Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-02-15
Mon.Not.Roy.Astron.Soc. 350 (2004) 277
Astronomy and Astrophysics
Astrophysics
To appear in MNRAS. 11 pages, 11 figures
Scientific paper
10.1111/j.1365-2966.2004.07644.x
Intermediate degree modes of the solar oscillations have previously been used to determine the solar helium abundance to a high degree of precision. However, we cannot expect to observe such modes in other stars. In this work we investigate whether low degree modes that should be available from space-based asteroseismology missions can be used to determine the helium abundance, Y, in stellar envelopes with sufficient precision. We find that the oscillatory signal in the frequencies caused by the depression in \Gamma_1 in the second helium ionisation zone can be used to determine the envelope helium abundance of low mass main sequence stars. For frequency errors of 1 part in 10^4, we expect errors \sigma_Y in the estimated helium abundance to range from 0.03 for 0.8M_sun stars to 0.01 for 1.2M_sun stars. The task is more complicated in evolved stars, such as subgiants, but is still feasible if the relative errors in the frequencies are less than 10^{-4}.
Antia H. M.
Basu Sarbani
Demarque Pierre
Mazumdar Anwesh
No associations
LandOfFree
Asteroseismic determination of helium abundance in stellar envelopes does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Asteroseismic determination of helium abundance in stellar envelopes, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Asteroseismic determination of helium abundance in stellar envelopes will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-680162