边缘耀斑中HeI 10830的加宽计算  

Broadening Calculation of HeI 10830  Line in Solar Limb Flare

作　　者：黎辉[1] 尤建圻[2] 

机构地区：[1]中国科学院紫金山天文台,南京210008 [2]中国科学院国家天文台,北京100012

出　　处：《天文学报》2002年第1期41-47,共7页Acta Astronomica Sinica

基　　金：国家自然科学基金(NSFC)项目(编号49990451);国家重点基础研究规划项目(编号G2000078402)

摘　　要：讨论了 ＨｅＩ １０８３０Ａ的 Ｄｏｐｐｌｅｒ和 Ｓｔａｒｋ加宽机制以及各种加宽参数的计算，并 得到以下一些结论：辐射阻尼对 ＨｅＩ １０８３０ Ａ的加宽作用与 Ｄｏｐｐｌｅｒ效应相比可以忽略； 在公认的耀斑电子密度（Ｎｅ＝３．２ ×１０１３ｃｍ－３）的情况下，所有阻尼项均不可能产生可以 觉察的加宽；直到 Ｎｅ＝１０１５ｃｍ－３，各种阻尼对线心半宽的增加都不起作用，其值最多 在１０－３的量级，因此；线心都可以看作是Ｄｏｐｐｌｅｒ加宽；当 Ｎｅ＞１０１４ ｃｍ－３时，Ｓｔａｒｋ 加宽，特别是电子碰撞的 Ｓｔａｒｋ加宽将在 ＨｅＩ １０８３０ Ａ的加宽中起主要作用；如要 Ｓｔａｒｋ 加宽谱线的线翼比纯Ｄｏｐｐｌｅｒ加宽大１－２倍，则阻尼加宽半宽与。可以相比拟；如果 用 Ｓｔａｒｋ加宽来解释 １９８９年边缘耀斑的观测轮廓，则电子密度将达１０～（１７）ｃｍ－３，与氦 原子的碰撞阻尼（γ３）造成的加宽对Ｉ１２和Ｉ３两分量明显不同，它们对Ｉ１２的影响比对Ｉ３ 的影响大近一个量级，我们的观测显示Ｉ１２和Ｉ３线翼的延伸基本一样，因而我们的观测The Doppler broadening, Stark broadening and various kinds of broadening parameters of HeI 10830 A line in solar flare are calculated and discussed and consequently the following results are got: radiation damping can be neglected when compared with Doppler broadening, and in the case of generally accepted electron density in a solar flare (Ne= 3.2 ×1013 cm3 ), all the damping terms will not lead to distinguishable broadening in the HeI 10830 A profile. All the damping effects will not result in discernible increment of the half width of HeI 10830 A until the electron density reaches to 1015 cm3 when the largest increment is about 10-3A. Therefore. the line center of HeI 10830 A line can be taken as Doppler broadening. When electron density is greater than 1014 cm3 , Stark broadening, especially that by electron collisicn, will play a major role in the broadening of HeI 10830 A line. In order for the half width of the line resulted from Stark broadening to be 1-2 times greater than that from Doppler broadening, the half width from damping effect will be equivalent to that from Doppler effect. Consequently, the electron density will be of the order of 1017 cm3 if we interpret the observed HeI 10830 A profiles in the 1989 limb flare by Stark broadening. Broadening effect caused by collision with helium atom (γ3) has different impact on I12 and I3 component. The impact on I12 is about one order greater than that on 13. The observed HeI 10830 A profiles of 1989 limb flare show that I12 and I3 have almost the same extended profile, therefore, they can not result from γ3.

关 键 词：太阳 耀斑 谱线加宽 激发 电离 氢线 加宽机制 

分 类 号：P182.52[天文地球—天文学]