Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...351..103f&link_type=abstract
Astronomy and Astrophysics, v.351, p.103-118 (1999)
Astronomy and Astrophysics
Astrophysics
29
Hydrodynamics, Methods: Numerical, Stars: Oscillations, Stars: Variables: Rr Lyr
Scientific paper
The Vienna nonlinear convective pulsation code is applied to the case of RR Lyrae stars. Assuming two sets of stellar parameters (M = 0.65 Msun, L = 52.5 Lsun, Z = 0.001 and M = 0.75 Msun, L = 52.5 Lsun, Z = 0.0001) we compute fundamental and first overtone limit cycle solutions for effective temperatures ranging from 6000 to 7100 K. The resulting light- and radial velocity curves are compared in detail with corresponding models in the literature and with recent observations. As main result, the light curve morphology is in good agreement with observed RR Lyrae light curves. In particular the theoretical light curve Fourier parameters up to the fifth order lie almost completely within the observed ranges, which means that we are able to resolve the well known RR Lyrae phase discrepancy problem. Regarding the radial velocity variations deviations from observed Fourier parameters occur. Possible explanations like the calibration of the turbulent convection model or the transformation from theoretical to observed radial velocities are discussed.
No associations
LandOfFree
A nonlinear convective model of pulsating stars. II. RR Lyrae stars 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 A nonlinear convective model of pulsating stars. II. RR Lyrae stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A nonlinear convective model of pulsating stars. II. RR Lyrae stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1282602