T-1020 NaI crystal test for DM-Ice

Maruyama, R.; Heeger, K. M.; Pierpoint, Zachary; Pettus, W.; Broerman, B.; Hilgenberg, Chris; Webber, D.M.; U., Madison Wisconsin

doi:10.2172/1037799

Cited by 6 publications

(6 citation statements)

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“…(9) depends on the combination µB T and hence we need to discuss the expected magnetic fields inside the supernova explosion (we drop the transverse subscript T on B hereafter). We make use of a toy model for the magnetic field and assume it falls off like 1/r 2 , where r is the distance from the center of the supernova, and assume a magnitude of 10 12 gauss at 50 km, which is consistent with estimates in the literature (see, for example, [48]) and might be considered, by some authors, to be conservative (see, for example, [49]):…”

Section: Neutrino Magnetic Moments and Magnetic Fields Inside Sumentioning

confidence: 96%

Effect of transition magnetic moments on collective supernova neutrino oscillations

Gouvêa

Shalgar²

2012

J. Cosmol. Astropart. Phys.

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We study the effect of Majorana transition magnetic moments on the flavor evolution of neutrinos and antineutrinos inside the core of Type-II supernova explosions. We find non-trivial collective oscillation effects relating neutrinos and antineutrinos of different flavors, even if one restricts the discussion to Majorana transition electromagnetic moment values that are not much larger than those expected from standard model interactions and nonzero neutrino Majorana masses. This appears to be, to the best of our knowledge, the only potentially observable phenomenon sensitive to such small values of Majorana transition magnetic moments. We briefly comment on the effect of Dirac transition magnetic moments and on the consequences of our results for future observations of the flux of neutrinos of different flavors from a nearby supernova explosion.

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Section: Neutrino Magnetic Moments and Magnetic Fields Inside Sumentioning

confidence: 96%

Effect of transition magnetic moments on collective supernova neutrino oscillations

Gouvêa

Shalgar²

2012

J. Cosmol. Astropart. Phys.

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“…The hh inelastic collision part is modeled by hadronic resonance productions at low energies and above this resonance region, the string excitation is adapted. The description of interacting N -body system of JAM comes from Relativistic QMD (RQMD) approach [42][43][44], which regarded as a hadronic transport model. A simplified version of RQMD (RQMD/S) that focuses in effective using of CPU was adapted in JAM.…”

Section: Jam Modelmentioning

confidence: 99%

Effects of nuclear potential on the cumulants of net-proton and net-baryon multiplicity distributions in Au+Au collisions atsNN=5GeV

Luo

Nara

et al. 2016

Physics Letters B

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We analyze the rapidity and transverse momentum dependence for the cumulants of the net-proton and net-baryon distributions in Au+Au collisions at √ sNN = 5 GeV with a microscopic hadronic transport (JAM) model. To study the effects of mean field potential and softening of equation of state (EoS) on the fluctuations of net-proton (baryon) in heavy-ion collisions, the calculations are performed with two different modes. The softening of EoS is realized in the model by implementing the attractive orbit in the two-body scattering to introduce a reduction pressure of the system. By comparing the results from the two modes with the results from default cascade, we find the mean field potential and softening of EoS have strong impacts on the rapidity distributions (dN/dy) and the shape of the net-proton (baryon) multiplicity distributions. The net-proton (baryon) cumulants and their ratios calculated from all of the three modes are with similar trends and show significant suppression with respect to unity, which can be explained by the presence of baryon number conservations. It indicates that the effects of mean field potential and softening of EoS might be not the ingredients that are responsible to the observed strong enhancement in the most central Au+Au collisions at 7.7 GeV measured by the STAR experiment at RHIC.PACS numbers: 24.10. Lx, 25.75.Ld, 25.75.Nq, 24.85.+p arXiv:1607.06376v2 [nucl-ex]

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“…If we incorporate this mechanism in the calculation of the cooling curves of young neutron stars, further works are needed which consider the realistic equation of state (EOS) of cold catalyzed quark matter instead of flavor symmetric quark matter and the numerical values of emissivity over the whole region of the DCDW phase without the restriction to the phase boundaries [39]. The effects of the magnetic field is also an interesting subject, since there should be large magnetic field inside compact stars.…”

Section: Summary and Concluding Remarksmentioning

confidence: 99%

Quark beta decay in the inhomogeneous chiral phase and cooling of compact stars

Tatsumi

Muto

2014

Phys. Rev. D

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A novel cooling mechanism is proposed for neutron stars, based on the recent development in the studies of the QCD phase diagram. Possible appearance of the inhomogeneous chiral phase makes the quark beta decay without gluonic interaction. An estimate of the neutrino emissivity shows the order of 10 24−26 (T /10 9 ) 6 (erg·cm −3 · s −1 ) near the phase boundaries, whose efficiency is comparable with the usual quark cooling or pion cooling, but it works only in the limited density region. These features may give another cooling scenario of neutron stars.

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T-1020 NaI crystal test for DM-Ice

Cited by 6 publications

References 0 publications

Effect of transition magnetic moments on collective supernova neutrino oscillations

Effect of transition magnetic moments on collective supernova neutrino oscillations

Effects of nuclear potential on the cumulants of net-proton and net-baryon multiplicity distributions in Au+Au collisions atsNN=5GeV

Quark beta decay in the inhomogeneous chiral phase and cooling of compact stars

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