Accretion and wind solutions with a variable adiabatic index and the possibilities of shock

Details Accretion and wind solutions with a variable adiabatic index and the possibilities of shock Accretion and wind solutions with a variable adiabatic index and the possibilities of shock

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011cqgra..28w5004m&link_type=abstract

Classical and Quantum Gravity, Volume 28, Issue 23, pp. 235004 (2011).

Astronomy and Astrophysics

Astronomy

Scientific paper

Using the relativistic equation of state (EOS) in which the adiabatic index γ varies smoothly from \frac{5}{3}\rightarrow \frac{4}{3} as a function radius (Basu and Mondal 2011 arXiv:1103.3330 [astro-ph]), we review accretion and wind solutions once again. We find that except for the region very near the compact object, γ does not change significantly from its non-relativistic value and therefore the EOS mostly remains non-relativistic in nature. As a consequence, the existence of two saddle-type critical points becomes a rare possibility indicating that it is an artifact of the choice of the constant ultrarelativistic \gamma\; (=\frac{4}{3}). Therefore, the formation of shocks in the flow (which requires the presence of two saddle-type points) becomes very unlikely.

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