Madappa Prakash and James M Lattimer 2004 J. Phys. G: Nucl. Part. Phys. 30 S451 doi:10.1088/0954-3899/30/1/053
Madappa Prakash and James M Lattimer
Show affiliationsWe contrast the evolution of gravitational binary mergers for the two cases of a black hole and a normal neutron star and a black hole and a self-bound strange quark matter star. In both cases inspiral continues until the Roche limit is reached, at which point it is expected that stable mass transfer to the black hole ensues. Whereas a neutron star would then outspiral, the strange quark matter star barely moves out at all. Eventually, the strange quark star loses all its mass to the black hole, as compared to the neutron star whose outspiral continues until stable mass transfer terminates and inspiral resumes. These scenarios result in distinctly different gravitational wave signatures.
95.30.Sf Relativity and gravitation
95.30.Cq Elementary particle processes
Issue 1 (January 2004)
Received 16 May 2003
Published 11 December 2003
Madappa Prakash and James M Lattimer 2004 J. Phys. G: Nucl. Part. Phys. 30 S451
J K Wright 1960 Proc. Phys. Soc. 75 412
D Smith and N G Adams 1980 J. Phys. D: Appl. Phys. 13 1267
Daniel W Nkemzi and Prabasaj Paul 2005 J. Opt. A: Pure Appl. Opt. 7 529
C E Aguiar and A R Souza 2009 Phys. Educ. 44 624
Y Tokura 2006 Rep. Prog. Phys. 69 797
A-M Perroche and M Boutillon 1995 Metrologia 32 43
J A Paixão et al 1999 J. Phys.: Condens. Matter 11 2127
J E Greene and J M Whelan 1972 J. Phys. E: Sci. Instrum. 5 975
J Hendriks et al 2006 J. Phys. D: Appl. Phys. 39 274