File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Modeling the optical afterglow of GRB 030329

TitleModeling the optical afterglow of GRB 030329
Authors
KeywordsGamma Rays: Bursts
Ism: Jets And Outflows
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 637 n. 2 I, p. 873-879 How to Cite?
AbstractThe best-sampled afterglow light curves available are for GRB 030329. A distinguishing feature of this event is the obvious rebrightening at around 1.6 days after the burst. Proposed explanations for the rebrightening mainly include the two-component jet model and the refreshed-shock model, although a sudden density jump in the circumburst environment is also a potential choice. Here we reexamine the optical afterglow of GRB 030329 numerically in light of the three models. In the density-jump model, no obvious rebrightening can be produced at the jump moment. In addition, after the density jump, the predicted flux density decreases rapidly to a level that is significantly below observations. A simple density-jump model thus can be excluded. In the two-component jet model, although the observed late afterglow (after 1.6 days) can potentially be explained as emission from the wide component, the emergence of this emission actually is too slow, and it does not manifest as a rebrightening as previously expected. The energy-injection model seems to be the most preferred choice. By engaging a sequence of energy-injection events, it provides an acceptable fit to the rebrightening at ∼1.6 days, as well as the whole observed light curve that extends to ~80 days. Further studies on these multiple energy-injection processes may provide a valuable insight into the nature of the central engines of gamma-ray bursts. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/174997
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHuang, YFen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorGao, TTen_US
dc.date.accessioned2012-11-26T08:48:42Z-
dc.date.available2012-11-26T08:48:42Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 637 n. 2 I, p. 873-879en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174997-
dc.description.abstractThe best-sampled afterglow light curves available are for GRB 030329. A distinguishing feature of this event is the obvious rebrightening at around 1.6 days after the burst. Proposed explanations for the rebrightening mainly include the two-component jet model and the refreshed-shock model, although a sudden density jump in the circumburst environment is also a potential choice. Here we reexamine the optical afterglow of GRB 030329 numerically in light of the three models. In the density-jump model, no obvious rebrightening can be produced at the jump moment. In addition, after the density jump, the predicted flux density decreases rapidly to a level that is significantly below observations. A simple density-jump model thus can be excluded. In the two-component jet model, although the observed late afterglow (after 1.6 days) can potentially be explained as emission from the wide component, the emergence of this emission actually is too slow, and it does not manifest as a rebrightening as previously expected. The energy-injection model seems to be the most preferred choice. By engaging a sequence of energy-injection events, it provides an acceptable fit to the rebrightening at ∼1.6 days, as well as the whole observed light curve that extends to ~80 days. Further studies on these multiple energy-injection processes may provide a valuable insight into the nature of the central engines of gamma-ray bursts. © 2006. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectGamma Rays: Burstsen_US
dc.subjectIsm: Jets And Outflowsen_US
dc.titleModeling the optical afterglow of GRB 030329en_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/498423en_US
dc.identifier.scopuseid_2-s2.0-32944477709en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-32944477709&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume637en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage873en_US
dc.identifier.epage879en_US
dc.identifier.isiWOS:000235131600030-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHuang, YF=24448042100en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridGao, TT=35962374700en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats