Orbital parameters and evolutionary status of the highly peculiar binary system HD 66051
Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent di...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2018-07, Vol.615, p.A36 |
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| creator | Paunzen, E. Fedurco, M. Hełminiak, K. G. Pintado, O. I. Hambsch, F.-J. Hümmerich, S. Niemczura, E. Bernhard, K. Konacki, M. Hubrig, S. Fraga, L. |
| description | Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent diffusion models. Aims. We aim at deriving astrophysical parameters, information on age, and an orbital solution of the system. Methods. We analysed radial velocity and photometric data using two different methods to determine astrophysical parameters and the orbit of the system. Appropriate isochrones were used to derive the age of the system. Results. The orbital solution and the estimates from the isochrones are in excellent agreement with the estimates from a prior spectroscopic study. The system is very close to the zero-age main sequence and younger than 120 Myr. Conclusions. HD 66051 is a most important spectroscopic binary system that can be used to test the predictions of the diffusion theory explaining the peculiar surface abundances of CP3 stars. |
| doi_str_mv | 10.1051/0004-6361/201732257 |
| format | Article |
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G. ; Pintado, O. I. ; Hambsch, F.-J. ; Hümmerich, S. ; Niemczura, E. ; Bernhard, K. ; Konacki, M. ; Hubrig, S. ; Fraga, L.</creator><creatorcontrib>Paunzen, E. ; Fedurco, M. ; Hełminiak, K. G. ; Pintado, O. I. ; Hambsch, F.-J. ; Hümmerich, S. ; Niemczura, E. ; Bernhard, K. ; Konacki, M. ; Hubrig, S. ; Fraga, L.</creatorcontrib><description>Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent diffusion models. Aims. We aim at deriving astrophysical parameters, information on age, and an orbital solution of the system. Methods. We analysed radial velocity and photometric data using two different methods to determine astrophysical parameters and the orbit of the system. Appropriate isochrones were used to derive the age of the system. Results. The orbital solution and the estimates from the isochrones are in excellent agreement with the estimates from a prior spectroscopic study. The system is very close to the zero-age main sequence and younger than 120 Myr. Conclusions. HD 66051 is a most important spectroscopic binary system that can be used to test the predictions of the diffusion theory explaining the peculiar surface abundances of CP3 stars.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201732257</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Age ; Astronomical models ; binaries: eclipsing ; Binary stars ; Binary system ; Diffusion theory ; Organic chemistry ; Parameters ; Photometry ; Radial velocity ; stars: chemically peculiar ; stars: individual: HD 66051 ; Stellar system evolution ; techniques: photometric ; Time dependence</subject><ispartof>Astronomy and astrophysics (Berlin), 2018-07, Vol.615, p.A36</ispartof><rights>Copyright EDP Sciences Jul 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c360t-a0c2c40a36bf7bc3c3de5e1358147595ee4dde0719d076ce85f37578b99ca9c53</citedby><cites>FETCH-LOGICAL-c360t-a0c2c40a36bf7bc3c3de5e1358147595ee4dde0719d076ce85f37578b99ca9c53</cites><orcidid>0000-0002-3304-5200</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,3713,27903,27904</link.rule.ids></links><search><creatorcontrib>Paunzen, E.</creatorcontrib><creatorcontrib>Fedurco, M.</creatorcontrib><creatorcontrib>Hełminiak, K. G.</creatorcontrib><creatorcontrib>Pintado, O. I.</creatorcontrib><creatorcontrib>Hambsch, F.-J.</creatorcontrib><creatorcontrib>Hümmerich, S.</creatorcontrib><creatorcontrib>Niemczura, E.</creatorcontrib><creatorcontrib>Bernhard, K.</creatorcontrib><creatorcontrib>Konacki, M.</creatorcontrib><creatorcontrib>Hubrig, S.</creatorcontrib><creatorcontrib>Fraga, L.</creatorcontrib><title>Orbital parameters and evolutionary status of the highly peculiar binary system HD 66051</title><title>Astronomy and astrophysics (Berlin)</title><description>Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent diffusion models. Aims. We aim at deriving astrophysical parameters, information on age, and an orbital solution of the system. Methods. We analysed radial velocity and photometric data using two different methods to determine astrophysical parameters and the orbit of the system. Appropriate isochrones were used to derive the age of the system. Results. The orbital solution and the estimates from the isochrones are in excellent agreement with the estimates from a prior spectroscopic study. The system is very close to the zero-age main sequence and younger than 120 Myr. Conclusions. HD 66051 is a most important spectroscopic binary system that can be used to test the predictions of the diffusion theory explaining the peculiar surface abundances of CP3 stars.