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Article: SiO maser spectra of V407 cygni after the 2010 march nova outburst

TitleSiO maser spectra of V407 cygni after the 2010 march nova outburst
Authors
KeywordsAGB and post-AGB-stars
Circumstellar matter-stars
Novae, cataclysmic variables-radio lines
Stars
Issue Date2011
PublisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/
Citation
Publications Of The Astronomical Society Of Japan, 2011, v. 63 n. 1, p. 309-315 How to Cite?
AbstractWe report on the time variation of SiO maser emission from the symbiotic stellar system V407 Cygni after the classical nova outburst on 2010 March 10. Although both the SiO J = 1-0 v = 1 and 2 lines at 43.122 and 42.821GHz were found previously in the envelope of amira in the binary system, only weak emission of the J = 1-0 v = 2 line has continuously been detectable after the nova outburst. The line profile exhibited a dramatic change several weeks after the burst; the component on the higher-velocity side of the systemic velocity disappeared two weeks after the burst, and a new persistent component appeared on the lower-velocity side later. These observations indicate that the SiO emitting regions were wiped out on a time scale of two weeks by the nova shock, but a part of the masing region was quickly replenished by cool molecular gases expelled by the mira pulsation. © 2011. Astronomical Society of Japan.
Persistent Identifierhttp://hdl.handle.net/10722/135369
ISSN
2015 Impact Factor: 1.961
2015 SCImago Journal Rankings: 0.804
References

 

DC FieldValueLanguage
dc.contributor.authorDeguchi, Sen_HK
dc.contributor.authorKoike, Ken_HK
dc.contributor.authorKuno, Nen_HK
dc.contributor.authorMatsunaga, Nen_HK
dc.contributor.authorNakashima, JIen_HK
dc.contributor.authorTakahashi, Sen_HK
dc.date.accessioned2011-07-27T01:34:13Z-
dc.date.available2011-07-27T01:34:13Z-
dc.date.issued2011en_HK
dc.identifier.citationPublications Of The Astronomical Society Of Japan, 2011, v. 63 n. 1, p. 309-315en_HK
dc.identifier.issn0004-6264en_HK
dc.identifier.urihttp://hdl.handle.net/10722/135369-
dc.description.abstractWe report on the time variation of SiO maser emission from the symbiotic stellar system V407 Cygni after the classical nova outburst on 2010 March 10. Although both the SiO J = 1-0 v = 1 and 2 lines at 43.122 and 42.821GHz were found previously in the envelope of amira in the binary system, only weak emission of the J = 1-0 v = 2 line has continuously been detectable after the nova outburst. The line profile exhibited a dramatic change several weeks after the burst; the component on the higher-velocity side of the systemic velocity disappeared two weeks after the burst, and a new persistent component appeared on the lower-velocity side later. These observations indicate that the SiO emitting regions were wiped out on a time scale of two weeks by the nova shock, but a part of the masing region was quickly replenished by cool molecular gases expelled by the mira pulsation. © 2011. Astronomical Society of Japan.en_HK
dc.languageengen_US
dc.publisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/en_HK
dc.relation.ispartofPublications of the Astronomical Society of Japanen_HK
dc.subjectAGB and post-AGB-starsen_HK
dc.subjectCircumstellar matter-starsen_HK
dc.subjectNovae, cataclysmic variables-radio linesen_HK
dc.subjectStarsen_HK
dc.titleSiO maser spectra of V407 cygni after the 2010 march nova outbursten_HK
dc.typeArticleen_HK
dc.identifier.emailNakashima, JI: junichi@hku.hken_HK
dc.identifier.authorityNakashima, JI=rp00764en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.scopuseid_2-s2.0-79952159941en_HK
dc.identifier.hkuros186856en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-79952159941&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume63en_HK
dc.identifier.issue1en_HK
dc.identifier.spage309en_HK
dc.identifier.epage315en_HK
dc.publisher.placeJapanen_HK
dc.identifier.scopusauthoridDeguchi, S=7006314159en_HK
dc.identifier.scopusauthoridKoike, K=26028631700en_HK
dc.identifier.scopusauthoridKuno, N=7005279621en_HK
dc.identifier.scopusauthoridMatsunaga, N=7201674206en_HK
dc.identifier.scopusauthoridNakashima, JI=35485342300en_HK
dc.identifier.scopusauthoridTakahashi, S=7407712968en_HK

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