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Article: Hubble Space Telescope and ground-based observations of SN 1993J and SN 1998S: CNO processing in the progenitors

TitleHubble Space Telescope and ground-based observations of SN 1993J and SN 1998S: CNO processing in the progenitors
Authors
KeywordsCircumstellar matter
Nuclear reactions, nucleosynthesis, abundances
Stars: evolution
Stars: mass loss
Supernovae: individual (SN 1993J, SN 1998S)
Issue Date2005
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2005, v. 622 n. 2 I, p. 991-1007 How to Cite?
AbstractGround-based and Hubble Space Telescope observations are presented for SN 1993J and SN 1998S. SN 1998S shows strong, relatively narrow circumstellar emission lines of N III-V and C III-IV, as well as broad lines from the ejecta. Both the broad ultraviolet and optical lines in SN 1998S indicate an expansion velocity of ∼7000 km s -1. The broad emission components of Lyα and Mg II are strongly asymmetrical after day 72 past the explosion and differ in shape from Hα. Different models based on dust extinction from dust in the ejecta or shock region, in combination with Hα from a circumstellar torus, are discussed. It is concluded, however, that the double-peaked line profiles are more likely to arise as a result of optical depth effects in the narrow, cool, dense shell behind the reverse shock than in a torus-like region. The ultraviolet lines of SN 1993J are broad, with a boxlike shape, coming from the ejecta and a cool, dense shell. The shapes of the lines are well fitted by a shell with inner velocity ∼7000 km s -1 and outer velocity ∼10,000 km s -1. For both SN 1993J and SN 1998S a strong nitrogen enrichment is found, with N/C ≈ 12.4 in SN 1993J and N/C ≈ 6.0 in SN 1998S. From a compilation of all supernovae with determined CNO ratios, we discuss the implications of these observations for the structure of the progenitors of Type II supernovae. © 2005. The American Astronomical Society. All rights reserved,.
Persistent Identifierhttp://hdl.handle.net/10722/43477
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorFransson, Cen_HK
dc.contributor.authorChallis, PMen_HK
dc.contributor.authorChevalier, RAen_HK
dc.contributor.authorFilippenko, AVen_HK
dc.contributor.authorKirshner, RPen_HK
dc.contributor.authorKozma, Cen_HK
dc.contributor.authorLeonard, DCen_HK
dc.contributor.authorMatheson, Ten_HK
dc.contributor.authorBaron, Een_HK
dc.contributor.authorGarnavich, Pen_HK
dc.contributor.authorJha, Sen_HK
dc.contributor.authorLeibundgut, Ben_HK
dc.contributor.authorLundqvist, Pen_HK
dc.contributor.authorPun, CSJen_HK
dc.contributor.authorWang, Len_HK
dc.contributor.authorWheeler, JCen_HK
dc.date.accessioned2007-03-23T04:46:27Z-
dc.date.available2007-03-23T04:46:27Z-
dc.date.issued2005en_HK
dc.identifier.citationAstrophysical Journal Letters, 2005, v. 622 n. 2 I, p. 991-1007en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43477-
dc.description.abstractGround-based and Hubble Space Telescope observations are presented for SN 1993J and SN 1998S. SN 1998S shows strong, relatively narrow circumstellar emission lines of N III-V and C III-IV, as well as broad lines from the ejecta. Both the broad ultraviolet and optical lines in SN 1998S indicate an expansion velocity of ∼7000 km s -1. The broad emission components of Lyα and Mg II are strongly asymmetrical after day 72 past the explosion and differ in shape from Hα. Different models based on dust extinction from dust in the ejecta or shock region, in combination with Hα from a circumstellar torus, are discussed. It is concluded, however, that the double-peaked line profiles are more likely to arise as a result of optical depth effects in the narrow, cool, dense shell behind the reverse shock than in a torus-like region. The ultraviolet lines of SN 1993J are broad, with a boxlike shape, coming from the ejecta and a cool, dense shell. The shapes of the lines are well fitted by a shell with inner velocity ∼7000 km s -1 and outer velocity ∼10,000 km s -1. For both SN 1993J and SN 1998S a strong nitrogen enrichment is found, with N/C ≈ 12.4 in SN 1993J and N/C ≈ 6.0 in SN 1998S. From a compilation of all supernovae with determined CNO ratios, we discuss the implications of these observations for the structure of the progenitors of Type II supernovae. © 2005. The American Astronomical Society. All rights reserved,.en_HK
dc.format.extent748725 bytes-
dc.format.extent26624 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypeapplication/msword-
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.subjectCircumstellar matteren_HK
dc.subjectNuclear reactions, nucleosynthesis, abundancesen_HK
dc.subjectStars: evolutionen_HK
dc.subjectStars: mass lossen_HK
dc.subjectSupernovae: individual (SN 1993J, SN 1998S)en_HK
dc.titleHubble Space Telescope and ground-based observations of SN 1993J and SN 1998S: CNO processing in the progenitorsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=622&issue=2 pt 1&spage=991&epage=1007&date=2005&atitle=Hubble+space+telescope+and+ground-based+observations+of+SN+1993J+and+SN+1998S:+CNO+processing+in+the+progenitorsen_HK
dc.identifier.emailPun, CSJ: jcspun@hkucc.hku.hken_HK
dc.identifier.authorityPun, CSJ=rp00772en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/426495en_HK
dc.identifier.scopuseid_2-s2.0-19944397125en_HK
dc.identifier.hkuros98586-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-19944397125&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume622en_HK
dc.identifier.issue2 Ien_HK
dc.identifier.spage991en_HK
dc.identifier.epage1007en_HK
dc.identifier.isiWOS:000228093400021-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridFransson, C=7004051800en_HK
dc.identifier.scopusauthoridChallis, PM=7004555495en_HK
dc.identifier.scopusauthoridChevalier, RA=7101871369en_HK
dc.identifier.scopusauthoridFilippenko, AV=34568722000en_HK
dc.identifier.scopusauthoridKirshner, RP=35277140000en_HK
dc.identifier.scopusauthoridKozma, C=12800852100en_HK
dc.identifier.scopusauthoridLeonard, DC=7201953982en_HK
dc.identifier.scopusauthoridMatheson, T=7006957627en_HK
dc.identifier.scopusauthoridBaron, E=7102558228en_HK
dc.identifier.scopusauthoridGarnavich, P=7006524172en_HK
dc.identifier.scopusauthoridJha, S=7202726891en_HK
dc.identifier.scopusauthoridLeibundgut, B=7007116593en_HK
dc.identifier.scopusauthoridLundqvist, P=7004499555en_HK
dc.identifier.scopusauthoridPun, CSJ=7003931846en_HK
dc.identifier.scopusauthoridWang, L=7409176960en_HK
dc.identifier.scopusauthoridWheeler, JC=7403110438en_HK

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