查看“︁IC 4651”︁的源代码

{{Infobox Cluster
|name=IC 4651
|image=[[File:The rich star cluster IC 4651.jpg|300px|The rich star cluster IC 4651]]
|caption= Wide Field Imager (WFI) camera拍摄到的疏散星团IC 4651，利用[[欧洲南方天文台]]在[[智利]][[拉西亚天文台]]的MPG/ESO 2.2米望远镜。<ref>{{cite web|title=Sibling Stars|url=http://www.eso.org/public/news/eso1534/|accessdate=19 August 2015|archive-date=2017-12-27|archive-url=https://web.archive.org/web/20171227124238/http://www.eso.org/public/news/eso1534/|dead-url=no}}</ref>
|epoch=[[J2000]]
|constellation=[[天坛座]]
|ra={{RA|17|24|49}}<ref name=apj619></ref>
|dec={{DEC|−49|56|00}}<ref name=apj619></ref>
|dist_ly=2,900 [[光年|ly]]
|dist_pc=888<ref name=aaa389></ref>&nbsp;[[秒差距|pc]]
|size_v=10.0' ([[角分]])
|names=Melotte 169
}}
'''IC 4651'''是一个位于[[天坛座]]，距离地球约2900光年的[[疏散星团]]，最早由[[約翰·路易·埃米爾·德雷耳|约翰·路易斯·埃米尔·德雷尔]]在他的1895年版''[[NGC天體表|NGC天体表]]''中记录<ref name=mras51/>。 

IC 4651的年龄大约为1.2±0.2亿年，属于中等年龄的[[星团]]<ref name=aaa475/>。 与太阳相比，该星团中的[[恒星]]具有更高的[[化學元素豐度|化学元素丰度]]（[[氢]]和[[氦]]除外）<ref name=aaa424/>。

IC 4651中活动恒星的总质量约为630个[[太阳质量]]<ref name=aaa386/>。目前已知的活动恒星的质量只占星团初始质量的约7%。剩余质量中约35%演化成了[[白矮星]]或其他[[致密星]]。其余丢失质量组成的恒星星已经离开了星团主体或完全离开星团<ref name=aaa386/>。

== 参考资料 ==
{{reflist|refs=<ref name="aaa389">{{cite journal |author1=Dias, W.S. |author2=Alessi, B.S. |author3=Moitinho, A. |author4=Lepine. J.R.D. | title=New catalog of optically visible open clusters and candidates | journal=Astronomy and Astrophysics | volume=389 | pages=871–873 |date=July 2002 | doi=10.1051/0004-6361:20020668 | bibcode=2002A&A...389..871D |arxiv = astro-ph/0203351 }} Note: see the [[VizieR]] catalogue [http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/ocl B/ocl] {{Wayback|url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B%2Focl |date=20201020004242 }}.</ref>

<ref name="mras51">{{cite journal | last=Dreyer | first=J. L. E. | title=Index Catalogue of Nebulae found in the years 1888 to 1894, with Notes and Corrections to the New General Catalogue | journal=Memoirs of the Royal Astronomical Society | volume=51 | pages=185–228 | year=1895 | bibcode=1895MmRAS..51..185D }}</ref>

<ref name="apj619">{{cite journal |author1=Xin, Y. |author2=Deng, L. | title=Blue Stragglers in Galactic Open Clusters and Integrated Spectral Energy Distributions | journal=The Astrophysical Journal | volume=619| issue=2 | pages=824–838 |date=February 2005
| doi=10.1086/426681 | bibcode=2005ApJ...619..824X |arxiv = astro-ph/0410325 }}</ref>

<ref name="aaa475">{{cite journal 
 | display-authors=1 | last1=Biazzo | first1=K.
 | last2=Pasquini | first2=L. | last3=Girardi | first3=L.
 | last4=Frasca | first4=A. | last5=da Silva | first5=L.
 | last6=Setiawan | first6=J. | last7=Marilli | first7=E.
 | last8=Hatzes | first8=A. P. | last9=Catalano | first9=S.
 | title=Deriving temperature, mass, and age of evolved stars from high-resolution spectra. Application to field stars and the open cluster IC 4651
 | journal=Astronomy and Astrophysics | arxiv=0704.3192
 | volume=475 | issue=3 | date=December 2007 | pages=981–989
 | doi=10.1051/0004-6361:20077374 | bibcode=2007A&A...475..981B }}</ref>

<ref name="aaa424">{{cite journal | author=Pasquini, L. |display-authors=etal | title=Detailed chemical composition of the open cluster IC 4651: The iron peak, α elements, and Li | journal=Astronomy and Astrophysics | volume=424 | pages=951–963 |date=September 2004 | doi=10.1051/0004-6361:20040240 | bibcode=2004A&A...424..951P |arxiv = astro-ph/0406113 }} This source gives a [[metallicity]] value of <math>\begin{smallmatrix}\left[\frac{Fe}{H}\right]\ =\ +0.10\ \pm\ 0.03\end{smallmatrix}</math>, which is equivalent to 125% of the Sun's abundance of Iron.</ref>

<ref name="aaa386">{{cite journal |author1=Meibom, S. |author2=Andersen, J. |author3=Nordström, B. | title=Critical tests of stellar evolution in open clusters. III. Stellar population and dynamical evolution of IC 4651 | journal=Astronomy and Astrophysics | volume=386 | pages=187–203 |date=April 2002 | doi=10.1051/0004-6361:20020183 | bibcode=2002A&A...386..187M }}</ref>}}

[[Category:IC天体]]
[[Category:疏散星团]]
[[Category:天坛座]]