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BLUE EGDES of the Delta Scuti instability domain computed with new OP opacities
A. A. Pamyatnykh i T. Zdravkov, Centrum Astronomiczne Mikołaja Kopernika
The evolutionary tracks have been calculated for stellar models
from 1 up to 40 solar masses in the MS and early post-MS evolutionary stages.
For every selected mass between 1.0 and 3.8 MSun, radial oscillations
have been computed using linear nonadiabatic code by W. A. Dziembowski
(Dziembowski 1977).
The computations were performed using new OP opacities (Seaton 2005)
for new solar heavy element mixture referred as A04 (Asplund et al. 2005).
Three heavy element mass fractions were used: Z=0.020, 0.015, 0.010.
One set of the models was computed for older heavy element
mixture GN93 (Grevesse & Noels 1993).
For each Z calculations have been made for
three hydrogen mass fractions: X=0.75, 0.70, 0.65.
The exception is mixture GN93, for which computations
were performed only for X=0.70 and Z=0.020.
In the computations the mixing-length theory of convection with
alpha(conv)=0.5 was used.
One set of computations was performed with alpha(conv)=1.0
(mixture A04, X=0.70, Z=0.02).
All other details of computations are the same as in Pamyatnykh (1999).
BIBLIOGRAFIA:
- Asplund M., Grevesse N., Sauval A.J., 2004, ASP Conf. Ser, 336, 25
- Dziembowski W., 1977, Acta Astronomica, 27, 95
- Grevesse N., Noels A., 1993, in Pratzo M., Vangioni-Flam E., Casse M., eds.,
Origin and Evolution of the Elements,
Cambridge Univ. Press, p. 15
- Pamyatnykh A.A., 1999, Acta Astr., 49, 119
- Pamyatnykh A.A., 2000, ASP Conf. Ser, 210, 215
- Seaton M.J., 2005, MNRAS, 362, L1
Pobierz:
- X = 0.65, Z = 0.010, α = 0.5 (a04)
- X = 0.70, Z = 0.010, α = 0.5 (a04)
- X = 0.75, Z = 0.010, α = 0.5 (a04)
- X = 0.65, Z = 0.015, α = 0.5 (a04)
- X = 0.70, Z = 0.015, α = 0.5 (a04)
- X = 0.75, Z = 0.015, α = 0.5 (a04)
- X = 0.65, Z = 0.020, α = 0.5 (a04)
- X = 0.70, Z = 0.020, α = 0.5 (a04)
- X = 0.70, Z = 0.020, α = 1.0 (a04)
- X = 0.70, Z = 0.020, α = 0.5 (gn93)
- pobierz wszystko
DESCRIPTION OF THE COLUMNS in each oscillation file:
| mod | – | model number |
| l | – | the spherical harmonic degree |
| n | – | number of nodes along radius |
| sig | – | non-dimensional frequency |
| P | – | Period, [days] |
| fa[c/d] | – | adiabatic oscillation frequency in [c/d] |
| fn[c/d] | – | nonadiabatic approximation frequency in [c/d] |
| COMPLEX F | – | ratio of the radiative flux perturbation to the radial displacement |
| ekg/ek | – | ratio of the kinetic energy in the gravity-wave propagation zone to the total kinetic energy |
| eta | – | normalized growth-rate [eta changes between +1 (full driving) and -1 (full damping)] |
| Mass | – | mass of the stellar model [MSun] |
| lg Te | – | log10 (effective temperature, [K]) |
| lg L | – | log10 (surface luminosity, [LSun]) |
| lg g | – | log10 (effective gravity, [c.g.s]) |
| Vrot | – | rotational velocity [km/s] (=0.0 in these computations) |
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