Avoided crossings between non-radial modes in low mass RGB stars

doi:10.1088/1674-4527/12/12/007

YNAO OpenIR > 恒星物理研究组

	Avoided crossings between non-radial modes in low mass RGB stars
	Guo JJ(郭军军)1,2,3 ; Li Y(李焱)1,2 ; Lai XJ(赖祥军)1,2 ; Guo, JJ (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
发表期刊	RESEARCH IN ASTRONOMY AND ASTROPHYSICS
	2012-12
卷号	12 期号:12 页码:1655-1665
DOI	10.1088/1674-4527/12/12/007
产权排序	第1完成单位
收录类别	SCI
关键词	Stars: Oscillations Stars: Red Giants
摘要	Non-radial p modes and g modes appear simultaneously in red giant stars. Their frequencies have different variation rates, causing their frequencies to become close during stellar evolution so that avoided crossings appear. The separation between regions where acoustic waves and gravity waves propagate for l = 1, 2 and 3 is different, which results in the coupling efficiency also being different. We present the results of numerical computations of the models we study. We find that the two kinds of modes for l = 2 and 3 need to be closer in frequency in order for a complete exchange to occur, compared to the case for modes with l = 1. Their scaled oscillation frequencies also present better regularity with evolution than modes with l = 1. In order to study the effect of the avoided crossings in detail, we set the mode which has the smallest mode inertia to be the p mode. We plot the two kinds of modes for l = 1, 2 and 3 in frequency and period echelle diagrams and find modes of l = 2 and 3 fit the two relations better; they are more equally spaced in frequency and period than modes with l = 1. Under careful observation of the two kinds of echelle diagrams for l = 2 and 3, we still find that some p modes shift a little from being equally spaced in frequency and some g modes, which are close to those p modes in period, shift a little from being equally spaced in period. Then, we study the relation between the deviation from period being equally spaced and the mode inertia of g modes for different l. The g modes of l = 1 with a period closer to the p mode have less inertia and the deviation is bigger in the period echelle diagram. Their deviation is also obvious. However g modes of l = 2 and 3 shift a little or have almost no deviation from being equally spaced in period, even though some of them may have strong coupling and close mode inertia like in the p modes. So, we suggest a possible method for measuring period spacing of g modes precisely using mixed g modes with l = 2 and 3 that have fewer observed mixed g modes than for l = 1.
项目资助者	National Natural Science Foundation of China [10973035, 10673030] ; Knowledge Innovation Key Program of the Chinese Academy of Sciences [KJCX2-YW-T24] ; Yunnan Natural Science Foundation [Y1YJ011001]
语种	英语
学科领域	Astronomy & Astrophysics
文章类型	Article
ISSN	1674-4527
URL	查看原文
归档日期	2012-12-10
WOS记录号	WOS:000313011000007
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	SOLAR-LIKE OSCILLATIONS ; MAIN-SEQUENCE STARS ; RED GIANTS ; STELLAR OSCILLATIONS ; GRAVITY MODES ; KEPLER ; ASTEROSEISMOLOGY ; AMPLITUDES ; OPACITIES ; EQUATION
引用统计
文献类型	期刊论文
条目标识符	http://ir.ynao.ac.cn/handle/114a53/5212
专题	恒星物理研究组中国科学院天体结构与演化重点实验室
通讯作者	Guo, JJ (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
作者单位	1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China 2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China 3.Graduate University of Chinese Academy of Sciences, Beijing 100049, China
第一作者单位	中国科学院云南天文台
推荐引用方式 GB/T 7714	Guo JJ,Li Y,Lai XJ,et al. Avoided crossings between non-radial modes in low mass RGB stars[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2012,12(12):1655-1665.
APA	Guo JJ,Li Y,Lai XJ,&Guo, JJ .(2012).Avoided crossings between non-radial modes in low mass RGB stars.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,12(12),1655-1665.
MLA	Guo JJ,et al."Avoided crossings between non-radial modes in low mass RGB stars".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 12.12(2012):1655-1665.

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