Hostname: page-component-848d4c4894-m9kch Total loading time: 0 Render date: 2024-05-02T20:19:40.860Z Has data issue: false hasContentIssue false
  • English
  • Français

Black hole demographics from TDE modeling

Published online by Cambridge University Press:  07 April 2020

T. Mageshwaran  and
A. Mangalam Open the ORCID record for A. Mangalam [Opens in a new window]
T. Mageshwaran
Affiliation:
Tata Institute of Fundamental Research, Mumbai, India email: t.mageshwaran@tifr.res.in
A. Mangalam
Affiliation:
Indian Institute of Astrophysics, Bangalore, India email: mangalam@iiap.res.in
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The occurence rate of tidal disruption events (TDEs) by survey missions depend on the black hole mass function of the galaxies, properties of the stellar cusp and mass of the central black hole. Using a power law density profile with Kroupa mass function, we solve the steady state Fokker-Planck to calculate the theoretical capture rate of stars by the black hole. Using a steady accretion model, the Schechter black hole mass function (BHMF) and the cosmological parameters, we calculate the detection rate of TDEs for various surveys which is then fit with the observed TDE rates to extract the Schechter parameters. The rate tension between observation (∼10−5yr−1) and theory (∼10−4yr−1 for individual galaxies is explained by the statistical average over the BHMF.

Keywords

galaxies: nucleigalaxies: luminosity functionmass functionGalaxy: kinematics and dynamicsgalaxies: statistics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S342: Perseus in Sicily: From Black Hole to Cluster Outskirts , May 2018 , pp. 260 - 262
Copyright
© International Astronomical Union 2020

References

Bardeen, J. M., Press, W. H., & Teukolsky, S. A. 1972, ApJ, 178, 347CrossRefGoogle Scholar
Chen, Y.-M., Wang, J.-M., & Zhang, F. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 373, 667Google Scholar
Donley, J. L., Brandt, W. N., Eracleous, M., & Boller, T. 1995, AJ, 124, 1308CrossRefGoogle Scholar
Ferrarese, L., & Ford, H. 2005, Space Science Reviews, 116, 523CrossRefGoogle Scholar
Kroupa, P. 2001, MNRAS, 322, 23110.1046/j.1365-8711.2001.04022.xCrossRefGoogle Scholar
Mageshwaran, T., & Mangalam, A. 2015, ApJ, 814, 141CrossRefGoogle Scholar
Merritt, D 2013, Dynamics and Evolution of Galactic Nuclei (Princeton University Press)Google Scholar
Milosavljević, M., Merritt, D., & Ho, L. C. 2006, ApJ, 652, 120CrossRefGoogle Scholar
Schechter, P. 1976, ApJ, 203, 297CrossRefGoogle Scholar
Stone, N. C., & Metzger, B. D. 2016, MNRAS, 455, 859CrossRefGoogle Scholar
van Velzen, S. 2018, ApJ, 852, 72CrossRefGoogle Scholar