期刊
PHYSICAL REVIEW LETTERS
卷 106, 期 8, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.106.081101
关键词
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资金
- UNAM-DGAPA [IN122609]
- U.S. DOE [DE-FG02-93ER-40756, DE-AC02-87ER40317]
- Joint Institute for Nuclear Astrophysics under NSF-PFC [PHYS 08-22648]
- NASA [NNX08AG76G]
- NSF [PHY-08-00026]
We propose that the observed cooling of the neutron star in Cassiopeia A is due to enhanced neutrino emission from the recent onset of the breaking and formation of neutron Cooper pairs in the P-3(2) channel. We find that the critical temperature for this superfluid transition is similar or equal to 0.5 X 10(9) K. The observed rapidity of the cooling implies that protons were already in a superconducting state with a larger critical temperature. This is the first direct evidence that superfluidity and superconductivity occur at supranuclear densities within neutron stars. Our prediction that this cooling will continue for several decades at the present rate can be tested by continuous monitoring of this neutron star.
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