THE CLOSE BINARY V757 CENTAURI
The W UMa system V757 Cen has been observed photoelectrically in the UBV system at Bosque Alegre and at El Leoncito Observatories. Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classica...
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| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 1982-02, Vol.94 (557), p.189-194 |
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| container_issue | 557 |
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| container_title | Publications of the Astronomical Society of the Pacific |
| container_volume | 94 |
| creator | CERRUTI, MIGUEL A. SISTERÓ, ROBERTO F. |
| description | The W UMa system V757 Cen has been observed photoelectrically in the UBV system at Bosque Alegre and at El Leoncito Observatories. Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classical solution for partial eclipses, determined with complementary spectroscopic data, suggests the system to be a contact W UMa star consisting of a larger component of spectral type G1-G2 and an F9-G0 companion. |
| doi_str_mv | 10.1086/130962 |
| format | Article |
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Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classical solution for partial eclipses, determined with complementary spectroscopic data, suggests the system to be a contact W UMa star consisting of a larger component of spectral type G1-G2 and an F9-G0 companion.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>DOI: 10.1086/130962</identifier><language>eng</language><publisher>The Astronomical Society of the Pacific</publisher><subject>Binary systems ; Comparison stars ; Eclipses ; Ephemerides ; Light curves ; Mathematical minima ; Observatories ; Spectroscopy ; Stellar classification ; Variable stars</subject><ispartof>Publications of the Astronomical Society of the Pacific, 1982-02, Vol.94 (557), p.189-194</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c207t-89a907f3df3643d4ff23fee07fe89db540c17968418b211c7decfbf46df936bc3</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://www.jstor.org/stable/pdf/40677934$$EPDF$$P50$$Gjstor$$H</linktopdf><linktohtml>$$Uhttps://www.jstor.org/stable/40677934$$EHTML$$P50$$Gjstor$$H</linktohtml><link.rule.ids>314,776,780,799,27901,27902,57992,58225</link.rule.ids></links><search><creatorcontrib>CERRUTI, MIGUEL A.</creatorcontrib><creatorcontrib>SISTERÓ, ROBERTO F.</creatorcontrib><title>THE CLOSE BINARY V757 CENTAURI</title><title>Publications of the Astronomical Society of the Pacific</title><description>The W UMa system V757 Cen has been observed photoelectrically in the UBV system at Bosque Alegre and at El Leoncito Observatories. Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classical solution for partial eclipses, determined with complementary spectroscopic data, suggests the system to be a contact W UMa star consisting of a larger component of spectral type G1-G2 and an F9-G0 companion.</description><subject>Binary systems</subject><subject>Comparison stars</subject><subject>Eclipses</subject><subject>Ephemerides</subject><subject>Light curves</subject><subject>Mathematical minima</subject><subject>Observatories</subject><subject>Spectroscopy</subject><subject>Stellar classification</subject><subject>Variable stars</subject><issn>0004-6280</issn><issn>1538-3873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1982</creationdate><recordtype>article</recordtype><recordid>eNo9j81KxDAURoMoWEd9A6Urd9F7c9P8LGupTqHMwNgRXJU2TcBBGUlm49s7UnH1wcfhwGHsGuEewagHJLBKnLAMCzKcjKZTlgGA5EoYOGcXKe0AEA1Cxm67ZZ1X7fqlzh-bVbl5y191ofOqXnXldtNcsrMwfCR_9bcLtn2qu2rJ2_VzU5UtdwL0gRs7WNCBpkBK0iRDEBS8P17e2GksJDjUVhmJZhSITk_ehTFINQVLanS0YHez18V9StGH_iu-fw7xu0fof6v6ueoI3szgLh328Z-SoLS2JOkHcexDgg</recordid><startdate>19820201</startdate><enddate>19820201</enddate><creator>CERRUTI, MIGUEL A.</creator><creator>SISTERÓ, ROBERTO F.</creator><general>The Astronomical Society of the Pacific</general><scope>AAYXX</scope><scope>CITATION</scope></search><sort><creationdate>19820201</creationdate><title>THE CLOSE BINARY V757 CENTAURI</title><author>CERRUTI, MIGUEL A. ; SISTERÓ, ROBERTO F.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c207t-89a907f3df3643d4ff23fee07fe89db540c17968418b211c7decfbf46df936bc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1982</creationdate><topic>Binary systems</topic><topic>Comparison stars</topic><topic>Eclipses</topic><topic>Ephemerides</topic><topic>Light curves</topic><topic>Mathematical minima</topic><topic>Observatories</topic><topic>Spectroscopy</topic><topic>Stellar classification</topic><topic>Variable stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>CERRUTI, MIGUEL A.</creatorcontrib><creatorcontrib>SISTERÓ, ROBERTO F.</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>CERRUTI, MIGUEL A.</au><au>SISTERÓ, ROBERTO F.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>THE CLOSE BINARY V757 CENTAURI</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>1982-02-01</date><risdate>1982</risdate><volume>94</volume><issue>557</issue><spage>189</spage><epage>194</epage><pages>189-194</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><abstract>The W UMa system V757 Cen has been observed photoelectrically in the UBV system at Bosque Alegre and at El Leoncito Observatories. Full light curves were constructed from 1135 V, 1104 B, and 1104 U individual observations. An improved ephemeris based on about 12,000 cycles is given. A first classical solution for partial eclipses, determined with complementary spectroscopic data, suggests the system to be a contact W UMa star consisting of a larger component of spectral type G1-G2 and an F9-G0 companion.</abstract><pub>The Astronomical Society of the Pacific</pub><doi>10.1086/130962</doi><tpages>6</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6280 |
| ispartof | Publications of the Astronomical Society of the Pacific, 1982-02, Vol.94 (557), p.189-194 |
| issn | 0004-6280 1538-3873 |
| language | eng |
| recordid | cdi_crossref_primary_10_1086_130962 |
| source | Jstor Complete Legacy; Institute of Physics Journals; Alma/SFX Local Collection; EZB Electronic Journals Library |
| subjects | Binary systems Comparison stars Eclipses Ephemerides Light curves Mathematical minima Observatories Spectroscopy Stellar classification Variable stars |
| title | THE CLOSE BINARY V757 CENTAURI |
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