75 PEGASI, A VERY-SHORT-PERIOD EXTREME MASS RATIO BINARY
The bright star 75 Peg has long been known to be a spectroscopie binary. The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available sp...
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| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 1985-03, Vol.97 (589), p.280-284 |
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| container_end_page | 284 |
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| container_issue | 589 |
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| container_title | Publications of the Astronomical Society of the Pacific |
| container_volume | 97 |
| creator | HUBE, DOUGLAS P. GULLIVER, AUSTIN F. |
| description | The bright star 75 Peg has long been known to be a spectroscopie binary. The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available spectroscopie observations leads to the conclusion that the primary fills, or is very close to filling, its critical Roche lobe, and will begin to lose mass to its companion before leaving the main sequence. |
| doi_str_mv | 10.1086/131530 |
| format | Article |
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The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available spectroscopie observations leads to the conclusion that the primary fills, or is very close to filling, its critical Roche lobe, and will begin to lose mass to its companion before leaving the main sequence.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>DOI: 10.1086/131530</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 ; Main sequence stars ; Mass ratio ; Mass spectroscopy ; Observatories ; Orbital elements ; Orbital velocity ; Radial velocity ; Rotation ; Spectroscopic binaries. 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The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available spectroscopie observations leads to the conclusion that the primary fills, or is very close to filling, its critical Roche lobe, and will begin to lose mass to its companion before leaving the main sequence.</description><subject>Astronomy</subject><subject>Binary and multiple stars</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Main sequence stars</subject><subject>Mass ratio</subject><subject>Mass spectroscopy</subject><subject>Observatories</subject><subject>Orbital elements</subject><subject>Orbital velocity</subject><subject>Radial velocity</subject><subject>Rotation</subject><subject>Spectroscopic binaries. 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Close binaries</topic><topic>Stars</topic><topic>Stellar radii</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>HUBE, DOUGLAS P.</creatorcontrib><creatorcontrib>GULLIVER, AUSTIN F.</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Publications of the Astronomical Society of the Pacific</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>HUBE, DOUGLAS P.</au><au>GULLIVER, AUSTIN F.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>75 PEGASI, A VERY-SHORT-PERIOD EXTREME MASS RATIO BINARY</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>1985-03-01</date><risdate>1985</risdate><volume>97</volume><issue>589</issue><spage>280</spage><epage>284</epage><pages>280-284</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><coden>PASPAU</coden><abstract>The bright star 75 Peg has long been known to be a spectroscopie binary. The orbital parameters are presented here for the first time, and include the very short period of 0ḍ5021035. The system has one of the most extreme values of mass ratio known. The most direct interpretation of the available spectroscopie observations leads to the conclusion that the primary fills, or is very close to filling, its critical Roche lobe, and will begin to lose mass to its companion before leaving the main sequence.</abstract><cop>Chicago, IL</cop><pub>The Astronomical Society of the Pacific</pub><doi>10.1086/131530</doi><tpages>5</tpages><oa>free_for_read</oa></addata></record> |
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| identifier | ISSN: 0004-6280 |
| ispartof | Publications of the Astronomical Society of the Pacific, 1985-03, Vol.97 (589), p.280-284 |
| issn | 0004-6280 1538-3873 |
| language | eng |
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| source | JSTOR Archive Collection A-Z Listing; Institute of Physics Journals; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astronomy Binary and multiple stars Earth, ocean, space Exact sciences and technology Main sequence stars Mass ratio Mass spectroscopy Observatories Orbital elements Orbital velocity Radial velocity Rotation Spectroscopic binaries. Close binaries Stars Stellar radii |
| title | 75 PEGASI, A VERY-SHORT-PERIOD EXTREME MASS RATIO BINARY |
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