Stellar and gas dynamical model for tidal disruption events in a quiescent galaxy
A detailed model of the tidal disruption events (TDEs) has been constructed using stellar dynamical and gas dynamical inputs that include black hole (BH) mass M{sub •}, specific orbital energy E and angular momentum J, star mass M{sub ⋆} and radius R{sub ⋆,} and the pericenter of the star orbit r{sub p}(E, J, M{sub •}). We solved the steady state Fokker–Planck equation using the standard loss cone theory for the galactic density profile ρ (r) ∝ r{sup −γ} and stellar mass function ξ(m) where m = M{sub ⋆}/M{sub ⊙} and obtained the feeding rate of stars to the BH integrated over the phase space as N-dot {sub t}∝M{sub ∙}{sup β}, where β=−0.3±0.01 for M{sub •} > 10{sup 7}M{sub ⊙} and ∼6.8 × 10{sup −5} Yr{sup −1} for γ = 0.7. We use this to model the in-fall rate of the disrupted debris, M-dot (E,J,m,t), and discuss the conditions for the disk formation, finding that the accretion disk is almost always formed for the fiduciary range of the physical parameters. We also find the conditions under which the disk formed from the tidal debris of a given star with a super Eddington accretion phase. We have simulated the light curve profiles in the relevant optical g band and soft X-rays for both super and sub-Eddington accretion disks as a function of M-dot (E,J,t). Using this, standard cosmological parameters, and mission instrument details, we predict the detectable TDE rates for various forthcoming surveys as a function of γ.
- OSTI ID:
- 22882380
- Journal Information:
- Astrophysical Journal, Vol. 814, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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