THE BINARY SYSTEM Σ2173
New high-dispersion spectroscopic observations of the visual binary Σ2173 are combined with earlier ones obtained during passage through the opposite node, and with the available visual and interferometric observations, to determine the orbital elements completely. We find P =46y.43, T=1962.52, Ω =...
Gespeichert in:
| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 1991-03, Vol.103 (661), p.294-299 |
|---|---|
| Hauptverfasser: | , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | 299 |
|---|---|
| container_issue | 661 |
| container_start_page | 294 |
| container_title | Publications of the Astronomical Society of the Pacific |
| container_volume | 103 |
| creator | BATTEN, A. H. FLETCHER, J. M. HILL, G. LU, WENXIAN MORBEY, C. L. |
| description | New high-dispersion spectroscopic observations of the visual binary Σ2173 are combined with earlier ones obtained during passage through the opposite node, and with the available visual and interferometric observations, to determine the orbital elements completely. We find P =46y.43, T=1962.52, Ω = 152°.7, ω=98°.7, ω=147°.6, α" = 0°.97, V₀ = -76.98 km s⁻¹ and K₂ = 4.84 km s⁻¹. The parallax derived is O". O59, somewhat larger than the best trigonometrical value of O". O5, which leads to masses and luminosities for the components in good agreement with the spectral types and luminosity classes but which are problematical from the point of view of theoretical studies of stellar evolution. The two stars are very similar: We can distinguish no difference in spectral type and find Δm to be approximately 0ṃ1. The brighter star appears to be the less massive. |
| format | Article |
| fullrecord | <record><control><sourceid>jstor_pasca</sourceid><recordid>TN_cdi_pascalfrancis_primary_19637383</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><jstor_id>40679684</jstor_id><sourcerecordid>40679684</sourcerecordid><originalsourceid>FETCH-LOGICAL-j523-8c658afb9310a8a58e60655e66849d6009904d712028507967ddf8afbcf96ea93</originalsourceid><addsrcrecordid>eNo9jLFKA0EURQdRcI32NsI2lgNv5s28eVPGsJpANJBskyo8d3cgS9SwY-P3-D9-kwkRq1vcc86ZKoxH1sgBz1UBAE6TZbhUVzn3AMawgULd1tOqfJi9jJfrcrVe1dVz-fNtTcBrdZFkl7ubvx2p-rGqJ1M9XzzNJuO57r1FzQ15lvQa0YCweO4IyPuOiF1sCSBGcG0wFix7CJFC26aj0KRInUQcqftTdi-5kV0a5L3Z5s1-2L7J8LUxkTAg44G7O3F9_vwY_n8HdIiyw1_OXj6r</addsrcrecordid><sourcetype>Index Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>THE BINARY SYSTEM Σ2173</title><source>IOP Publishing Journals</source><source>Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals</source><source>Jstor Complete Legacy</source><source>Institute of Physics (IOP) Journals - HEAL-Link</source><source>Alma/SFX Local Collection</source><creator>BATTEN, A. H. ; FLETCHER, J. M. ; HILL, G. ; LU, WENXIAN ; MORBEY, C. L.</creator><creatorcontrib>BATTEN, A. H. ; FLETCHER, J. M. ; HILL, G. ; LU, WENXIAN ; MORBEY, C. L.</creatorcontrib><description>New high-dispersion spectroscopic observations of the visual binary Σ2173 are combined with earlier ones obtained during passage through the opposite node, and with the available visual and interferometric observations, to determine the orbital elements completely. We find P =46y.43, T=1962.52, Ω = 152°.7, ω=98°.7, ω=147°.6, α" = 0°.97, V₀ = -76.98 km s⁻¹ and K₂ = 4.84 km s⁻¹. The parallax derived is O". O59, somewhat larger than the best trigonometrical value of O". O5, which leads to masses and luminosities for the components in good agreement with the spectral types and luminosity classes but which are problematical from the point of view of theoretical studies of stellar evolution. The two stars are very similar: We can distinguish no difference in spectral type and find Δm to be approximately 0ṃ1. The brighter star appears to be the less massive.