Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...318..629w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 15, 1987, p. 629-644.
Astronomy and Astrophysics
Astrophysics
50
Cooling, Cooling Flows (Astrophysics), Galactic Clusters, Magnetohydrodynamic Flow, Star Formation, Stellar Models, X Ray Sources, Galactic Structure, Intergalactic Media, Star Distribution, Thermal Instability
Scientific paper
At the center of each observed X-ray cluster cooling flow is a central dominant galaxy accreting up to several hundred solar masses per year from the flow. Here, the authors calculate theoretical models of such flows, including the effects of ongoing star formation. They relate the local star formation rate in these models to either the local cooling rate of the gas or the local growth rate of thermal instabilities. It is shown how the structure of cooling flows is affected by variations in the star formation rate, as well as by variations in intracluster temperature, overall accretion rate, elemental abundances, and the form of the gravitational potential. The authors also calculate the X-ray emission from these models.
Sarazin Craig L.
White Raymond Edwin III
No associations
LandOfFree
Numerical models of star formation in X-ray cluster cooling flows 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 Numerical models of star formation in X-ray cluster cooling flows, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical models of star formation in X-ray cluster cooling flows will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-789735