2007
DOI: 10.1051/0004-6361:20077082
|View full text |Cite
|
Sign up to set email alerts
|

The frequency separations of stellar p-modes

Abstract: Aims. The purpose of this work is to investigate the characteristics of a new frequency separation of stellar p-modes. Methods. Frequency separations are deduced from the asymptotic formula of stellar p-modes. Then, using the theoretical adiabatic frequencies of stellar model, we compute the frequency separations. Results. A new separation σ l−1l+1 (n), which is similar to the scaled small separation d ll+2 (n)/(2l + 3), is obtained from the asymptotic formula of stellar p-modes. The separations σ l−1l+1 (n) a… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
5

Citation Types

0
11
0

Year Published

2009
2009
2022
2022

Publication Types

Select...
8

Relationship

1
7

Authors

Journals

citations
Cited by 10 publications
(11 citation statements)
references
References 34 publications
0
11
0
Order By: Relevance
“…When seeking to probe the internal structures of stars with low-l p-modes, the small separations, d 10 , d 01 , d 02 , and d 13 , and the ratios of the small separations to the large separations, r 10 , r 01 , r 02 , and r 13 (Roxburgh & Vorontsov 2003;Yang & Bi 2007b, and references therein), are considered to be the very useful diagnostic tools. The small separations d 10 and d 01 are defined as (Roxburgh & Vorontsov 2003) d 10 (n) = − 1 2 (−ν n,0 + 2ν n,1 − ν n+1,0 )…”
Section: Introductionmentioning
confidence: 99%
“…When seeking to probe the internal structures of stars with low-l p-modes, the small separations, d 10 , d 01 , d 02 , and d 13 , and the ratios of the small separations to the large separations, r 10 , r 01 , r 02 , and r 13 (Roxburgh & Vorontsov 2003;Yang & Bi 2007b, and references therein), are considered to be the very useful diagnostic tools. The small separations d 10 and d 01 are defined as (Roxburgh & Vorontsov 2003) d 10 (n) = − 1 2 (−ν n,0 + 2ν n,1 − ν n+1,0 )…”
Section: Introductionmentioning
confidence: 99%
“…Although only a very limited number of modes ( l ≤ 3) are likely to be observed in solar‐like oscillations due to geometrical cancellation effects, the low‐degree p modes of the oscillations can penetrate deep into the interiors of stars (Dziembowski & Goode 1997) and each low‐degree p mode carries unique information about the stellar interior. Thus, asteroseismology has the capability to probe the interior of stars and to determine stellar fundamental parameters (Ulrich 1986; Gough 1987; Kjeldsen & Bedding 1995; Christensen‐Dalsgaard 2002; Yang & Bi 2007; Stello et al 2009a,b; Kallinger et al 2010a,b; Mosser et al 2010; Yang & Meng 2010).…”
Section: Introductionmentioning
confidence: 99%
“…Fortunately, Δν and ν max also allow us to determine the fundamental parameters of stars (mass and radius) to within a few percent (Kjeldsen & Bedding 1995; Stello et al 2009a,b). Moreover, the properties of frequency separations have been studied by many investigators (Ulrich 1986; Gough 1987; Gabriel 1989; Roxburgh & Vorontsov 2000; Yang & Bi 2007; Yang & Meng 2009). Asteroseismic parameters Δν and ν max will be the primary parameters for asteroseismology.…”
Section: Introductionmentioning
confidence: 99%