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Add 2 books for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

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{{Starbox begin
| name = WR 25
}}
{{Starbox image
| image=
{{Location mark
|image=Carina Nebula by ESO.jpg|alt=|float=center|width=280
|label=|position=right
|mark=Red circle.svg|mark_width=12|mark_link=WR 25
|x=582|y=740
}}
|caption=Location of WR 25的位置（紅圈）
|credit=[[歐洲南方天文台|ESO]]
}}
{{Starbox observe
| epoch = [[曆元|J2000.0]]
| equinox = [[曆元|J2000.0]]
| constell = [[船底座]]
| ra = {{RA|10|44|10.337}}<ref name=roeser>{{cite journal |bibcode=1988A&AS...74..449R |title=A new star catalogue of SAO type |journal=Astronomy and Astrophysics Supplement Series |issn=0365-0138 |volume=74 |pages=449 |author1=Roeser |first1=S. |last2=Bastian |first2=U. |date=1988}}</ref>
| dec = {{DEC|-59|43|11.41}}<ref name=roeser/>
| appmag_v = 8.80<ref name=ducati>{{cite journal |bibcode=2002yCat.2237....0D |title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system |journal=CDS/ADC Collection of Electronic Catalogues |volume=2237 |pages=0 |author1=Ducati |first1=J. R. |date=2002}}</ref>
}}
{{Starbox character
| type = [[沃夫–瑞葉星]]
| class = O2.5If*/WN6 + OB<ref name=gosss>{{cite journal |bibcode=2014ApJS..211...10S |title=The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars |journal=The Astrophysical Journal Supplement |volume=211 |issue=1 |pages=10 |author1=Sota |first1=A. |last2=Maíz Apellániz |first2=J. |last3=Morrell |first3=N. I. |author-link3=Nidia Morrell |last4=Barbá |first4=R. H. |last5=Walborn |first5=N. R. |last6=Gamen |first6=R. C. |last7=Arias |first7=J. I. |last8=Alfaro |first8=E. J. |year=2014 |doi=10.1088/0067-0049/211/1/10|arxiv = 1312.6222 }}</ref>
}}
{{Starbox astrometry
| radial_v = −34.6<ref name=gamen/>
| prop_mo_ra = {{val|-6.813|0.057}}<ref name=dr2/>
| prop_mo_dec = {{val|2.721|0.055}}<ref name=dr2/>
| parallax = 0.4763
| p_error = 0.0329
| parallax_footnote = <ref name=dr2>{{cite DR2|5350357519345171200}}</ref>
| dist_ly =
| dist_pc =
| absmag_bol =
| absmag_v = -6.98<ref name=hamann2019/>
}}
{{Starbox orbit
| reference=<ref name=gamen/>
| period_unitless=207.85 days
| eccentricity=0.50
| inclination=
| axis_unitless={{Solar radius|156}}
| k1=44
}}
{{Starbox detail
| component1 = WR
| mass = 98<ref name=hamann2019/>
| radius = 20.24<ref name=hamann2019/>
| luminosity_bolometric = 2,400,000<ref name=hamann2019/>
| temperature = 50,100<ref name=hamann2019>{{cite arXiv|eprint=1904.04687|last1=Sota|first1=A.|title=The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters|last2=Maíz Apellániz|first2=J.|last3=Morrell|first3=N. I.|author-link3=Nidia Morrell|last4=Barbá|first4=R. H.|last5=Walborn|first5=N. R.|last6=Gamen|first6=R. C.|last7=Arias|first7=J. I.|last8=Alfaro|first8=E. J.|last9=Oskinova|first9=L. M.|class=astro-ph.SR|year=2019}}</ref>
| age_myr =
}}
{{Starbox catalog
| names = [[HD星表|HD]] 93162、[[2微米全天巡天]] J10441038-5943111、WR 25、[[XMM-牛頓衛星|XMMU]] J104410.3-594311、[[波恩星表|CD]]−59°3282、[[PPM星表|PPM]] 339385、[[SAO星表|SAO]] 238408、[[川普勒16]] 177、[[導引星表|GSC]] 08626-01989、UBV 9882、Hen 3-478
}}
{{Starbox reference
| Simbad = HD+93162
}}
{{Starbox end}}
'''WR 25'''（'''HD 93162'''）是在[[船底座星雲]]湍流恆星形成區的[[聯星]]系統，距離[[地球]]大約6,800光年。它包含一顆[[沃夫–瑞葉星]]和一顆熱且明亮伴星，並且是[[川普勒16]]星團的成員。

