Vector current conservation and neutrino emission from singlet-paired baryons in neutron stars

Leinson, L. B.; Perez, A.

doi:10.1016/j.physletb.2006.05.036

Cited by 98 publications

(155 citation statements)

References 15 publications

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“…The neutrino emissivity from neutrons paired in the 1 S 0 state in the inner crust is suppressed by a factor (v F /c) 2 (Leinson & Perez 2006;Sedrakian et al 2007). Recent calculations (Steiner & Reddy 2009) show that this suppression follows from conservation of baryon vector current.…”

Section: Discussionmentioning

confidence: 99%

Mapping Crustal Heating With the Cooling Light Curves of Quasi-Persistent Transients

Brown

Cumming

2009

ApJ

260

461

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The monitoring of quiescent emission from neutron star transients with accretion outbursts long enough to significantly heat the neutron star crust has opened a new vista onto the physics of dense matter. In this paper we construct models of the thermal relaxation of the neutron star crust following the end of a protracted accretion outburst. We confirm the finding of Shternin et al., that the thermal conductivity of the neutron star crust is high, consistent with a low impurity parameter. We describe the basic physics that sets the broken power-law form of the cooling lightcurve. The initial power law decay gives a direct measure of the temperature profile, and hence the thermal flux during outburst, in the outer crust. The time of the break, at hundreds of days post-outburst, corresponds to the thermal time where the solid transitions from a classical to quantum crystal, close to neutron drip. We calculate in detail the constraints on the crust parameters of both KS 1731−260 and MXB 1659−29 from fitting their cooling lightcurves. Our fits to the lightcurves require that the neutrons do not contribute significantly to the heat capacity in the inner crust, and provide evidence in favor of the existence of a neutron superfluid throughout the inner crust. Our fits to both sources indicate an impurity parameter of order unity in the inner crust.

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Section: Discussionmentioning

confidence: 99%

Mapping Crustal Heating With the Cooling Light Curves of Quasi-Persistent Transients

Brown

Cumming

2009

ApJ

260

461

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“…[14,16]. Calculations of the superfluid density response has a long history in condensed matter physics and a pedagogic discussion can be found in Ref.…”

Section: Vector Responsementioning

confidence: 99%

“…This approximate form for the vertex was used in Ref. [15] to compute the response function. It is possible to solve the vertex equation (Eq.…”

Section: Vector Responsementioning

confidence: 99%

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Superfluid response and the neutrino emissivity of neutron matter

Steiner

Reddy

2009

Phys. Rev. C

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We calculate the neutrino emissivity of superfluid neutron matter in the inner crust of neutron stars. We find that neutrino emission due to fluctuations resulting from the formation of Cooper pairs at finite temperature is highly suppressed in non-relativistic systems. This suppression of the pair breaking emissivity in a simplified model of neutron matter with interactions that conserve spin is of the order of v 4 F for density fluctuations and v 2 F for spin fluctuations, where vF is the Fermi velocity of neutrons. The larger suppression of density fluctuations arises because the dipole moment of the density distribution of a single component system does not vary in time. For this reason, we find that the axial current response (spin fluctuations) dominates. In more realistic models of neutron matter which include tensor interactions where the neutron spin is not conserved, neutrino radiation from bremsstrahlung reactions occurs at order v 0 F . Consequently, even with the suppression factors due to superfluidity, this rate dominates near TC. Present calculations of the pair-breaking emissivity are incomplete because they neglect the tensor component of the nucleonnucleon interaction.

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“…Previously, Ref. [32] (hereafter abbreviated as KS) computed the axion counterparts of the PBF processes in neutron stars and set approximate limits on the axion's coupling to baryons and its mass by requiring that the axion emission rate via the PBF processes be smaller than its neutrino counterpart [33][34][35][36][37].…”

Section: Introductionmentioning

confidence: 99%

Axion cooling of neutron stars

2016

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Cooling simulations of neutron stars and their comparison with the data from thermally emitting x-ray sources put constraints on the properties of axions, and by extension of any light pseudoscalar dark matter particles, whose existence has been postulated to solve the strong-CP problem of QCD. We incorporate the axion emission by pair-breaking and formation processes by S-and P -wave nucleonic condensates in a benchmark code for cooling simulations as well as provide fit formulas for the rates of these processes. Axion cooling of neutron stars has been simulated for 24 models covering the mass range 1 to 1.8 solar masses, featuring nonaccreted iron and accreted light-element envelopes, and a range of nucleon-axion couplings. The models are based on an equation state predicting conservative physics of superdense nuclear matter that does not allow for the onset of fast cooling processes induced by phase transitions to non-nucleonic forms of matter or high proton concentration. The cooling tracks in the temperature vs age plane were confronted with the (timeaveraged) measured surface temperature of the central compact object in the Cas A supernova remnant as well as surface temperatures of three nearby middle-aged thermally emitting pulsars.We find that the axion coupling is limited to fa/10 7 GeV ≥ (5-10), which translates into an upper bound on axion mass ma ≤ (0.06-0.12) eV for Peccei-Quinn charges of the neutron |Cn| ∼ 0.04 and proton |Cp| ∼ 0.4 characteristic for hadronic models of axions.

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Vector current conservation and neutrino emission from singlet-paired baryons in neutron stars

Cited by 98 publications

References 15 publications

Mapping Crustal Heating With the Cooling Light Curves of Quasi-Persistent Transients

Mapping Crustal Heating With the Cooling Light Curves of Quasi-Persistent Transients

Superfluid response and the neutrino emissivity of neutron matter

Axion cooling of neutron stars

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