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HD 202206 b - 版本历史
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<p><b>新页面</b></p><div>{{Planetbox begin<br />
| name = HD 202206 b<br />
}}<br />
{{Planetbox star<br />
| star = [[HD 202206]]<br />
| constell = [[摩羯座]]<br />
| RA = {{RA|21|14|57.79}}<br />
| DEC = {{DEC|-20|47|20.1}}<br />
| dist_ly = 151.14<br />
| dist_pc = 46.3<br />
| class = G6V<br />
}}<br />
{{Planetbox orbit<br />
| semimajor = 0.83<ref name="correia"/><br />
| eccentricity = 0.435 ± 0.001<ref name="correia"/><br />
| period = 255.87 ± 0.06<ref name="correia"/><br />
| arg_peri = 161.18 ± 0.3<ref name="correia"/><br />
}}<br />
{{Planetbox character<br />
| minimum_mass = 17.4<ref name="correia"/><br />
}}<br />
{{Planetbox discovery<br />
| discovery_date = 2000年<ref>{{cite web | title=Exoplanets Galore! | url=http://www.eso.org/public/outreach/press-rel/pr-2000/pr-13-00.html | date=4 May 2000 | work= | publisher=European Southern Observatory | accessdate=8 August 2009 | deadurl=yes | archiveurl=https://web.archive.org/web/20090228024326/http://www.eso.org/public/outreach/press-rel/pr-2000/pr-13-00.html | archivedate=2009年2月28日 }}</ref> <br />
| discoverers = [[米歇爾·麥耶]]等人<br />
| discovery_method = [[都卜勒光譜學]]<br />
| discovery_site = {{flag|France}}<br />
| discovery_status = 已確認<br />
}}<br />
{{Planetbox end}}<br />
<br />
'''HD 202206 b'''是一個環繞恆星 [[HD 202206]] 的次恆星天體，距離地球約151光年。該天體可能是[[系外行星]]或[[棕矮星]]，但目前仍未確認<ref name="correia">{{cite journal |url=http://www.edpsciences.org/articles/aa/abs/2005/35/aa2376-04/aa2376-04.html |author=Correia, A. et al. |title=The CORALIE survey for southern extra-solar planets. XIII. A pair of planets around HD202206 or a circumbinary planet? |journal=[[Astronomy and Astrophysics]] |volume=440 |issue=2 |year=2005 |pages=751–758 |doi=10.1051/0004-6361:20042376 |format=abstract |bibcode=2005A&A...440..751C |arxiv=astro-ph/0411512 |deadurl=yes |archiveurl=https://web.archive.org/web/20051023060124/http://www.edpsciences.org/articles/aa/abs/2005/35/aa2376-04/aa2376-04.html |archivedate=2005-10-23 |access-date=2012-07-30 }}</ref>。該天體質量至少是木星的17.4倍，這超過了讓星體核心中的氫可經由[[核融合]]變成氘的質量下限。氘燃燒是否會發生是國際天文聯會的太陽系外行星工作小組界定氣體巨行星和棕矮星的方式，照此定義 HD 202206 b 應屬於棕矮星<ref>{{cite web|url=http://www.dtm.ciw.edu/users/boss/definition.html|title=Definition of a "Planet"|publisher=Working Group on Extrasolar Planets (WGESP) of the International Astronomical Union|accessdate=2009-07-04|archive-date=2012-04-10|archive-url=https://www.webcitation.org/66oFUmADq?url=http://www.dtm.ciw.edu/users/boss/definition.html|dead-url=no}}</ref>。另一方面，行星形成的[[吸積]]模擬顯示它可以形成最高25到30倍木星質量，而且這類天體仍屬於行星<ref>{{cite arXiv|eprint=0710.5667|class=astro-ph|title=Giant Planet Formation by Core Accretion|version=v1|author=Mordasini, C. ''et al.''|year=2007|accessdate=2008-10-04}}</ref><ref>{{cite journal |url=http://www.edpsciences.org/articles/aa/abs/2002/28/aa2416/aa2416.html |author=Udry, S. et al. |title=The CORALIE survey for southern extra-solar planets VIII. The very low-mass companions of HD 141937, HD 162020, HD 168443, HD 202206: Brown dwarfs or "superplanets"? |journal=[[Astronomy and Astrophysics]] |volume=390 |issue=1 |year=2002 |pages=267–279 |doi=10.1051/0004-6361:20020685 |format=abstract |bibcode=2002A&A...390..267U |arxiv=astro-ph/0202458 |deadurl=yes |archiveurl=https://web.archive.org/web/20060601190259/http://www.edpsciences.org/articles/aa/abs/2002/28/aa2416/aa2416.html |archivedate=2006-06-01 |access-date=2012-07-30 }}</ref>。<br />
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==參考資料==<br />
{{reflist}}<br />
<br />
{{Sky|21|14|57.79|-|20|47|20.1|151.14}}<br />
<br />
[[Category:棕矮星]]<br />
[[Category:摩羯座]]</div>
imported>InternetArchiveBot