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L. B. Leinson

Publications and source records attributed to L. B. Leinson.

At least 19 recordsLinked to original sources
arXiv2014

Comment on "The low lying modes of triplet-condensed neutron matter and their effective theory"

Contrary to what is claimed in the article by P. F. Bedaque and A. N. Nicholson [Phys. Rev. C 87, 055807 (2013)], their result do not contradict but rather complement the conclusion of the paper by L. B. Leinson [Phys. Rev. C 85, 0655021 (2012)] with respect to the low lying nonunitary excitations in the anisotropic neutron superfluid. In fact, the corresponding Goldstone modes (angulons), existing at zero temperature, can be found from Eq. (59) of the work by Leinson. Being massless at absolute zero these modes acquire a mass gap at finite temperature.

nucl-th↗
arXiv2013

Neutrino emissivity of anisotropic neutron superfluids

We examine the influence of the anisotropy of the superfluid energy gap and residual Fermi-liquid interactions in the triplet-correlated neutron liquid onto neutrino energy losses through neutral weak currents. The neutrino-pair emission caused by the pair breaking and formation processes and by the spin-wave decays is considered for the case of the $^{3}P_{2}$ pairing in the state with $m_{j}=0$. The simple analytical formulae are obtained. A comparison with the previous results of the average-angle approach shows that the gap anisotropy leads to quenching of the neutrino emissivity caused by the pair recombination processes on about 15% and to substantial suppression of the spin-wave decays. Residual particle-hole interactions increase the energy losses in both the channels on about 5%.

nucl-th↗
arXiv2012

Collective modes of the order parameter in a triplet superfluid neutron liquid

The complete spectrum of collective modes of the triplet order parameter in the superfluid neutron matter is examined in the BCS approximation below the pair-breaking threshold. The dispersion equations both for the unitary and nonunitary excitations are derived and solved in the limit of $q\rightarrow0$ by taking into account the anisotropy of the energy gap for the case of $P$-wave pairing. By our analysis, there is only one Goldstone mode which is associated with the broken gauge symmetry. We found no additional Goldstone modes associated with the broken rotational symmetry but found that the oscillations of the total angular momentum are qualitatively similar to the "normal-flapping" mode in the A-phase of superfluid Helium. There are also two collective modes associated with internal vibrations of the structure of the order parameter oscillating with $ω(T=0) =1.20Δ_{0}$ and $ω(T=0) =0.61Δ_{0}$.

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arXiv2011

Neutrino emissivity of $^{3}P_{2}$-$^{3}F_{2}$ superfluid cores in neutron stars

The influence of the admixture of the $^{3}F_{2}$ state onto collective spin oscillations and neutrino emission processes in the triplet superfluid neutron liquid is studied in the BCS approximation. The eigen mode of spin oscillations with $ω\simeq\sqrt{58/35}Δ$ is predicted to exist in the triplet superfluid neutron condensate besides the already known mode $ω\simeqΔ/\sqrt{5}$. Excitation of the high-frequency spin oscillations in the condensate occurs through the tensor interactions between quasiparticles. Neutrino energy losses through neutral weak currents are found to consist of three separate contributions caused by a recombination of broken Cooper pairs and by weak decays of the collective modes of spin oscillations. Neutrino decays of the low-frequency spin waves can play an important role in the cooling scenario of neutron stars. Weak decays of the high-frequency oscillations that occur only if the tensor forces are taken into account in the pairing interactions does not modify substantially the total energy losses. Simple expressions are suggested for the total neutrino emissivity.

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arXiv2011

New eigen-mode of spin oscillations in the triplet superfluid condensate in neutron stars

The eigen mode of spin oscillations with $ω\simeq \sqrt{58/35}Δ$ is predicted to exist besides already known spin waves with $ω\simeqΔ/\sqrt{5}$ in the triplet superfluid neutron condensate in the inner core of neutron stars. The new mode is kinematically able to decay into neutrino pairs through neutral weak currents. The problem is considered in BCS approximation for the case of $^{3}P_{2}-^{3}F_{2}$ pairing with a projection of the total angular momentum $m_{j}=0$ which is conventionally considered as preferable one at supernuclear densities.

