PMID- 23971549
OWN - NLM
STAT- PubMed-not-MEDLINE
DCOM- 20131127
LR  - 20130826
IS  - 1079-7114 (Electronic)
IS  - 0031-9007 (Linking)
VI  - 111
IP  - 6
DP  - 2013 Aug 9
TI  - Establishing a relation between the mass and the spin of stellar-mass black 
      holes.
PG  - 061101
AB  - Stellar mass black holes (SMBHs), forming by the core collapse of very massive, 
      rapidly rotating stars, are expected to exhibit a high density accretion disk 
      around them developed from the spinning mantle of the collapsing star. A wide 
      class of such disks, due to their high density and temperature, are effective 
      emitters of neutrinos and hence called neutrino cooled disks. Tracking the 
      physics relating the observed (neutrino) luminosity to the mass, spin of black 
      holes (BHs) and the accretion rate (M) of such disks, here we establish a 
      correlation between the spin and mass of SMBHs at their formation stage. Our work 
      shows that spinning BHs are more massive than nonspinning BHs for a given M. 
      However, slowly spinning BHs can turn out to be more massive than spinning BHs if 
      M at their formation stage was higher compared to faster spinning BHs.
FAU - Banerjee, Indrani
AU  - Banerjee I
AD  - Department of Physics, Indian Institute of Science, Bangalore 560012, India. 
      indrani@physics.iisc.ernet.in
FAU - Mukhopadhyay, Banibrata
AU  - Mukhopadhyay B
LA  - eng
PT  - Journal Article
DEP - 20130806
PL  - United States
TA  - Phys Rev Lett
JT  - Physical review letters
JID - 0401141
EDAT- 2013/08/27 06:00
MHDA- 2013/08/27 06:01
CRDT- 2013/08/27 06:00
PHST- 2013/04/18 00:00 [received]
PHST- 2013/08/27 06:00 [entrez]
PHST- 2013/08/27 06:00 [pubmed]
PHST- 2013/08/27 06:01 [medline]
AID - 10.1103/PhysRevLett.111.061101 [doi]
PST - ppublish
SO  - Phys Rev Lett. 2013 Aug 9;111(6):061101. doi: 10.1103/PhysRevLett.111.061101. 
      Epub 2013 Aug 6.