== 光譜 ==
WR 25因為它的亮度和光譜以寬發射線為主，在19世紀就被認定為[[沃夫–瑞葉星]]<ref name=campbell>{{cite journal |bibcode=1894AstAp..13..448C |title=The Wolf-Rayet stars |url=https://archive.org/details/sim_astronomy-and-astro-physics_1894-06_13_7/page/448 |journal=Astronomy and Astro-Physics |volume=13 |pages=448 |author1=Campbell |first1=W. W. |year=1894}}</ref>。它的光譜包含氫線，介於經典的WN星和O型超巨星之間。這導致早期報告是聯星，例如WN7星加上O7的恆星<ref name=smith>{{cite journal |bibcode=1968MNRAS.138..109S |title=A revised spectral classification system and a new catalogue for galactic Wolf-Rayet stars |url=https://archive.org/details/sim_monthly-notices-of-the-royal-astronomical-society_1968_138_1/page/109 |journal=Monthly Notices of the Royal Astronomical Society |volume=138 |pages=109–121 |author1=Smith |first1=Lindsey F. |year=1968 |doi=10.1093/mnras/138.1.109|doi-access=free }}</ref>。它也被描述為WN7 + abs<ref name=crowther1993>{{cite journal |bibcode=1993SSRv...66..271C |title=Tailored analyses of 24 Galactic WN stars |journal=Space Science Reviews |volume=66 |issue=1–4 |pages=271–275 |author1=Crowther |first1=Paul A. |last2=Smith |first2=Linda J. |last3=Hillier |first3=D. John |year=1993 |doi=10.1007/BF00771076}}</ref>和WN6ha<ref>{{cite journal |bibcode=1998A&A...334..845S |title=The relationship between the WR classification and stellar models. II. The WN stars without hydrogen |journal=Astronomy and Astrophysics |volume=334 |pages=845 |author1=Smith |first1=Lindsey F. |last2=Maeder |first2=A. |year=1998}}</ref>。WR 25的光譜被歸類為特定分類引進的熱[[沃夫–瑞葉星#斜槓星|斜槓星]]，O2.5If<sup>*</sup>/WN6<sup> </sup>。由許多微弱的發射譜線，認識到有氮的存在，還有一些氫和氦的吸收線。這個分類表示比WN6ha光譜類型更精細，有更弱的發射線和更強的吸收線<ref name=crowther2011>{{cite journal |bibcode=2011MNRAS.416.1311C |arxiv=1105.4757 |title=Spectral classification of O2-3.5 If*/WN5-7 stars |journal=Monthly Notices of the Royal Astronomical Society |volume=416 |issue=2 |pages=1311 |author1=Crowther |first1=Paul A. |last2=Walborn |first2=Nolan R. |year=2011 |doi=10.1111/j.1365-2966.2011.19129.x}}</ref>。但是無法清楚的檢測到伴星的光譜，而對伴星的認識毫無貢獻<ref name=gamen/>。

== 性質 ==
[[File:WR 25 and Tr16-244 region (cropped).jpg|thumb|left|WR 25是影像中最亮的恆星。在其左側的橙色星只是前景星。]]

WR 25系統的主星大約比太陽亮240萬倍，並照亮了川普勒16星團的遠端。用於推導恆星參數的模型不適合在聯星系統中使用，作者指出伴星佔系統亮度的15%以上，因此亮度極不穩定。早先基於電離通量測量的估計所產生的值為太陽的150萬倍，其它物理數據的估計值也相應降低<ref name=crowther>{{Cite journal |doi=10.1046/j.1365-8711.1998.01400.x |title=Quantitative spectroscopy of Wolf--Rayet stars in HD 97950 and R136a -- the cores of giant H II regions |url=https://archive.org/details/sim_monthly-notices-of-the-royal-astronomical-society_1998-05-21_296_3/page/622 |journal=Monthly Notices of the Royal Astronomical Society |volume=296 |issue=3 |pages=622–642 |year=1998 |last1=Crowther |first1=P. A. |last2=Dessart |first2=L. |bibcode=1998MNRAS.296..622C|doi-access=free }}</ref>。

