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- WR 137 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus. WR 137, together with WR 134 and WR 135, was one of three stars in Cygnus observed in 1867 to have unusual spectra consisting of intense emission lines rather than the more normal continuum and absorption lines. These were the first members of the class of stars that came to be called Wolf-Rayet stars (WR stars) after Charles Wolf and Georges Rayet who discovered their unusual appearance. It is a member of the carbon sequence of WR stars, indicated by the lack of nitrogen lines and the strength of carbon emission. WR 137 has a spectrum with CIII emission weaker than CIV and OV weaker still, leading to the assignment of a WC7 spectral type. The spectrum also shows emission lines of HeII and OIV. WR 137 is a binary system, with an O9 main sequence or giant companion. The two stars orbit every thirteen years in a mildly eccentric orbit, and there is an episode of dust production near periastron. The inclination of the orbit is uncertain, most likely near 67° but with some analyses suggesting values around 23°. The O star is visually brighter and more massive, but the WR star dominates the spectrum and has a higher bolometric luminosity. Visible in the spectrum are absorption lines and some narrow emission lines, each thought to originate from the secondary star. The line profiles suggest a decretion disc around the star, produced by its rapid rotation, which would make it the only known system containing a WR star and an Oe star. WR 137 is about a degree away from WR 135 and the two are believed to lie at approximately the same distance from Earth within the Cygnus OB3 association. Its properties are uncertain because of the presence of the hot luminous companion. A pseudo-fit of the combined spectrum yielded a temperature of 56,000 K, a luminosity of 537,000 L☉, and a radius of 10 R☉. A more typical radius for a WC7 star would be 4.5 R☉, implying a hotter temperature. Evolutionary modelling of the WR 137 pair suggest an initial mass for the primary of 60 M☉ and for the secondary of 30 M☉, with an age of 4.1 million years. The initial orbital period would have been around 1,580 days. Around three M☉ have been transferred from the primary to the secondary. (en)
- WR 137位於天鵝座，是一顆距離地球大約6,000光年的沃夫–瑞葉星變星。WR 137與WR 134和WR 135是1867年在天鵝座觀測到的3顆光譜在連續的譜帶中有強烈的發射線，而不是常見的吸收線組成。它們是天文學家沃夫和瑞葉發現的第一批外觀不尋常，並以發現著的名字命名的沃夫–瑞葉星。它是碳序列的沃夫–瑞葉星，表明缺乏氮的譜線而有強的碳發射譜線射。WR 137光譜的CIII發射比CIV微弱，OV也微弱，因此它的光譜型為WC7。它的頻譜還顯示HeII和OIV的譜線。 WR 137是聯星系統，伴星O9的主序星或巨星。這兩顆星在一個相對扁平的橢圓軌道上互繞，軌道週期為13年。在近星點附近似乎產生了一個塵埃雲。軌道的傾斜度不確定，很可能在67°附近，氮一些分析的建議值在23°左右。O型星在視覺上更亮，質量也更大，但WR星主導了光譜，具有更高的輻射熱發光度（熱光度）。 WR 137距離WR135大約1度，兩者被認為都在天鵝座OB3星協內，且與地球有大致相同的距離。因為存在熱發光伴侶，使它的屬性不確定。組合光譜的偽擬合產生56,000K的溫度，光度為537,000 L☉，半徑為10 R☉。典型WC7型的半徑是4.5 R☉，這意味著溫度要更熱。 (zh)
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- WR 137位於天鵝座，是一顆距離地球大約6,000光年的沃夫–瑞葉星變星。WR 137與WR 134和WR 135是1867年在天鵝座觀測到的3顆光譜在連續的譜帶中有強烈的發射線，而不是常見的吸收線組成。它們是天文學家沃夫和瑞葉發現的第一批外觀不尋常，並以發現著的名字命名的沃夫–瑞葉星。它是碳序列的沃夫–瑞葉星，表明缺乏氮的譜線而有強的碳發射譜線射。WR 137光譜的CIII發射比CIV微弱，OV也微弱，因此它的光譜型為WC7。它的頻譜還顯示HeII和OIV的譜線。 WR 137是聯星系統，伴星O9的主序星或巨星。這兩顆星在一個相對扁平的橢圓軌道上互繞，軌道週期為13年。在近星點附近似乎產生了一個塵埃雲。軌道的傾斜度不確定，很可能在67°附近，氮一些分析的建議值在23°左右。O型星在視覺上更亮，質量也更大，但WR星主導了光譜，具有更高的輻射熱發光度（熱光度）。 WR 137距離WR135大約1度，兩者被認為都在天鵝座OB3星協內，且與地球有大致相同的距離。因為存在熱發光伴侶，使它的屬性不確定。組合光譜的偽擬合產生56,000K的溫度，光度為537,000 L☉，半徑為10 R☉。典型WC7型的半徑是4.5 R☉，這意味著溫度要更熱。 (zh)
- WR 137 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus. WR 137, together with WR 134 and WR 135, was one of three stars in Cygnus observed in 1867 to have unusual spectra consisting of intense emission lines rather than the more normal continuum and absorption lines. These were the first members of the class of stars that came to be called Wolf-Rayet stars (WR stars) after Charles Wolf and Georges Rayet who discovered their unusual appearance. It is a member of the carbon sequence of WR stars, indicated by the lack of nitrogen lines and the strength of carbon emission. WR 137 has a spectrum with CIII emission weaker than CIV and OV weaker still, leading to the assignment of a WC7 spectral type. The spectrum also shows emission l (en)
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