Evolution of a primordial black hole inside a rotating solar-type star

Details Evolution of a primordial black hole inside a rotating solar-type star Evolution of a primordial black hole inside a rotating solar-type star

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277...25m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 25-35.

Physics

5

Accretion, Accretion Discs, Black Hole Physics, Stars: Evolution

Scientific paper

We study the accretion-driven evolution of a primordial black hole at the centre of the Sun or any solar-type star. We show that, if the star's rotation is small enough for the accretion to be radial, then the black hole grows at the fast `Bondi' rate [so the remaining life of the star is 50(M_solar/M)s when the hole's mass is M], and the flow produces luminosity at the rather low `Flammang' level [L_F1=2.5x10^34(M/M_solar) erg s^-1]. As a result, the growing hole has no influence on the star's external appearance until tens of minutes before it completely destroys the star. We also examine the effects of a solar-like rotation. If the inflowing fluid elements retain their angular momentum, the accretion will centrifugally hang up and form an `accretion torus' near the growing hole, until the hole's mass, M, reaches M_+=10^-3M_solar thereafter, the inflow will be radial. We show that, when M_v=10^-11 M_solar, molecular viscosity removes angular momentum fast enough to prevent such an accretion torus forming. Similarly, magnetic torques preclude the formation of a torus when M_B=6x10^-8B^3/4_0M_solar, where B_0 is the magnetic field strength at the star's centre. For M above these regimes but below M_+, an accretion torus probably does form, and may increase the luminosity L above L_Fl and slow the flow M_solar below Bondi. However, until at most 3d before the star is destroyed, L cannot increase by more than about an order of magnitude, because a higher L would produce strong convection outside the accretion torus and the resulting turbulent viscosity would remove so much angular momentum from the flow as to prevent the torus from forming in the first place. As a corollary, the `solar neutrino problem' cannot be solved by postulating a small black hole at the Sun's centre.

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