Boson Stars Efficiently Nucleate Vacuum Phase Transitions: Small Star, Large Bubble Limit

Details Boson Stars Efficiently Nucleate Vacuum Phase Transitions: Small Star, Large Bubble Limit Boson Stars Efficiently Nucleate Vacuum Phase Transitions: Small Star, Large Bubble Limit

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr.i1202b&link_type=abstract

American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #I12.02

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In the hot, dense early universe, first order vacuum phase transitions were possible through the tunnelling of a scalar field. In the semi-classical approximation, the bubble nucleation rate depends primarily upon the Euclidean action of the bubble solution. True vacuum bubble nucleation by compact objects (neutron stars, black holes) is more efficient than bubble formation in empty space, i.e., in Coleman's original theory of spontaneous decay of the false vacuum. In this talk, we consider nucleation by another kind of astrophysical object, a boson star, the ground state of a self-gravitating scalar field configuration. Specifically, we model a boson star in a self-interacting potential that also has a term cubic in the scalar field, the so-called 2-3-4 potential. In the limiting case of a ``small'' star nucleating a ``large'' bubble, the dominant change in the total Euclidean action is due to the action of the boson star. We show that the total Euclidean action decreases significantly, enhancing the nucleation rate. We discuss possible observations of the after-effects specific to bubble nucleation by a boson star. boson star and tunnelling

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