Bulletin of the American Physical Society
APS April Meeting 2013
Volume 58, Number 4
Saturday–Tuesday, April 13–16, 2013; Denver, Colorado
Session J4: Invited Session: Neutron Stars and Core-Collapse Supernovae |
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Sponsoring Units: DAP DNP Chair: John Beacom, Ohio State University Room: Plaza F |
Sunday, April 14, 2013 1:30PM - 2:06PM |
J4.00001: Superfluidity in the Core of Neutron Stars Invited Speaker: Dany Page The year (1958) after the publication of the BCS theory, Bohr, Mottelson \& Pines showed that nuclei should also contain superfluid neutrons and superconducting protons. In 1959, A. Migdal proposed that neutron superfluidity should also occur in the interior of neutron stars. Pairing in nuclei forms Cooper pairs with zero spin, but the relevant component of the nuclear interaction becomes repulsive at densities larger than the nuclear matter density. It has been proposed that neutron-neutron interaction in the spin-triplet state, and $L=1$ orbital angular momentum, that is known to be attractive from laboratory experiments, may result in a new form of neutron superfluidity in the neutron star interior. I will review our present understanding of the structure of neutron stars and describe how superfluidity strongly affects their thermal evolution. I will show how a ``Minimal Model'' that excludes the presence of ``exotic'' matter (Bose condensates, quarks, etc.) is compatible with most observations of the surface temperatures of young isolated neutron stars in the case this neutron superfluid exists. Compared to the case of isotropic spin-zero Cooper pairs, the formation of anisotropic spin-one Cooper pairs results in a strong neutrino emission that leads to an enhanced cooling of neutron stars after the onset of the pairing phase transition and allows the Minimal Cooling scenario to be compatible with most observations. In the case the pairing critical temperature $T_c$ is less than about $6 \times 10^8$ K, the resulting rapid cooling of the neutron star may be observable. It was recently reported that 10 years of Chandra observations of the 333 year young neutron star in the Cassiopeia A supernova remnant revealed that its temperature has dropped by about 5\%. This result indicates that neutrons in this star are presently becoming superfluid and, if confirmed, provides us with the first direct observational evidence for neutron superfluidity at supra-nuclear densities. [Preview Abstract] |
Sunday, April 14, 2013 2:06PM - 2:42PM |
J4.00002: X-Ray Bursts and the Neutron Star Crust Invited Speaker: Andrew Cumming |
Sunday, April 14, 2013 2:42PM - 3:18PM |
J4.00003: Observing Core-Collapse Supernovae Invited Speaker: Mansi Kasliwal Our understanding of the ultimate fate of massive stars has grown immensely with the advent of systematic, synoptic surveys. Here, I will review the diverse deaths of massive stars with special emphasis on supernovae from the least massive and most massive progenitors. I will also discuss recently discovered precursor eruptions that precede supernova explosions. [Preview Abstract] |
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