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>CODEN: PASPAU</identifier><language>eng</language><publisher>Chicago, IL: The Astronomical Society of the Pacific</publisher><subject>Astronomy ; Binary and multiple stars ; Earth, ocean, space ; Exact sciences and technology ; Multiple stars ; Observational astronomy ; Orbital elements ; Orbits ; Parallax ; Radial velocity ; Space based observatories ; Spectroscopy ; Stars ; Stellar classification ; Stellar luminosities</subject><ispartof>Publications of the Astronomical Society of the Pacific, 1991-03, Vol.103 (661), p.294-299</ispartof><rights>1991 INIST-CNRS</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://www.jstor.org/stable/pdf/40679684$$EPDF$$P50$$Gjstor$$H</linktopdf><linktohtml>$$Uhttps://www.jstor.org/stable/40679684$$EHTML$$P50$$Gjstor$$H</linktohtml><link.rule.ids>314,777,781,800,57998,58231</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=19637383$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>BATTEN, A. H.</creatorcontrib><creatorcontrib>FLETCHER, J. M.</creatorcontrib><creatorcontrib>HILL, G.</creatorcontrib><creatorcontrib>LU, WENXIAN</creatorcontrib><creatorcontrib>MORBEY, C. L.</creatorcontrib><title>THE BINARY SYSTEM Σ2173</title><title>Publications of the Astronomical Society of the Pacific</title><description>New high-dispersion spectroscopic observations of the visual binary Σ2173 are combined with earlier ones obtained during passage through the opposite node, and with the available visual and interferometric observations, to determine the orbital elements completely. We find P =46y.43, T=1962.52, Ω = 152°.7, ω=98°.7, ω=147°.6, α" = 0°.97, V₀ = -76.98 km s⁻¹ and K₂ = 4.84 km s⁻¹. The parallax derived is O". O59, somewhat larger than the best trigonometrical value of O". O5, which leads to masses and luminosities for the components in good agreement with the spectral types and luminosity classes but which are problematical from the point of view of theoretical studies of stellar evolution. The two stars are very similar: We can distinguish no difference in spectral type and find Δm to be approximately 0ṃ1. The brighter star appears to be the less massive.</description><subject>Astronomy</subject><subject>Binary and multiple stars</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Multiple stars</subject><subject>Observational astronomy</subject><subject>Orbital elements</subject><subject>Orbits</subject><subject>Parallax</subject><subject>Radial velocity</subject><subject>Space based observatories</subject><subject>Spectroscopy</subject><subject>Stars</subject><subject>Stellar classification</subject><subject>Stellar luminosities</subject><issn>0004-6280</issn><issn>1538-3873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1991</creationdate><recordtype>article</recordtype><recordid>eNo9jLFKA0EURQdRcI32NsI2lgNv5s28eVPGsJpANJBskyo8d3cgS9SwY-P3-D9-kwkRq1vcc86ZKoxH1sgBz1UBAE6TZbhUVzn3AMawgULd1tOqfJi9jJfrcrVe1dVz-fNtTcBrdZFkl7ubvx2p-rGqJ1M9XzzNJuO57r1FzQ15lvQa0YCweO4IyPuOiF1sCSBGcG0wFix7CJFC26aj0KRInUQcqftTdi-5kV0a5L3Z5s1-2L7J8LUxkTAg44G7O3F9_vwY_n8HdIiyw1_OXj6r</recordid><startdate>19910301</startdate><enddate>19910301</enddate><creator>BATTEN, A. H.</creator><creator>FLETCHER, J. M.</creator><creator>HILL, G.</creator><creator>LU, WENXIAN</creator><creator>MORBEY, C. L.</creator><general>The Astronomical Society of the Pacific</general><general>University of Chicago Press</general><scope>IQODW</scope></search><sort><creationdate>19910301</creationdate><title>THE BINARY SYSTEM Σ2173</title><author>BATTEN, A. H. ; FLETCHER, J. M. ; HILL, G. ; LU, WENXIAN ; MORBEY, C. L.