Abstract
We present a qualitative picture of prompt emission from tidal disruptions of white dwarfs (WD) by intermediate mass black holes (IMBH). The smaller size of an IMBH compared to a supermassive black hole and a smaller tidal radius of a WD disruption lead to a very fast event with high peak luminosity. Magnetic field is generated in situ following the tidal disruption, which leads to effective accretion. Since large-scale magnetic field is also produced, geometrically thick super-Eddington inflow leads to a relativistic jet. The dense jet possesses a photosphere, which emits quasi-thermal radiation in soft X-rays. The source can be classified as a long low-luminosity gamma-ray burst (ll-GRB). Tidal compression of a WD causes nuclear ignition, which is observable as an accompanying supernova. We suggest that GRB060218 and SN2006aj is such a pair of ll-GRB and supernova. We argue that in a flux-limited sample the disruptions of WDs by IMBHs are more frequent then the disruptions of other stars by IMBHs.
Highlights
Two well-known populations of BHs are the stellar mass BHs with mass MBH < 100MSun and supermassive black holes (SMBH) with mass MBH > 105 MSun
intermediate mass black holes (IMBH) can form as a result of a collapse of a massive star [7,8,9] or a massive cloud [10] or grow from a stellar mass BH
In this work we briefly summarize how the jet can be launched following a tidal disruption of a white dwarfs (WD) by an IMBH
Summary
Two well-known populations of BHs are the stellar mass BHs with mass MBH < 100MSun and supermassive black holes (SMBH) with mass MBH > 105 MSun. A third population of intermediate mass black holes (IMBH) likely exists with masses 100MSun < MBH < 105 MSun. A third population of intermediate mass black holes (IMBH) likely exists with masses 100MSun < MBH < 105 MSun They could live in the centers of galaxies that fail to feed their BHs [1] or in globular clusters [2,3,4,5,6]. IMBH can form as a result of a collapse of a massive star [7,8,9] or a massive cloud [10] or grow from a stellar mass BH. While the presence of stellar mass BHs and SMBHs is established, only tentative candidates of IMBHs exist [1, 11, 12] and the debates of the nature of the candidates are ongoing More IMBH candidates with qualitatively different observational signatures could help identify those objects
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