Vibrational instability of a 1 solar mass star towards non-radial oscillations

Details Vibrational instability of a 1 solar mass star towards non-radial oscillations Vibrational instability of a 1 solar mass star towards non-radial oscillations

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....41..279b&link_type=abstract

Astronomy and Astrophysics, vol. 41, no. 3-4, July 1975, p. 279-285.

Astronomy and Astrophysics

Astrophysics

61

Dynamic Stability, Main Sequence Stars, Stellar Evolution, Vibration Mode, Astronomical Models, Chemical Composition, Gravitational Collapse, Perturbation Theory

Scientific paper

Vibrational stability is analyzed for nonradial adiabatic oscillations of a star of one solar mass during the main-sequence phase. Stellar evolution from gravitational contraction to the main-sequence phase is computed by the Henyey method, and the analysis is conducted using the Lagrangian formalism. The analysis indicates that the star becomes unstable at an age of 240 million years and that stability is restored after three billion years.

Affiliated with

Also associated with

No associations

Rating

Vibrational instability of a 1 solar mass star towards non-radial oscillations 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 Vibrational instability of a 1 solar mass star towards non-radial oscillations, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Vibrational instability of a 1 solar mass star towards non-radial oscillations will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1754529