Astronomy and Astrophysics – Astronomy
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.262..119f&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 262, no. 1, p. 119-127.
Astronomy and Astrophysics
Astronomy
5
B Stars, Hot Stars, Stellar Envelopes, Stellar Oscillations, Variable Stars, Fourier Analysis, Hydrodynamic Equations, Nonadiabatic Conditions, Pulsed Radiation
Scientific paper
Consideration is given to hydrodynamic models of helium stars, with masses of 0.7 and 0.6 solar mass, bolometric magnitudes in the range -4 to -6 mag, and effective temperatures in the range 9000 to 30,000 K. The vertical part of the blue boundary of the pulsation instability region is found to shift from T(eff) of about 7400 to 11,000 K when the stellar mass changes from 1 to 0.7 solar mass. In stars located along the vertical part of the instability region boundary, the pulsation instability is driven by both the kappa and gamma mechanisms, the order of the principal pulsation mode increasing with decreasing luminosity. Stars with T(eff) of not less than 12,000 K are found to be unstable only for L of not less than 12,800 solar luminosities. In stars located along the horizontal part of the instability region boundary, the role of the kappa mechanism decreases with increasing effective temperature, so that for T(eff) of greater than about 20,000 K the pulsations are mostly due to the gamma mechanism.
No associations
LandOfFree
Non-linear radial pulsations of hot extreme helium 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 Non-linear radial pulsations of hot extreme helium stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Non-linear radial pulsations of hot extreme helium stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1682409