Medium effects in the pion-pole mechanism[γγ→π0→νRν¯L(νLν¯R)]of neutron star cooling

2003 ◽  
Vol 68 (3) ◽  
Author(s):  
F. Arretche ◽  
A. A. Natale ◽  
D. N. Voskresensky
Keyword(s):  
Neutron Star ◽  
Pion Pole ◽  
Medium Effects ◽  
Neutron Star Cooling ◽  
Pole Mechanism

scholarly journals Developing an end-to-end simulation framework of supernova neutrino detection

2020 ◽  
Author(s):  
Masamitsu Mori ◽  
Yudai Suwa ◽  
Ken’ichiro Nakazato ◽  
Kohsuke Sumiyoshi ◽  
Masayuki Harada ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutrino Emission ◽  
Neutrino Detectors ◽  
Sn 1987A ◽  
Neutrino Detection ◽  
Time Simulation ◽  
Consistent Manner ◽  
Long Time ◽  
Neutron Star Cooling ◽  
Proto Neutron Star

Abstract Massive stars can explode as supernovae at the end of their life cycle, releasing neutrinos whose total energy reaches 1053erg. Moreover, neutrinos play key roles in supernovae, heating and reviving the shock wave as well as cooling the resulting proto-neutron star. Therefore, neutrino detectors are waiting to observe the next galactic supernova and several theoretical simulations of supernova neutrinos are underway. While these simulation concentrate mainly on only the first one second after the supernova bounce, the only observation of a supernova with neutrinos, SN 1987A, revealed that neutrino emission lasts for more than 10 seconds. For this reason, long-time simulation and analysis tools are needed to compare theories with the next observation. Our study is to develop an integrated supernova analysis framework to prepare an analysis pipeline for treating galactic supernovae observations in the near future. This framework deals with the core-collapse, bounce and proto-neutron star cooling processes, as well as with neutrino detection on earth in a consistent manner. We have developed a new long-time supernova simulation in one dimension that explodes successfully and computes the neutrino emission for up to 20 seconds. Using this model we estimate the resulting neutrino signal in the Super-Kamiokande detector to be about 1,800 events for an explosion at 10 kpc and discuss its implications in this paper. We compare this result with the SN 1987A observation to test its reliability.

scholarly journals Neutron Star Cooling with a Dynamic Stellar Structure

2018 ◽  
Vol 862 (1) ◽  
pp. 67
Author(s):  
J. M. Dong ◽  
L. J. Wang ◽  
W. Zuo
Keyword(s):  
Neutron Star ◽  
Stellar Structure ◽  
Neutron Star Cooling

scholarly journals Onset of superconductivity and retention of magnetic fields in cooling neutron stars

2017 ◽  
Vol 13 (S337) ◽  
pp. 213-216
Author(s):  
Wynn C. G. Ho ◽  
Nils Andersson ◽  
Vanessa Graber
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Neutron Stars ◽  
Minimum Energy ◽  
Meissner Effect ◽  
Energy Conditions ◽  
Field Diffusion ◽  
Neutron Star Cooling ◽  
Proton Pairing

AbstractA superconductor of paired protons is thought to form in the core of neutron stars soon after their birth. Minimum energy conditions suggest that magnetic flux is expelled from the superconducting region due to the Meissner effect, such that the neutron star core retains or is largely devoid of magnetic fields for some nuclear equation of state and proton pairing models. We show via neutron star cooling simulations that the superconducting region expands faster than flux is expected to be expelled because cooling timescales are much shorter than timescales of magnetic field diffusion. Thus magnetic fields remain in the bulk of the neutron star core for at least 106 − 107yr. We estimate the size of flux free regions at 107yr to be ≲ 100m for a magnetic field of 1011G and possibly smaller for stronger field strengths.

scholarly journals Neutron Star Cooling: Effects of Envelope Physics

1983 ◽  
Vol 101 ◽  
pp. 513-516
Author(s):  
Kenneth A. Van Riper
Keyword(s):  
Neutron Star ◽  
Surface Temperature ◽  
Supernova Remnants ◽  
Temperature Drop ◽  
Magnetic Star ◽  
Pion Condensate ◽  
Neutron Star Cooling ◽  
Cooling Mechanism ◽  
Cooling Effects ◽  
Star Surface

Neutron star cooling calculations are reported which employ improved physics in the calculation of the temperature drop through the atmosphere. The atmosphere microphysics is discussed briefly. The predicted neutron star surface temperatures, in the interesting interval 300 ≤ t (yr) ≤ 105, do not differ appreciably from the earlier results of Van Riper and Lamb (1981) for a non-magnetic star; for a magnetic star, the surface temperature is lower than in the previous work. Comparison with observational limits show that an exotic cooling mechanism such as neutrino emission from a pion-condensate or in the presence of percolating quarks, is not required, unless the existence of a neutron star in the Tycho or SN1006 supernova remnants is established.

Direct Urca Processes Involving Proton 1 S 0 Superfluidity in Neutron Star Cooling

2018 ◽  
Vol 69 (4) ◽  
pp. 425 ◽  
Author(s):  
Yan Xu ◽  
Zi Yu ◽  
Xiao-Jun Zhang ◽  
Cun-Bo Fan ◽  
Guang-Zhou Liu ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutron Star Cooling

scholarly journals Evolution of Neutron Stars in Young Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 509-512
Author(s):  
K. Nomoto ◽  
S. Tsuruta
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Neutron Star Cooling

The exciting observational developments in recent years (see Seward, Helfand, Harnden, Becker, etc., in this volume) have made it worthwhile to reexamine neutron star cooling theories. Here we shall give an intermediate report on our work.

scholarly journals Role of strangeness to the neutron star mass and cooling

2018 ◽  
Vol 168 ◽  
pp. 04011
Author(s):  
Chang-Hwan Lee ◽  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Kyujin Kwak
Keyword(s):  
Neutron Star ◽  
Dense Matter ◽  
High Density ◽  
Saturation Density ◽  
Strange Quarks ◽  
Star Mass ◽  
Neutron Star Mass ◽  
Neutron Star Cooling

Neutron star provides unique environments for the investigation of the physics of extreme dense matter beyond normal nuclear saturation density. In such high density environments, hadrons with strange quarks are expected to play very important role in stabilizing the system. Kaons and hyperons are the lowest mass states with strangeness among meson and bayron families, respectively. In this work, we investigate the role of kaons and hyperons to the neutron star mass, and discuss their role in the neutron star cooling.

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