Are C-60 Molecules Detectable In Circumstellar Shells Of R Coronae Borealis Stars?

dc.contributor.utaustinauthorRao, N. Kameswaraen_US
dc.contributor.utaustinauthorLambert, David L.en_US
dc.creatorGarcia-Hernandez, D. Anibalen_US
dc.creatorRao, N. Kameswaraen_US
dc.creatorLambert, David L.en_US
dc.date.accessioned2016-04-28T22:21:58Z
dc.date.available2016-04-28T22:21:58Z
dc.date.issued2011-03en
dc.description.abstractThe hydrogen-poor, helium-rich, and carbon-rich character of the gas around R Coronae Borealis (RCB) stars has been suggested to be a site for formation of C-60 molecules. This suggestion is not supported by observations reported here showing that infrared transitions of C-60 are not seen in a large sample of RCB stars observed with the Infrared Spectrograph on the Spitzer Space Telescope. The infrared C-60 transitions are seen, however, in emission and blended with polycyclic aromatic hydrocarbon (PAH) features in spectra of DY Cen and possibly also of V854 Cen, the two least hydrogen-deficient (hydrogen deficiency of only similar to 10-100) RCB stars. The speculation is offered that C-60 (and the PAHs) in the moderately H-deficient circumstellar envelopes may be formed by the decomposition of hydrogenated amorphous carbon but fullerene formation is inefficient in the highly H-deficient environments of most RCBs.en_US
dc.description.departmentMcDonald Observatoryen_US
dc.description.sponsorshipNASA 1407, GO 50212en_US
dc.description.sponsorshipSpanish Ministry of Science and Innovation (MICINN) AYA-2007-64748en_US
dc.description.sponsorshipRobert A. Welch Foundation of Houston, Texas F-634en_US
dc.identifierdoi:10.15781/T27834
dc.identifier.Filename2011_03_c60molecules.pdfen_US
dc.identifier.citationGarc�a-Hern�ndez, D. A., N. Kameswara Rao, and D. L. Lambert. "Are C60 molecules detectable in circumstellar shells of R Coronae Borealis stars?." The Astrophysical Journal, Vol., 729, No. 2 (Mar., 2011): 126.en_US
dc.identifier.doi10.1088/0004-637x/729/2/126en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35204
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjectastrochemistryen_US
dc.subjectcircumstellar matteren_US
dc.subjectinfrared: starsen_US
dc.subjectstars: chemicallyen_US
dc.subjectpeculiaren_US
dc.subjectwhite dwarfsen_US
dc.subjectpolycyclic aromatic-hydrocarbonsen_US
dc.subjecthydrogenated amorphous-carbonen_US
dc.subjectinfrared-emission spectraen_US
dc.subjectplanetary-nebulaeen_US
dc.subjectdust formationen_US
dc.subjectfeaturesen_US
dc.subjectbuckminsterfullereneen_US
dc.subjectfullerenesen_US
dc.subjectabundancesen_US
dc.subjectsearchen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleAre C-60 Molecules Detectable In Circumstellar Shells Of R Coronae Borealis Stars?en_US
dc.typeArticleen_US

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