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HD 93205, or V560 Carinae, is a binary ste … HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula (NGC 3372) in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days. The more massive member of the pair is an O3.5 main sequence star. The spectrum shows some ionised nitrogen and helium emission lines, indicating some mixing of fusion products to the surface and a strong stellar wind. The mass calculated from apsidal motion of the orbits is 40 to 60 M☉. This is somewhat lower than expected from evolutionary modelling of a star with its observed parameters. The less massive member is an O8 main sequence star of approximately 20 M☉. It moves in its orbit at a speed of over 300 km/s and is considered to be a relativistic binary, which causes the apses of the orbit to change in a predictable way. The closeness of the two stars causes them to become deformed, and this means that the observed brightness of the system varies slightly every six days during its orbit. The total amplitude of the variation is only 0.02 magnitudes. It is generally considered as a member of the open cluster Trumpler 16. Among its neighbors are some of the most massive and luminous stars in the galaxy, like Eta Carinae, HD 93250 and the binary HD 93129. It lies five arc-minutes from Eta Carinae.It lies five arc-minutes from Eta Carinae.
, HD 93205或稱為船底座V560（V560 Carinae）是一個位於船底座星雲內的船底座聯星。該聯星系統包含兩個大質量的O型恆星，軌道週期6日。質量較高的成員星光譜型 O3V，大約45倍太陽質量，質量較低者大約是太陽質量的20倍，光譜型 O8V。 在HD 93205的鄰近區域有數顆銀河系中質量極大與光度極高的數顆恆星，例如海山二、HD 93250和聯星HD 93129。
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60
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17
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3.6
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7
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51300
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| rdfs:comment |
HD 93205或稱為船底座V560（V560 Carinae）是一個位於船底座星雲內的船底座聯星。該聯星系統包含兩個大質量的O型恆星，軌道週期6日。質量較高的成員星光譜型 O3V，大約45倍太陽質量，質量較低者大約是太陽質量的20倍，光譜型 O8V。 在HD 93205的鄰近區域有數顆銀河系中質量極大與光度極高的數顆恆星，例如海山二、HD 93250和聯星HD 93129。
, HD 93205, or V560 Carinae, is a binary ste … HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula (NGC 3372) in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days. The more massive member of the pair is an O3.5 main sequence star. The spectrum shows some ionised nitrogen and helium emission lines, indicating some mixing of fusion products to the surface and a strong stellar wind. The mass calculated from apsidal motion of the orbits is 40 to 60 M☉. This is somewhat lower than expected from evolutionary modelling of a star with its observed parameters.ng of a star with its observed parameters.
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HD 93205
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