Baryonic-to-hyperonic transition in collapsing stars

Details Baryonic-to-hyperonic transition in collapsing stars Baryonic-to-hyperonic transition in collapsing stars

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...309..161g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 1, 1986, p. 161-166.

Other

Baryons, Elementary Particle Interactions, Gravitational Collapse, Hyperons, Neutron Stars, Stellar Evolution, Nuclear Reactions, Quarks, Stellar Temperature, Strong Interactions (Field Theory), Supernovae, Weak Interactions (Field Theory)

Scientific paper

Massive stars undergoing hydrodynamic gravitational collapse at the end of their evolution will undergo a phase transition from baryonic to hyperonic matter above densities 7 x 10 to the 14th g/cu cm. At these high densities, quark degrees of freedom must be used for the strongly interacting hadronic matter. Because of blockage by filled states in the Fermi sea, the weak reaction u + d - s + u has a time scale comparable to the collapse time of 0.001 s. The compression due to collapse then drives the reaction rate and results in an exothermic transition producing a temperature increase of 1 MeV, depending weakly on the infall velocity profile. This heating mechanism is thus too weak to alter significantly the late stages of supernova collapse.

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