Dynamical instability of bosonic stellar configurations

Details Dynamical instability of bosonic stellar configurations Dynamical instability of bosonic stellar configurations

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989nuphb.316..411j&link_type=abstract

Nuclear Physics B, Volume 316, Issue 2, p. 411-428.

Physics

Nuclear Physics

31

Scientific paper

We study the problem of the dynamical stability of the equilibrium solutions for the bosonic stellar configurations in the framework of general relativity. The time evolution of infinitesimal radial oscillations, which conserve the total number of particles, is analyzed starting from the scalar wave equation coupled to the Einstein field equations. Following the method developed by Chandrasekhar, one finds a variational principle for determining the eigenfrequencies of the oscillations. Using the variational principle, one can find numerically an upper bound for the central densities where dynamical instability occurs. As examples we consider the equilibrium configurations, found by Ruffini and Bonazzola, for the non-interacting massive complex scalar fields as well as the quartic self-interacting case, V(φ) = 1/4λ~ > φl4 (λ~ > 0), discussed by Colpi, Shapiro and Wasserman. In the non-interacting case, we find that for central densities bigger than ϱ = 2.1 × 1098m2 g/cm3 (m is the boson mass in grams) the configuration is dynamically unstable; whereas in the interacting case, with a value λ~ = 3.8 × 1012m2, the bound is given by ϱ = 1.3 × 1098m2 g/cm3.
Supported by the Swiss National Science Foundation. Address after October 1, 1988: CERN, Theory Division, CH-1211, Genève 23, Switzerland.

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