查看“︁超星團”︁的源代码

'''超星團''' ('''SSC''')是一個很大的[[恆星形成]]區域，被認為是[[球狀星團]]的前身<ref name=gallagher02>{{cite journal
 | author = Gallagher & Grebel
 | year = 2002
 | title = Extragalactic Star Clusters: Speculations on the Future
 | journal = Extragalactic Star Clusters, IAU Symposium
 | pages = 207
 | url = http://adsabs.harvard.edu/abs/2002IAUS..207..745G
 | access-date = 2010-05-27
 | archive-date = 2017-07-10
 | archive-url = https://web.archive.org/web/20170710025441/http://adsabs.harvard.edu/abs/2002IAUS..207..745G
 }}</ref>。它們通常包含大量被[[電離氫區]]環繞的[[金牛T星|年輕]]、[[OB 星|大質量恆星]]，類似於我們[[銀河系]]內的「超密電離氫區」(UDHIIs)<ref name=kobulnicky99>{{cite journal
 | author = Kobulnicky & Johnson
 | year = 1999
 | title = Signatures of the Youngest Starbursts: Optically Thick Thermal Bremsstrahlung Radio Sources in Henize 2-10
 | journal = ApJ
 | pages = 154–166
 | volume = 527
 | url = http://adsabs.harvard.edu/abs/1999ApJ...527..154K
 | doi = 10.1086/308075
 | last2 = Johnson
 | first2 = Kelsey E.
 | access-date = 2010-05-27
 | archive-date = 2019-08-22
 | archive-url = https://web.archive.org/web/20190822123634/http://adsabs.harvard.edu/abs/1999ApJ...527..154K
 }}</ref>。一個超星團的[[電離氫區]]像是被翻轉出來的[[宇宙塵|塵埃]]繭包圍著。在許多情況下，恆星和電離氫區都因為高度的[[消光]]而在光學上是看不見的。結果是，越年輕的超星團越適合用[[射電天文學|電波]]和[[紅外線天文學|紅外線]]觀測<ref name=johnson04>{{cite journal
 | author = Johnson
 | year = 2004
 | title = Extragalactic Ultracompact HII Regions: Probing the Birth Environments of Super Star Clusters
 | journal = Astronomical Society of the Pacific Conference Series
 | pages = 322
 | volume = 527
 | url = http://adsabs.harvard.edu/abs/2004ASPC..322..339J
}}</ref>。

超星團獨特的特徵是巨大的[[電子]][[密度]] <math>n_e=10^3</math>–<math>10^6</math> [[立方公分|cm<math>^{-3}</math>]]和[[壓力]] <math>P/</math>[[波茲曼常數|<math>k_b</math>]]<math>=10^7</math>–<math>10^{10}</math> [[熱力學溫標|K]] [[立方公分|cm<math>^{-3}</math>]]<ref name=johnson04/>。

雖然在其他星系有許多超星團的例子，但[[維斯特盧1]] (Westerlund 1) 可能是[[銀河系]]內唯一的一個超星團群集<ref>{{cite news | date=March 22, 2005 | title=Young and Exotic Stellar Zoo: ESO's Telescopes Uncover Super Star Cluster in the Milky Way | publisher=ESO | url=http://www.eso.org/outreach/press-rel/pr-2005/pr-08-05.html | accessdate=2007-03-20 | archive-url=https://web.archive.org/web/20070409105105/http://eso.org/outreach/press-rel/pr-2005/pr-08-05.html | archive-date=2007-04-09 | dead-url=yes }}</ref>。在邻近宇宙中，碰撞星系[[NGC 4038]]/NGC 4039 含有大量的超级星团，一般当相互作用的星系富含气体时，都是孕育超星团的温床。早期宇宙中，超级星团非常普遍；而现在的星系，由于宇宙密度的大幅度下降，超星团已经罕见了。

== 列表 ==
{|class=wikitable
|-
! 名稱
! 星系
! 說明
! 註解
|-
| [[維斯特盧1]] (Wd1)
| [[銀河系]]
| 在我門的銀河系發現的第一個超星團。
| <ref> Astronomy and Astrophysics, "On the massive stellar population of the super star cluster Westerlund 1", '''Clark, J. S.; Negueruela, I.; Crowther, P. A.; Goodwin, S. P.''', ''Volume 434, Issue 3, May II 2005, pp.949-969'', {{doi|10.1051/0004-6361:20042413}} , {{bibcode|2005A&A...434..949C}} , {{arXiv|astro-ph/0504342v2}} </ref>
|-
| [[R136]]
| [[大麥哲倫星系]] (LMC)
| 超星團的原型
| <ref> Astrophysical Journal, "Star Formation in R136: A Cluster of O3 Stars Revealed by Hubble Space Telescope Spectroscopy", '''Massey, Philip; Hunter, Deidre A.''', ''01/1998, v.493, p.180'', {{doi|10.1086/305126}} , {{bibcode|1998ApJ...493..180M}} </ref>
|-
|
| [[NGC 1569]]
| 包含兩個超星團的星系
| <ref>"The Star Clusters in the Starburst Irregular Galaxy NGC 1569" http://adsabs.harvard.edu/abs/2000AJ....120.2383H</ref>
|}

{{listdev}}

== 參考資料 ==
{{Reflist}}

== 外部連結 ==
*[http://www.sciencedaily.com/releases/2005/05/050528143304.htm Monster Super Star Cluster Discovered In Milky Way] {{Wayback|url=http://www.sciencedaily.com/releases/2005/05/050528143304.htm |date=20120811210143 }}


[[Category:星團]]