Open AccessAn upper bound on Q-star masses
Author(s) -
D.R. Hochron,
Bryan W. Lynn,
Stephen B. Selipsky
Publication year - 1992
Language(s) - English
Resource type - Reports
DOI - 10.2172/94554
Subject(s) - physics , star (game theory) , upper and lower bounds , generalization , stars , bound state , field (mathematics) , symmetry (geometry) , astrophysics , quantum mechanics , geometry , mathematics , mathematical analysis , pure mathematics
Q-stars (the gravitational generalization of Q-balls, strongly bound bulk matter that an appear in field theories of strongly interacting hadrons) are the only known impact objects consistent with the known bulk structure of nuclei and chiral symmetry that evade the Rhoades-Ruffini upper bound of 3.2M{sub {circle_dot}}. Generic bounds are quite weak: M{sub Q-star} < 400M{sub {circle_dot}}. If, however, we assume that the 1.558 ms pulsar is a Q-star, equilibrium. A stability criteria of rotating fluids place a much stronger upper bound of M{sub c} {le} 5.3M{sub {circle_dot}} on such models under certain special assumptions. This has important implications for heavy compact objects such as Cygnus X-1