Disk Instability Model for the AM Canum Venaticorum Stars

Details Disk Instability Model for the AM Canum Venaticorum Stars Disk Instability Model for the AM Canum Venaticorum Stars

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasj...49...75t&link_type=abstract

Publications of the Astronomical Society of Japan, v.49, p.75-84.

Astronomy and Astrophysics

Astronomy

47

Accretion Disks, Instabilities, Stars: Am Cvn Stars, Stars: Cataclysmic

Scientific paper

We examine AM CVn stars, ultra-short-period variables thought to have helium disks, from the standpoint of the disk instability model. By calculating the vertical structure of the helium accretion disks, we have confirmed that the helium accretion disks are thermally unstable, since their thermal-equilibrium curves exhibit the characteristic S-shaped form. We apply these results to AM CVn stars. We have found that the observed large-amplitude photometric variations in AM CVn stars can be explained by the thermal-tidal instability model of helium accretion disks.

Affiliated with

Also associated with

No associations

Rating

Disk Instability Model for the AM Canum Venaticorum 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 Disk Instability Model for the AM Canum Venaticorum Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Disk Instability Model for the AM Canum Venaticorum Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1607193