关于恒星大气超声对流的注释  

A Note on Supersonic Convection in Stellar Atmosphere

作　　者：熊大闰[1] 邓李才[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》2011年第3期177-179,共3页Acta Astronomica Sinica

基　　金：国家自然科学基金项目(11073053;10973015)资助

摘　　要：1引言 尽管有诸多的不满之处，由于其物理上的直观性和应用上的简单性，至今混合长理论仍几乎是唯一一个广泛用于恒星结构、演化和脉动计算的恒星对流理论．混合长理论预言，在红、黄巨星和超巨星大气中，对流是超声速的．我们曾指出，Using a non-local convection theory, both of the local and non-local convective envelope models of evolutionary series of stars with masses from 1 to 30 solar masses are calculated. The problem of supersonic convection is reviewed. The results show that convective velocities in the stellar atmosphere are seriously overestimated by the local mixing-length theory. Convection is strong supersonic in the atmosphere of yellow giants and super-giants in the local mixing-length theory. They, however, become subsonic for the most stars when convection is return to the normal non-local treatment. Convective velocities increase with the increases of the luminosities of stars. There are still weak supersonic convection in few red and yellow giants and super-giants. It is suspected whether this supersonic convection in the stellar atmosphere is true.

关 键 词：对流 恒星 大气 

分 类 号：P152[天文地球—天文学]