Stratification and isotope separation in CP stars ★
dc.contributor.author | Cowley, C. R. | en_US |
dc.contributor.author | Hubrig, S. | en_US |
dc.contributor.author | González, J. F. | en_US |
dc.date.accessioned | 2010-06-01T21:31:32Z | |
dc.date.available | 2010-06-01T21:31:32Z | |
dc.date.issued | 2009-06-11 | en_US |
dc.identifier.citation | Cowley, C. R.; Hubrig, S.; GonzÁlez, J. F. (2009). "Stratification and isotope separation in CP stars ★ ." Monthly Notices of the Royal Astronomical Society 396(1): 485-499. <http://hdl.handle.net/2027.42/74580> | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.issn | 1365-2966 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/74580 | |
dc.description.abstract | We investigate the elemental and isotopic stratification in the atmospheres of selected chemically peculiar (CP) stars of the upper main sequence. Reconfiguration of the UV-Visual Echelle Spectrograph in 2004 has made it possible to examine all three lines of the Ca ii infrared (IR) triplet. Much of the material analysed was obtained in 2008. We support the claim of Ryabchikova, Kochukhov & Bagnulo (RKB) that the calcium isotopes have distinct stratification profiles for the stars 10 Aql, HR 1217 and HD 122970, with the heavy isotope concentrated towards the higher layers. Better observations are needed to learn the extent to which 40 Ca dominates in the deepest layers of all or most CP stars that show the presence of 48 Ca. There is little evidence for 40 Ca in the spectra of some HgMn stars, and the infrared (IR) triplet in the magnetic star HD 101065 is well fit by pure 48 Ca. In HR 5623 (HD 133792) and HD 217522, it is likely that the heavy isotope dominates, though models are possible where this is not the case. While elemental stratification is surely needed in many cases, we point out the importance of including adjustments in the assumed T eff and log ( g ) values, in attempts to model stratification. We recommend emphasis on profiles of the strongest lines, where the influence of stratification is most evident. Isotopic mixtures, involving the four stable calcium nuclides with masses between 40 and 48 are plausible, but are not emphasized. | en_US |
dc.format.extent | 1104008 bytes | |
dc.format.extent | 3109 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Blackwell Publishing Ltd | en_US |
dc.rights | Journal compilation © 2009 RAS | en_US |
dc.subject.other | Stars: Chemically Peculiar | en_US |
dc.subject.other | Stars: Individual: HD 101065 | en_US |
dc.subject.other | Stars: Individual: HD 122970 | en_US |
dc.subject.other | Stars: Individual: HR 5623 | en_US |
dc.subject.other | Stars: Individual: 10 Aql | en_US |
dc.subject.other | Stars: Individual: HD 217522 | en_US |
dc.title | Stratification and isotope separation in CP stars ★ | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Astronomy | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA | en_US |
dc.contributor.affiliationother | European Southern Observatory, Casilla 19001, Santiago 19, Chile | en_US |
dc.contributor.affiliationother | Complejo AstronÓmico El Leoncito, Casilla 467, 5400 San Juan, Argentina | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/74580/1/j.1365-2966.2009.14723.x.pdf | |
dc.identifier.doi | 10.1111/j.1365-2966.2009.14723.x | en_US |
dc.identifier.source | Monthly Notices of the Royal Astronomical Society | en_US |
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