Blue loops of intermediate mass stars - II. Metallicity and blue loops

	Blue loops of intermediate mass stars - II. Metallicity and blue loops
	Xu HY(许华崟)1 ; Li Y(李焱)1,2
刊名	ASTRONOMY & ASTROPHYSICS
	2004-04
卷号	418 期号:1 页码:225-233
关键词	stars : evolution stars : interiors stars : Hertzsprung-Russell (HR) and C-M diagrams
ISSN号	0004-6361
通讯作者	Xu, HY (reprint author), Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
产权排序	第一完成单位
英文摘要	Based oil the results of the blue loop formation for models of solar-like metallicity, we have explored the blue loop evolution of metal-poor stars. Three series of models with a wide ran.-c of metallicity and the initial helium abundance were calculated. An important parameter, eta(c), defined as the envelope convection mass divided by the total envelope mass at the bottom of the RGB. was introduced as a criterion to determine the formation of the blue loop. We have found that the low-Z models will develop extensive blue loops when eta(c) is lower than a critical value eta(crit). The physical explanation for this result Could be as follows. Lower Z reduces the envelope opacity and leads to a hotter stellar envelope and a bluer RGB. Thus file model will have a smaller eta(a) at the top and an even smaller eta(c) at the bottom of the RGB. When eta(c) is lower than the critical value eta(crit), the envelope is radiation-dominated. Under this condition and the constraint of the virial theorem, the response of the star to the increase of the stellar luminosity is to contract to increase the thermal conductivity coefficient in the stellar envelope and to form a blue loop. Compared with the high-Z models, we have confirmed that the development of convection in the stellar envelope is a crucial factor to determine the formation of the blue loop, but the low-Z models reach low eta(c) values in a different way from the high-Z models. in which the modulation of the nuclear reaction rates by higher N-14 abundance in the H-burning shell is responsible for the stars to get small eta(c) values. It has been found that eta(crit) depends not only on the stellar mass, but also on metallicity and the initial helium abundance. Our numerical results show that eta(crit) decreases with Z while slowly increases with Y.
学科主题	Astronomy & Astrophysics
WOS标题词	Science & Technology ; Physical Sciences
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	STELLAR MODELS ; EVOLUTION ; HELIUM ; OPACITIES ; ABUNDANCES ; SOLAR
收录类别	SCI ; EI
原文出处	http://www.aanda.org/articles/aa/abs/2004/16/aa3972/aa3972.html
语种	英语
WOS记录号	WOS:000221299500027
内容类型	期刊论文
源URL	[http://ir.ynao.ac.cn/handle/114a53/5173]
专题	云南天文台_恒星物理研究组
作者单位	1.National Astronomical Observatories/Yunnan Observatory, PO Box 110, 650011 Kunming, PR China 2.Joint Laboratory for Optical Astronomy, Chinese Academy of Sciences, PR China
推荐引用方式 GB/T 7714	Xu HY,Li Y. Blue loops of intermediate mass stars - II. Metallicity and blue loops[J]. ASTRONOMY & ASTROPHYSICS,2004,418(1):225-233.
APA	Xu HY,&Li Y.(2004).Blue loops of intermediate mass stars - II. Metallicity and blue loops.ASTRONOMY & ASTROPHYSICS,418(1),225-233.
MLA	Xu HY,et al."Blue loops of intermediate mass stars - II. Metallicity and blue loops".ASTRONOMY & ASTROPHYSICS 418.1(2004):225-233.