Tables of the partition functions for iron, Fe I -- Fe X.pdfVIP

下载本文档

5
0
约1.96万字
约 9页
2017-04-09 发布于江苏
举报
版权申诉

Tables of the partition functions for iron, Fe I -- Fe X.pdf

1、有哪些信誉好的足球投注网站（book118）网站文档一经付费（服务费），不意味着购买了该文档的版权，仅供个人/单位学习、研究之用，不得用于商业用途，未经授权，严禁复制、发行、汇编、翻译或者网络传播等，侵权必究。。
2、本站所有内容均由合作方或网友上传，本站不对文档的完整性、权威性及其观点立场正确性做任何保证或承诺！文档内容仅供研究参考，付费前请自行鉴别。如您付费，意味着您自己接受本站规则且自行承担风险，本站不退款、不进行额外附加服务；查看《如何避免下载的几个坑》。如果您已付费下载过本站文档，您可以点击这里二次下载。
3、如文档侵犯商业秘密、侵犯著作权、侵犯人身权等，请点击“版权申诉”（推荐），也可以打举报电话：400-050-0827(电话支持时间：9:00-18:30)。
4、该文档为VIP文档，如果想要下载，成为VIP会员后，下载免费。
5、成为VIP后，下载本文档将扣除1次下载权益。下载后，不支持退款、换文档。如有疑问请联系我们。
6、成为VIP后，您将拥有八大权益，权益包括：VIP文档下载权益、阅读免打扰、文档格式转换、高级专利检索、专属身份标志、高级客服、多端互通、版权登记。
7、VIP文档为合作方或网友上传，每下载1次，网站将根据用户上传文档的质量评分、类型等，对文档贡献者给予高额补贴、流量扶持。如果你也想贡献VIP文档。上传文档

Tables of the partition functions for iron, Fe I -- Fe X

a r X i v : a s t r o - p h / 0 2 0 4 3 8 4 v 1 2 3 A p r 2 0 0 2 Tables of the partition functions for iron, Fe I – Fe X. J. Halenka 1, and J. Madej 2, 3 1Institute of Physics, University of Opole, Oleska 48, 45–052 Opole, Poland e-mail: halenka@uni.opole.pl 2Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warszawa, Poland e-mail: jm@.pl 3Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland ABSTRACT We present extensive tables of the Atomic Partition Function for iron ions, Fe I – Fe X, and discuss details of the computational method. Partition functions are given in wide range of temperatures, 103 K T 106 K, and lowering of ionization energy (0.001 eV LIE 5.0 eV). Our APF take into account all energy levels predicted by quantum mechanics, including autoionization levels. The tables can be applied for the computations of model stellar atmospheres and theoretical spectra over all existing spectral and luminosity classes. Our tables are available at .pl/～acta/acta.html (Acta Astronomica Archive), and http://draco.uni.opole.pl/Halenka.html. Key words: Atomic data – Plasmas – Stars: atmospheres 21. Introduction Iron is the most abundant and important heavy element in astrophysical plasmas. Due to its relatively high abundance in solar type composition and low ionization energy, iron ions are important contributors of free electrons in stellar atmospheres of population II at low and moderate effective temperatures (spectral types F and lower). In atmospheres of these types hydrogen and helium atoms remain almost perfectly neutral, and therefore iron donors of free electrons can be critically important for the populations and opacity of negative ions H? and He?, which in turn determine the whole atmospheric structure and visual/infrared spectra of these most numerous classes of stars. Also on the opposite end of the Hertzsprung-Russell diagram, various ions of iron contribute to the stratifica