</description><subject>Age</subject><subject>Astronomical models</subject><subject>binaries: eclipsing</subject><subject>Binary stars</subject><subject>Binary system</subject><subject>Diffusion theory</subject><subject>Organic chemistry</subject><subject>Parameters</subject><subject>Photometry</subject><subject>Radial velocity</subject><subject>stars: chemically peculiar</subject><subject>stars: individual: HD 66051</subject><subject>Stellar system evolution</subject><subject>techniques: photometric</subject><subject>Time dependence</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNo9kF1PwyAUhonRxDn9Bd6QeF13gALtpZkfM1ncxdR5RyilrrNbK1Dj_r0sNbs6IXleznsehK4J3BLgZAIAaSKYIBMKRDJKuTxBI5IymoBMxSkaHYlzdOH9Jj4pydgIfSxcUQfd4E47vbXBOo_1rsT2p236ULc77fbYBx16j9sKh7XF6_pz3exxZ03f1Nrhoh6gvQ92i2f3WIjY6RKdVbrx9up_jtHb48PrdJbMF0_P07t5YpiAkGgw1KSgmSgqWRhmWGm5JYxnJJU859amZWlBkrwEKYzNeMUkl1mR50bnhrMxuhn-7Vz73Vsf1Kbt3S6uVBTyDAjJCI0UGyjjWu-drVTn6m2srQiog0J1EKQOgtRRYUwlQ6qOp_0eI9p9KSFjDZXBSonlC1--50Kt2B9fOnIN</recordid><startdate>20180701</startdate><enddate>20180701</enddate><creator>Paunzen, E.</creator><creator>Fedurco, M.</creator><creator>Hełminiak, K. 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I. ; Hambsch, F.-J. ; Hümmerich, S. ; Niemczura, E. ; Bernhard, K. ; Konacki, M. ; Hubrig, S. ; Fraga, L.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c360t-a0c2c40a36bf7bc3c3de5e1358147595ee4dde0719d076ce85f37578b99ca9c53</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Age</topic><topic>Astronomical models</topic><topic>binaries: eclipsing</topic><topic>Binary stars</topic><topic>Binary system</topic><topic>Diffusion theory</topic><topic>Organic chemistry</topic><topic>Parameters</topic><topic>Photometry</topic><topic>Radial velocity</topic><topic>stars: chemically peculiar</topic><topic>stars: individual: HD 66051</topic><topic>Stellar system evolution</topic><topic>techniques: photometric</topic><topic>Time dependence</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Paunzen, E.</creatorcontrib><creatorcontrib>Fedurco, M.</creatorcontrib><creatorcontrib>Hełminiak, K. G.</creatorcontrib><creatorcontrib>Pintado, O. I.</creatorcontrib><creatorcontrib>Hambsch, F.-J.</creatorcontrib><creatorcontrib>Hümmerich, S.</creatorcontrib><creatorcontrib>Niemczura, E.</creatorcontrib><creatorcontrib>Bernhard, K.</creatorcontrib><creatorcontrib>Konacki, M.</creatorcontrib><creatorcontrib>Hubrig, S.</creatorcontrib><creatorcontrib>Fraga, L.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Paunzen, E.</au><au>Fedurco, M.</au><au>Hełminiak, K. G.</au><au>Pintado, O. I.</au><au>Hambsch, F.-J.</au><au>Hümmerich, S.</au><au>Niemczura, E.</au><au>Bernhard, K.</au><au>Konacki, M.</au><au>Hubrig, S.</au><au>Fraga, L.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Orbital parameters and evolutionary status of the highly peculiar binary system HD 66051</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2018-07-01</date><risdate>2018</risdate><volume>615</volume><spage>A36</spage><pages>A36-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent diffusion models. Aims. We aim at deriving astrophysical parameters, information on age, and an orbital solution of the system. Methods. We analysed radial velocity and photometric data using two different methods to determine astrophysical parameters and the orbit of the system. Appropriate isochrones were used to derive the age of the system. Results. The orbital solution and the estimates from the isochrones are in excellent agreement with the estimates from a prior spectroscopic study. The system is very close to the zero-age main sequence and younger than 120 Myr. Conclusions. HD 66051 is a most important spectroscopic binary system that can be used to test the predictions of the diffusion theory explaining the peculiar surface abundances of CP3 stars.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201732257</doi><orcidid>https://orcid.org/0000-0002-3304-5200</orcidid><oa>free_for_read</oa></addata></record> |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; EDP Sciences |
| subjects | Age Astronomical models binaries: eclipsing Binary stars Binary system Diffusion theory Organic chemistry Parameters Photometry Radial velocity stars: chemically peculiar stars: individual: HD 66051 Stellar system evolution techniques: photometric Time dependence |
| title | Orbital parameters and evolutionary status of the highly peculiar binary system HD 66051 |
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