening during the deep Newtonian phase.en_HK
dc.languageengen_HK
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_HK
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_HK
dc.subjectGamma-rays: burstsen_HK
dc.subjectISM: jets and outflowsen_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.subjectStars: neutronen_HK
dc.titleGamma-ray bursts: Optical afterglows in the deep Newtonian phaseen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0035-8711&volume=341&spage=263&epage=269&date=2003&atitle=Gamma-ray+bursts:+optical+afterglows+in+the+deep+Newtonian+phaseen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1046/j.1365-8711.2003.06430.xen_HK
dc.identifier.scopuseid_2-s2.0-0142087555en_HK
dc.identifier.hkuros76227en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0142087555&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume341en_HK
dc.identifier.issue1en_HK
dc.identifier.spage263en_HK
dc.identifier.epage269en_HK
dc.identifier.isiWOS:000182577300023-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridHuang, YF=7501574835en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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