In this study, vibrational properties and stability of delta-Scuti
like pulsating pre-main sequence stars have been investigated.
Studies were held in the mass range 2-4 Mo
and limited to radial linear adiabatic pulsations. Numerical computations were performed by the
oscillation
program written by Kirbiyik & / Al-Murad (1993). The models were selected to be at the latest phases
of the pre-main sequence evolution where the luminosity starts to increase.
We have limited our calculations upto the end of the radiative inner regions, since at the surface of
the star, our adiabatic perturbation computation does not perfectly fit to the relatively thin
non-adiabatic convective envelope of the star. The results of the stability analysis showed that the
PMS models undergo an instability whose time period is a function of mass.
Instability Strip of pulsating PMS stars
was re-drawn with comparison
to
M. Marconi & / F.Palla (1998). The effect of gravitational contraction
on stability was also investigated.
| Identifer | oai:union.ndltd.org:METU/oai:etd.lib.metu.edu.tr:http://etd.lib.metu.edu.tr/upload/12604705/index.pdf |
| Date | 01 February 2004 |
| Creators | Burhan, Mehmet |
| Contributors | Kiziloglu, Nilgun |
| Publisher | METU |
| Source Sets | Middle East Technical Univ. |
| Language | English |
| Detected Language | English |
| Type | M.S. Thesis |
| Format | text/pdf |
| Rights | To liberate the content for public access |
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