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For refcode 1993MNRAS.263..323T:
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Copyright by Royal Astronomical Society. 1993MNRAS.263..323T Elliptical galaxy cooling flows without mass drop-out Gavin Tabor and James Binney Theoretical Physics, Keble Road, Oxford OX1 3NP Accepted 1993 January 18. Received 1993 January 18; in original form 1992 September 14 ABSTRACT The existence of a hot X-ray emitting gas phase in giant elliptical galaxies has long been recognized, but its structure and dynamics are still controversial. We explore the possibility that the gas is heated from below, causing it to convect. This leads to a two-component model in which a cooling flow feeds into an adiabatic core. The heat source for this core is taken to be the central black hole. The model is applied to the three galaxies with the best data from the Einstein observatory: NGC 4472,4636 and 4649. In our models of NGC 4636, gas flows inwards at all radii, while in NGC 4472 and 4649 the flow is directed outwards at large radii. Consequently, the adiabatic core of NGC 4636 is significantly larger and more luminous than those of NGC 4472 and 4649. The time-averaged luminosity that should be generated by accretion of the core's gas on to a central massive black hole is of the order of that required to enable the core to swell and accommodate most of the gas fed to it by the enveloping flow. However, one expects the nuclear luminosity to be intermittent, and observations suggest that the nuclei of all three galaxies are dormant at the present epoch Key words: cooling flows - galaxies: individual: NGC 4472 - galaxies: individual NGC 4636 - galaxies: individual: NGC 4649 - galaxies: ISM - X- rays: galaxies
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