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-j523-8c658afb9310a8a58e60655e66849d6009904d712028507967ddf8afbcf96ea93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1991</creationdate><topic>Astronomy</topic><topic>Binary and multiple stars</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Multiple stars</topic><topic>Observational astronomy</topic><topic>Orbital elements</topic><topic>Orbits</topic><topic>Parallax</topic><topic>Radial velocity</topic><topic>Space based observatories</topic><topic>Spectroscopy</topic><topic>Stars</topic><topic>Stellar classification</topic><topic>Stellar luminosities</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>BATTEN, A. H.</creatorcontrib><creatorcontrib>FLETCHER, J. M.</creatorcontrib><creatorcontrib>HILL, G.</creatorcontrib><creatorcontrib>LU, WENXIAN</creatorcontrib><creatorcontrib>MORBEY, C. L.</creatorcontrib><collection>Pascal-Francis</collection><jtitle>Publications of the Astronomical Society of the Pacific</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>BATTEN, A. H.</au><au>FLETCHER, J. M.</au><au>HILL, G.</au><au>LU, WENXIAN</au><au>MORBEY, C. L.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>THE BINARY SYSTEM Σ2173</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>1991-03-01</date><risdate>1991</risdate><volume>103</volume><issue>661</issue><spage>294</spage><epage>299</epage><pages>294-299</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><coden>PASPAU</coden><abstract>New high-dispersion spectroscopic observations of the visual binary Σ2173 are combined with earlier ones obtained during passage through the opposite node, and with the available visual and interferometric observations, to determine the orbital elements completely. We find P =46y.43, T=1962.52, Ω = 152°.7, ω=98°.7, ω=147°.6, α" = 0°.97, V₀ = -76.98 km s⁻¹ and K₂ = 4.84 km s⁻¹. The parallax derived is O". O59, somewhat larger than the best trigonometrical value of O". O5, which leads to masses and luminosities for the components in good agreement with the spectral types and luminosity classes but which are problematical from the point of view of theoretical studies of stellar evolution. The two stars are very similar: We can distinguish no difference in spectral type and find Δm to be approximately 0ṃ1. The brighter star appears to be the less massive.</abstract><cop>Chicago, IL</cop><pub>The Astronomical Society of the Pacific</pub><tpages>6</tpages></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6280 |
| ispartof | Publications of the Astronomical Society of the Pacific, 1991-03, Vol.103 (661), p.294-299 |
| issn | 0004-6280 1538-3873 |
| language | eng |
| recordid | cdi_pascalfrancis_primary_19637383 |
| source | IOP Publishing Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; Jstor Complete Legacy; Institute of Physics (IOP) Journals - HEAL-Link; Alma/SFX Local Collection |
| subjects | Astronomy Binary and multiple stars Earth, ocean, space Exact sciences and technology Multiple stars Observational astronomy Orbital elements Orbits Parallax Radial velocity Space based observatories Spectroscopy Stars Stellar classification Stellar luminosities |
| title | THE BINARY SYSTEM Σ2173 |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-21T08%3A37%3A08IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-jstor_pasca&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=THE%20BINARY%20SYSTEM%20%CE%A32173&rft.jtitle=Publications%20of%20the%20Astronomical%20Society%20of%20the%20Pacific&rft.au=BATTEN,%20A.%20H.&rft.date=1991-03-01&rft.volume=103&rft.issue=661&rft.spage=294&rft.epage=299&rft.pages=294-299&rft.issn=0004-6280&rft.eissn=1538-3873&rft.coden=PASPAU&rft_id=info:doi/&rft_dat=%3Cjstor_pasca%3E40679684%3C/jstor_pasca%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_jstor_id=40679684&rfr_iscdi=true |