The R Stars: Carbon Stars of a Different Kind

After ~ 16 years of radial-velocity observations of a sample of 22 R-type carbon stars, no evidence for binary motion has been detected in any of them. This is surprising considering that approximately 20% of normal late-type giants are spectroscopie binaries, and the fraction is close to 100% in ba...

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Veröffentlicht in:	Publications of the Astronomical Society of the Pacific 1997-03, Vol.109 (733), p.256-263
1. Verfasser:	McClure, Robert D.
Format:	Artikel
Sprache:	eng
Schlagworte:	Barium stars Carbon Carbon stars CH stars K giants R stars Radial velocity S process Stars Stellar spectra
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creator	McClure, Robert D.
description	After ~ 16 years of radial-velocity observations of a sample of 22 R-type carbon stars, no evidence for binary motion has been detected in any of them. This is surprising considering that approximately 20% of normal late-type giants are spectroscopie binaries, and the fraction is close to 100% in barium, CH, and subgiant/dwarf CH and barium stars. It is suggested, therefore, that a process that has caused the mixing of carbon to the surface of these stars cannot act in a wide binary system. Possibly, the R stars were once all binaries, but with separations that would not allow them to evolve completely up the giant and asymptotic giant branches without coalescing. This coalescence may be the agent which causes carbon produced in the helium-core flash to be mixed outward to a region where convection zones can bring it to the surface of the star.
doi_str_mv	10.1086/133882
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This is surprising considering that approximately 20% of normal late-type giants are spectroscopie binaries, and the fraction is close to 100% in barium, CH, and subgiant/dwarf CH and barium stars. It is suggested, therefore, that a process that has caused the mixing of carbon to the surface of these stars cannot act in a wide binary system. Possibly, the R stars were once all binaries, but with separations that would not allow them to evolve completely up the giant and asymptotic giant branches without coalescing. This coalescence may be the agent which causes carbon produced in the helium-core flash to be mixed outward to a region where convection zones can bring it to the surface of the star.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>DOI: 10.1086/133882</identifier><language>eng</language><publisher>American Institute of Physics</publisher><subject>Barium stars ; Carbon ; Carbon stars ; CH stars ; K giants ; R stars ; Radial velocity ; S process ; Stars ; Stellar spectra</subject><ispartof>Publications of the Astronomical Society of the Pacific, 1997-03, Vol.109 (733), p.256-263</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c275t-b5523e77006e98eca20ad7e0aefb37a9c7248efd547b812e4513f16a014f49c43</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://www.jstor.org/stable/pdf/40680894$$EPDF$$P50$$Gjstor$$H</linktopdf><linktohtml>$$Uhttps://www.jstor.org/stable/40680894$$EHTML$$P50$$Gjstor$$H</linktohtml><link.rule.ids>314,780,784,803,27924,27925,58017,58250</link.rule.ids></links><search><creatorcontrib>McClure, Robert D.</creatorcontrib><title>The R Stars: Carbon Stars of a Different Kind</title><title>Publications of the Astronomical Society of the Pacific</title><description>After ~ 16 years of radial-velocity observations of a sample of 22 R-type carbon stars, no evidence for binary motion has been detected in any of them. This is surprising considering that approximately 20% of normal late-type giants are spectroscopie binaries, and the fraction is close to 100% in barium, CH, and subgiant/dwarf CH and barium stars. It is suggested, therefore, that a process that has caused the mixing of carbon to the surface of these stars cannot act in a wide binary system. Possibly, the R stars were once all binaries, but with separations that would not allow them to evolve completely up the giant and asymptotic giant branches without coalescing. This coalescence may be the agent which causes carbon produced in the helium-core flash to be mixed outward to a region where convection zones can bring it to the surface of the star.</description><subject>Barium stars</subject><subject>Carbon</subject><subject>Carbon stars</subject><subject>CH stars</subject><subject>K giants</subject><subject>R stars</subject><subject>Radial velocity</subject><subject>S process</subject><subject>Stars</subject><subject>Stellar spectra</subject><issn>0004-6280</issn><issn>1538-3873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1997</creationdate><recordtype>article</recordtype><recordid>eNo9j0tLxDAURoMoWEf9B0JW7qL35tHcupM6PnBA0HFd0vYGO2grSTf-e5WKq48PDgeOEKcIFwhUXqIxRHpPFOgMKUPe7IsCAKwqNcGhOMp5B4BICIVQ2zeWz_JlDilfyTqkdhqXJ6cog7wZYuTE4ywfh7E_FgcxvGc--duVeL1db-t7tXm6e6ivN6rT3s2qdU4b9h6g5Iq4CxpC7xkCx9b4UHVeW-LYO-tbQs3WoYlYBkAbbdVZsxLni7dLU86JY_OZho-QvhqE5jeyWSJ_wLMF3OV5Sv-UhZKAKmu-AerzSmk</recordid><startdate>19970301</startdate><enddate>19970301</enddate><creator>McClure, Robert D.</creator><general>American Institute of Physics</general><scope>AAYXX</scope><scope>CITATION</scope></search><sort><creationdate>19970301</creationdate><title>The R Stars: Carbon Stars of a Different Kind</title><author>McClure, Robert D.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c275t-b5523e77006e98eca20ad7e0aefb37a9c7248efd547b812e4513f16a014f49c43</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1997</creationdate><topic>Barium stars</topic><topic>Carbon</topic><topic>Carbon stars</topic><topic>CH stars</topic><topic>K giants</topic><topic>R stars</topic><topic>Radial velocity</topic><topic>S process</topic><topic>Stars</topic><topic>Stellar spectra</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>McClure, Robert D.</creatorcontrib><collection>CrossRef</collection><jtitle>Publications of the Astronomical Society of the Pacific</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>McClure, Robert D.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The R Stars: Carbon Stars of a Different Kind</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>1997-03-01</date><risdate>1997</risdate><volume>109</volume><issue>733</issue><spage>256</spage><epage>263</epage><pages>256-263</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><abstract>After ~ 16 years of radial-velocity observations of a sample of 22 R-type carbon stars, no evidence for binary motion has been detected in any of them. This is surprising considering that approximately 20% of normal late-type giants are spectroscopie binaries, and the fraction is close to 100% in barium, CH, and subgiant/dwarf CH and barium stars. It is suggested, therefore, that a process that has caused the mixing of carbon to the surface of these stars cannot act in a wide binary system. Possibly, the R stars were once all binaries, but with separations that would not allow them to evolve completely up the giant and asymptotic giant branches without coalescing. This coalescence may be the agent which causes carbon produced in the helium-core flash to be mixed outward to a region where convection zones can bring it to the surface of the star.</abstract><pub>American Institute of Physics</pub><doi>10.1086/133882</doi><tpages>8</tpages><oa>free_for_read</oa></addata></record>
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source	IOP Publishing Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; JSTOR Archive Collection A-Z Listing; Institute of Physics (IOP) Journals - HEAL-Link; Alma/SFX Local Collection
subjects	Barium stars Carbon Carbon stars CH stars K giants R stars Radial velocity S process Stars Stellar spectra
title	The R Stars: Carbon Stars of a Different Kind
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