File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Probing the mass-loss history of the yellow hypergiant irc+10420

TitleProbing the mass-loss history of the yellow hypergiant irc+10420
Authors
KeywordsCircumstellar matter
ISM: molecules
Stars: AGB and post-AGB
Stars: individual (IRC+10420)
Stars: mass loss
Issue Date2009
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2009, v. 697 n. 1, p. 409-419 How to Cite?
AbstractWe have used the submillimeter array to image the molecular envelope around the yellow hypergiant IRC+10420. Our observations reveal a large and clumpy expanding envelope around the star. The molecular envelope shows a clear asymmetry in 12CO J = 2-1 emission in the southwest direction. The elongation of the envelope is found even more pronounced in the emission of 13CO J = 2-1 and SO J K = 6 5-5 4. A small positional velocity gradient across velocity channels is seen in these lines, suggesting the presence of a weak bipolar outflow in the envelope of IRC+10420. In the higher resolution 12CO J = 2-1 map, we find that the envelope has two components: (1) an inner shell (shell I) located between radius of about 1″ and 2″; (2) an outer shell (shell II) located between 3″ and 6″ in radius. These shells represent two previous mass-loss episodes from IRC+10420. We attempt to derive in self-consistent manner the physical conditions inside the envelope by modeling the dust properties, and the heating and cooling of molecular gas. We estimate a mass-loss rate of 9 × 10 -4 M⊙ yr -1 for shellI and 7 × 10 -4 M⊙ yr -1 for shell II. The gas temperature is found to be unusually high in IRC+10420 in comparison with other oxygen-rich envelopes. The elevated gas temperature is mainly due to higher heating rate, which results from the large luminosity of the central star. We also derive an isotopic ratio 12C/ 13C = 6. © 2009. The American Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/59653
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorTrung, DVen_HK
dc.contributor.authorMuller, Sen_HK
dc.contributor.authorLim, Jen_HK
dc.contributor.authorKwok, Sen_HK
dc.contributor.authorMuthu, Cen_HK
dc.date.accessioned2010-05-31T03:54:33Z-
dc.date.available2010-05-31T03:54:33Z-
dc.date.issued2009en_HK
dc.identifier.citationAstrophysical Journal Letters, 2009, v. 697 n. 1, p. 409-419en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/59653-
dc.description.abstractWe have used the submillimeter array to image the molecular envelope around the yellow hypergiant IRC+10420. Our observations reveal a large and clumpy expanding envelope around the star. The molecular envelope shows a clear asymmetry in 12CO J = 2-1 emission in the southwest direction. The elongation of the envelope is found even more pronounced in the emission of 13CO J = 2-1 and SO J K = 6 5-5 4. A small positional velocity gradient across velocity channels is seen in these lines, suggesting the presence of a weak bipolar outflow in the envelope of IRC+10420. In the higher resolution 12CO J = 2-1 map, we find that the envelope has two components: (1) an inner shell (shell I) located between radius of about 1″ and 2″; (2) an outer shell (shell II) located between 3″ and 6″ in radius. These shells represent two previous mass-loss episodes from IRC+10420. We attempt to derive in self-consistent manner the physical conditions inside the envelope by modeling the dust properties, and the heating and cooling of molecular gas. We estimate a mass-loss rate of 9 × 10 -4 M⊙ yr -1 for shellI and 7 × 10 -4 M⊙ yr -1 for shell II. The gas temperature is found to be unusually high in IRC+10420 in comparison with other oxygen-rich envelopes. The elevated gas temperature is mainly due to higher heating rate, which results from the large luminosity of the central star. We also derive an isotopic ratio 12C/ 13C = 6. © 2009. The American Astronomical Society.en_HK
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.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectCircumstellar matteren_HK
dc.subjectISM: moleculesen_HK
dc.subjectStars: AGB and post-AGBen_HK
dc.subjectStars: individual (IRC+10420)en_HK
dc.subjectStars: mass lossen_HK
dc.titleProbing the mass-loss history of the yellow hypergiant irc+10420en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=697&spage=409&epage=419&date=2009&atitle=Probing+the+Mass-Loss+History+of+the+Yellow+Hypergiant+IRC+10420en_HK
dc.identifier.emailLim, J: jjlim@hku.hken_HK
dc.identifier.emailKwok, S: deannote@hku.hken_HK
dc.identifier.authorityLim, J=rp00745en_HK
dc.identifier.authorityKwok, S=rp00716en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/697/1/409en_HK
dc.identifier.scopuseid_2-s2.0-66649094528en_HK
dc.identifier.hkuros156357en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-66649094528&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume697en_HK
dc.identifier.issue1en_HK
dc.identifier.spage409en_HK
dc.identifier.epage419en_HK
dc.identifier.isiWOS:000265764000034-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridTrung, DV=6701469660en_HK
dc.identifier.scopusauthoridMuller, S=15071043100en_HK
dc.identifier.scopusauthoridLim, J=7403453870en_HK
dc.identifier.scopusauthoridKwok, S=22980498300en_HK
dc.identifier.scopusauthoridMuthu, C=6602324244en_HK

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats