Hot coronas of galaxies: the effects of a dark halo, the intergalactic medium, and heat conduction

Journal Article · Fri Jul 01 04:00:00 EDT 1988 · Astrophysics (Engl. Transl.); (United States)

DOI:https://doi.org/10.1007/BF01014848· OSTI ID:6069002

Suchkov, A A; Berman, V G

The dynamics of hot coronas of galaxies is studied by numerical solution of the nonlinear equations of gas dynamics for a series of corresponding models. It is shown that the observed coronas may represent relics of a hot protogalaxy that have hardly changed in approx.10/sup 9/ yr after the initial phase of rapid evolution. A quasisteady state and retention of coronas in a galaxy can be assured equally effectively by either the field of the hidden mass of a dark halo or by the pressure of the hot intergalactic medium. These two factors can be distinguished observationally by means of the temperature profile in the corona, which is different for these cases. It is concluded that the coronas and the intergalactic medium cannot be heat conducting - it was found that in such a case the coronas either rapidly disappear or, in disagreement with observations, rapidly acquire the temperature of the hot intergalactic gas.

• Research Organization: Rostov State Univ. (USSR)
• OSTI ID: 6069002
• Journal Information: Astrophysics (Engl. Transl.); (United States), Journal Name: Astrophysics (Engl. Transl.); (United States) Vol. 28:1; ISSN ATPYA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC ELECTRONS
COSMIC GASES
COSMIC RADIATION
COSMOLOGICAL MODELS
ELECTRON TEMPERATURE
ELECTRONS
ELEMENTARY PARTICLES
ENERGY TRANSFER
ERUPTIVE VARIABLE STARS
FERMIONS
FLUID FLOW
FLUID MECHANICS
FLUIDS
FUNCTIONS
GALACTIC EVOLUTION
GALAXIES
GALAXY NUCLEI
GAS FLOW
GASES
GRAVITATIONAL FIELDS
HEAT TRANSFER
HYDRODYNAMICS
INTERGALACTIC SPACE
IONIZING RADIATIONS
LAGRANGIAN FUNCTION
LEPTONS
MATHEMATICAL MODELS
MECHANICS
NEBULAE
NUMERICAL SOLUTION
PHYSICAL PROPERTIES
PRESSURE EFFECTS
RADIATIONS
SPACE
STARS
SUPERNOVAE
TEMPERATURE DISTRIBUTION
THERMAL CONDUCTIVITY
THERMODYNAMIC PROPERTIES
VARIABLE STARS
VELOCITY