Neutrino Emission from the Bubble Phase of Stellar Nuclear Matter

Details Neutrino Emission from the Bubble Phase of Stellar Nuclear Matter Neutrino Emission from the Bubble Phase of Stellar Nuclear Matter

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...415..759l&link_type=abstract

Astrophysical Journal v.415, p.759

Astronomy and Astrophysics

Astronomy

5

Dense Matter, Elementary Particles, Stars: Interiors, Stars: Neutron

Scientific paper

A new mechanism of neutrino emission from the bubble phase of nuclear matter is suggested for neutron star cooling. Via the weak neutral current, nucleons emit neutrino-antineutrino pairs by collisions with the bubbles. At the earliest stages of a newly born neutron star cooling, the νμtilde-over-νμ pair luminosity from the bubble phase layer is of the order of 1053 ergs s-1.
Some physical consequences of the bubble phase regime (if any) during the long cooling epoch are also considered. At this stage, the neutrino luminosity of the somewhat thin (˜104 cm) spherical layer of the bubble phase nuclear matter exceeds luminosity of the rest of the stellar body. Intensive matter cooling inside this layer breaks the stellar isothermality and can significantly change the stellar cooling scenario and the theoretical value of neutron star surface temperature.

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