伴星被認為是一顆年輕的炙熱大質量恆星，類似於其它已知的WR + O 或WR + WR聯星。據報導，它曾被視為O4超巨星，但後續的測量仍然不確定確實的光譜類型。兩顆炙熱恆星的[[恆星風]]碰撞，產生硬X射線<ref name=pandey>{{Cite journal |doi=10.1088/0004-637X/788/1/84 |title=Phase-Resolvedxmm-Newtonandswiftobservations of Wr 25 |journal=The Astrophysical Journal |volume=788 |issue=1 |pages=84 |year=2014 |last1=Pandey |first1=J. C. |last2=Pandey |first2=S. B. |last3=Karmakar |first3=S. |bibcode=2014ApJ...788...84P |arxiv=1405.7137}}</ref>，而早在檢測到208天的軌道周期之前出，就懷疑是聯星<ref name=gamen>{{Cite journal |doi=10.1051/0004-6361:20065618 |title=The first orbital solution for the massive colliding-wind binary HD 93162 (≡WR 25) |journal=Astronomy and Astrophysics |volume=460 |issue=3 |pages=777–782 |year=2006 |last1=Gamen |first1=R. |last2=Gosset |first2=E. |last3=Morrell |first3=N. |author-link3=Nidia Morrell |last4=Niemela |first4=V. |last5=Sana |first5=H. |last6=Nazé |first6=Y. |last7=Rauw |first7=G. |last8=Barbá |first8=R. |last9=Solivella |first9=G. |bibcode=2006A&A...460..777G |arxiv=astro-ph/0609454}}</ref>。

WR 25雖然非常明亮，但由於星雲中大量灰塵的[[消光]]，以及大部分的輻射是在[[紫外線]]，所以無法以肉眼看見，而只能在X射線和紅外線中觀測<ref name=pandey/><ref name=sanchawaka>{{Cite journal |doi=10.1086/510184 |title=An X‐Ray and Near‐Infrared Study of Young Stars in the Carina Nebula |url=https://archive.org/details/sim_astrophysical-journal_2007-02-10_656_1/page/462 |journal=The Astrophysical Journal |volume=656 |issue=1 |pages=462–473 |year=2007 |last1=Sanchawala |first1=K. |last2=Chen |first2=W. P. |last3=Lee |first3=H. T. |last4=Chu |first4=Y. H. |last5=Nakajima |first5=Y. |last6=Tamura |first6=M. |last7=Baba |first7=D. |last8=Sato |first8=S. |bibcode=2007ApJ...656..462S|citeseerx=10.1.1.667.3955 }}</ref>。

WR 25位於川普勒16星團的西側邊界處，是[[銀河系]]中最巨大的[[恆星運動學#星協|OB星協]][[船底座OB1]]的一部分<ref name=wolk>{{cite journal |bibcode=2011ApJS..194...12W |arxiv=1103.1126 |title=The Chandra Carina Complex Project View of Trumpler 16 |journal=The Astrophysical Journal Supplement |volume=194 |issue=1 |pages=12 |author1=Wolk |first1=Scott J. |last2=Broos |first2=Patrick S. |last3=Getman |first3=Konstantin V. |last4=Feigelson |first4=Eric D. |last5=Preibisch |first5=Thomas |last6=Townsley |first6=Leisa K. |last7=Wang |first7=Junfeng |last8=Stassun |first8=Keivan G. |last9=King |first9=Robert R.|last10=McCaughrean|first10=Mark J. |last11=Moffat |first11=Anthony F. J. |last12=Zinnecker |first12=Hans |year=2011 |doi=10.1088/0067-0049/194/1/12}}</ref>。由於它極端的亮度，對恆星環境有極大的影響，從恆星移動離開的細長弧線和細絲中可以看到[[船底座星雲#鑰匙孔星雲|手指星雲]]<ref name=walborn>{{cite journal |bibcode=2012ASSL..384...25W |title=The Company Eta Carinae Keeps: Stellar and Interstellar Content of the Carina Nebula |journal=Eta Carinae and the Supernova Impostors |volume=384 |pages=25–42 |author1=Walborn |first1=Nolan R. |year=2012 |doi=10.1007/978-1-4614-2275-4_2 |series=Astrophysics and Space Science Library |isbn=978-1-4614-2274-7}}</ref>。

== 相關條目 ==
*[[R136a1]]
*[[手槍星]]
*[[WR 102ka]]
*[[LBV 1806-20]]

== 參考資料 ==
{{Reflist}}

{{船底座恆星}}

[[Category:船底座星雲]]
[[Category:沃尔夫-拉叶星]]
[[Category:船底座]]
[[Category:HD和HDE天體|093162]]
[[Category:O型超巨星]]
[[Category:光譜聯星]]
[[Category:2MASS天體]]
[[Category:波恩天體]]

WR 25 - 版本历史

imported>InternetArchiveBot：​Add 2 books for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

imported>InternetArchiveBot：Add 2 books for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot