Formation of quasar clouds by thermal instability in the presence of Alfven wave heating

Details Formation of quasar clouds by thermal instability in the presence of Alfven wave heating Formation of quasar clouds by thermal instability in the presence of Alfven wave heating

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...414...57g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 414, no. 1, p. 57-63.

Astronomy and Astrophysics

Astrophysics

20

Clouds, Magnetohydrodynamic Waves, Quasars, Radiative Heat Transfer, Radiative Transfer, Seyfert Galaxies, Thermal Instability, Cooling Flows (Astrophysics), Magnetic Field Configurations, Magnetohydrodynamic Shear Heating, Radiant Cooling, Stellar Atmospheres

Scientific paper

Highly perturbed magnetic field exist in quasars which will produce a large Alfven wave flux. We investigate here the effect of Alfven wave heating on the radiative heating-cooling function of broad-line emitting clouds in quasars with respect to the thermal instability. Jatenco-Pereira & Opher (1989) investigated resonance surface damping of Alfven waves in the atmospheres of young and old stars and the sun, and we study here resonance surface damping of Alfven waves in the region of broad-line emitting clouds in quasars. The radiative heating-cooling function used depends on (1) heating and cooling associated with recombination; (2) radiative losses due to electron excitation of resonance transitions in metal ions; (3) thermal bremsstrahlung; (4) Compton heating-cooling; and (5) Alfven wave heating. We find that a thermal instability can occur at the observed pressure about 0.01 dynes/cm.

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