摘要
从1974 年起,基特峰天文台几乎每月定期对太阳大气的K 线及其他一些谱线进行观测记录.以往对K 线的研究表明:K1 形成于温度极小区(TMR) ,K1 到线心的距离以及K1 的强度分别与温度极小区的位置和温度密切相关.对基特峰K 线轮廓的有关数据以及最近数十年的太阳黑子数进行了研究,发现:全日面K 线轮廓的K1 到线心的距离随时间的变化与太阳黑子数的变化是同步的,而对于日面中心( 可视为宁静太阳) 的K 线轮廓而言,K1到线心的距离及其强度的变化相对于太阳黑子数的变化表现出一种可能的相位滞后;粗略的估算表明宁静太阳大气温度极小区的温度在一个太阳周的变幅为30 K～50 K.
Calcium K line as well as some other solar spectral lines have been measured regularly nearly every month since 1974 at Kitt Peak. It is now widely accepted that K 1 is formed in the temperature minimum region (TMR) and that the distance of the component K 1 from the line center and the intensity of K 1 is well related to the position and temperature of TMR, respectively. The author's study on the data of K line profiles and on the sunspot numbers over decades shows: In full disc integrated spectra the distance of K 1 from the line center fluctuates in the same way as the sunspot numbetr does, indicating a solar cyclic variation. In disc center spectra, basically for quiet sun atmosphere, the distance of K 1 from the line center and its intensity also show periodical variations, but there is a time delay with respect to the sunspot number. Rough estimation yields a temperature variation of about 30～50 K of TMR in the quiet sun atmosphere.
出处
《天文学报》
CSCD
北大核心
2000年第1期44-50,共7页
Acta Astronomica Sinica
基金
国家自然科学基金委资助
教育部博士点基金
关键词
太阳
大气
温度变化
周期性变化
极小区
solar cycle variation, CaII K line profile, temperature minimum region
