Tidal compression of a star by a large black hole. I Mechanical evolution and nuclear energy release by proton capture

Details Tidal compression of a star by a large black hole. I Mechanical evolution and nuclear energy release by proton capture Tidal compression of a star by a large black hole. I Mechanical evolution and nuclear energy release by proton capture

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...121...97c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 121, no. 1, May 1983, p. 97-113.

Astronomy and Astrophysics

Astrophysics

68

Black Holes (Astronomy), Capture Effect, Gravitational Effects, Nuclear Fusion, Stellar Atmospheres, Stellar Evolution, Galactic Nuclei, Lagrangian Equilibrium Points, Nuclear Astrophysics, Protons, Roche Limit, Stellar Models, Stellar Temperature

Scientific paper

The gross qualitative behaviour of a star plunging deeply within the Roche tidal radius, RR, of a large black hole to a pericentre radius β-1RR, with β≳3, is examined using a simplified affine star model whose evolution is canonically determined by a Lagrangian formalism. In Phase I, for R≳RR, the star remains in only slightly distorted self-gravitating quasi-equilibrium, but in Phase II its particles undergo approximately free fall in the strong external tidal field within the Roche radius. In Phase III the compression is halted and reversed by the build-up of pressure in a highly flattened pancake configuration, in which adiabatic heating raises the temperature to a maximum given in most cases by Θm ≍ β-2Θ* where Θ* is the equilibrium core temperature. In Phase IV the matter expands again in approximately free fall, and in Phase V, as the star moves outside the Roche radius, pressure and self-gravitational forces again come into play. For stars rich in intermediate weight elements, nuclear energy release by proton capture in Phase III is shown to be important. Consideration of the more spectacular possibility of helium detonation is postponed until Part II.

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