Testing turbulent convection theory in solar models - II. Solar p-mode oscillations

	Testing turbulent convection theory in solar models - II. Solar p-mode oscillations
	Yang JY(杨家艳)1,2 ; Li Y(李焱)1
刊名	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
	2007-02-11
卷号	375 期号:1 页码:403-414
关键词	convection turbulence Sun : helioseismology Sun : interior
ISSN号	0035-8711
通讯作者	Yang, JY (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, POB 110, Kunming 650011, Peoples R China.
产权排序	第一完成单位
英文摘要	The free parameters involved in the turbulent convection models are determined in the solar interior with the aid of helioseismology. We calculated solar p-mode oscillation l = 150 for a series of solar models described by Li & Yang, and compared the calculated frequencies with the helioseismic observations. It is found that, with appropriate choices of the turbulent parameters, solar model with both local and non-local turbulent convection models can give the calculated p-mode frequencies that are better consistent with the observations than the standard solar model does. The turbulent dissipation plays a major role in the frequency corrections, while the turbulent diffusion makes further improvements in the frequencies. Decreasing the values of parameters C-t and C-e or increasing the values of C-t1 and C-e1 helps reduce the calculated frequencies, indicating that the turbulent dissipation is weak and the turbulent diffusion is strong in the convection zone of the Sun. The parameters C-k and C-s have no obvious effect on the p-mode frequencies. The temperature is found to have a bump near the surface of the convection zone and a mild depression over the inner convection zone. It is just this temperature depression that makes the sound speed a little less, and the p modes spending a little longer time to travel in the convection zone. Combined with better values of the free parameters, our solar models with the TCMs can reduce the frequency differences between the model calculations and observation as much as 30 per cent for the modes of middle and high l. This result can give a clue to solar modelling, i.e., including turbulence in solar models is helpful to reproduce the observed solar p-mode frequencies.
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]	HELIOSEISMOLOGY ; INTERIOR ; STARS
收录类别	SCI
原文出处	http://mnras.oxfordjournals.org/content/375/1/403
语种	英语
WOS记录号	WOS:000243910500047
内容类型	期刊论文
源URL	[http://ir.ynao.ac.cn/handle/114a53/5188]
专题	云南天文台_恒星物理研究组
作者单位	1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming 650011, China 2.Graduate School of Chinese Academy of Sciences, Beijing 100039, China
推荐引用方式 GB/T 7714	Yang JY,Li Y. Testing turbulent convection theory in solar models - II. Solar p-mode oscillations[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2007,375(1):403-414.
APA	Yang JY,&Li Y.(2007).Testing turbulent convection theory in solar models - II. Solar p-mode oscillations.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,375(1),403-414.
MLA	Yang JY,et al."Testing turbulent convection theory in solar models - II. Solar p-mode oscillations".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 375.1(2007):403-414.