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arXiv2011

Zero sound in triplet-correlated superfluid neutron matter

The linear response of a superfluid neutron liquid onto external vector field is studied for the case of $^{3}P_{2}-\,^{3}F_{2}$ pairing. The consideration is limited to the case when the wave-length of the perturbation is large as compared to the coherence length in the superfluid matter and the transferred energy is small in comparison with the gap amplitude. The obtained results are used to analyse the collisionless phonon-like excitations of the condensate of superfluid neutrons. In particular, we analyze the case of neutron condensation into the state with $m_{j}=0$ which is conventionally considered as the preferable one in the bulk matter of neutron stars. Zero sound (if it exists) is found to be anisotropic and undergoes strong decrement below some temperature threshold depending substantially on the intensity of Fermi-liquid interactions.

hep-ph↗
arXiv2010

Superfluid phases of triplet pairing and neutrino emission from neutron stars

Neutrino energy losses through neutral weak currents in the triplet-spin superfluid neutron liquid are studied for the case of condensate involving several magnetic quantum numbers. Low-energy excitations of the multicomponent condensate in the timelike domain of the energy and momentum are analyzed. Along with the well-known excitations in the form of broken Cooper pairs, the theoretical analysis predicts the existence of collective waves of spin density at very low energy. Because of a rather small excitation energy of spin waves, their decay leads to a substantial neutrino emission at the lowest temperatures, when all other mechanisms of neutrino energy loss are killed by a superfluidity. Neutrino energy losses caused by the pair recombination and spin-wave decays are examined in all of the multicomponent phases that might represent the ground state of the condensate, according to modern theories, and for the case when a phase transition occurs in the condensate at some temperature. Our estimate predicts a sharp increase in the neutrino energy losses followed by a decrease, along with a decrease in the temperature, that takes place more rapidly than it would without the phase transition. We demonstrate the important role of the neutrino radiation caused by the decay of spin waves in the cooling of neutron stars.

hep-ph↗
arXiv2010

Neutrino emission from spin waves in neutron spin-triplet superfluid

The linear response of a neutron spin-triplet superfluid onto external weak axial-vector field is studied for the case of $^{3}P_{2}$ pairing with a projection of the total angular momentum $m_{j}=0$. The problem is considered in the BCS approximation discarding Fermi-liquid effects. The anomalous axial-vector vertices of neutron quasiparticles possess singularities at some frequencies which specify existence of undamped spin-density waves in the Cooper condensate. The spin waves are of a low excitation energy and are kinematically able to decay into neutrino pairs through neutral weak currents. We evaluate the neutrino emissivity from the spin wave decays in the bulk neutron superfluid in old neutron stars. This calculation predicts significant energy losses from within a neutron star at lowest temperatures when all other mechanisms of neutrino emission are killed by the neutron and proton superfluidity.

astro-ph.SR↗
arXiv2010

Neutrino emission from triplet pairing of neutrons in neutron stars

Neutrino emission due to the pair breaking and formation processes in the bulk triplet superfluid in neutron stars is investigated with taking into account of anomalous weak interactions. We consider the problem in the BCS approximation discarding Fermi-liquid effects. In this approach we derive self-consistent equations for anomalous vector and axial-vector vertices of weak interactions taking into account the $^{3}P_{2}- ^{3}F_{2}$ mixing. Further we simplify the problem and consider the pure $^{3}P_{2}$ pairing with $m_{j}=0$, as is adopted in the minimal cooling paradigm. As was expected because of current conservation we have obtained a large suppression of the neutrino emissivity in the vector channel. More exactly, the neutrino emission through the vector channel vanishes in the nonrelativistic limit $V_F=0$. The axial channel is also found to be moderately suppressed. The total neutrino emissivity is suppressed by a factor of $1.9\times10^{-1}$ relative to original estimates using bare weak vertices.

astro-ph.SR↗
arXiv2009

Superfluid response and the neutrino emissivity of baryon matter: Fermi-liquid effects

The linear response of a nonrelativistic superfluid baryon system on an external weak field is investigated while taking into account of the Fermi-liquid interactions. We generalize the theory developed by Leggett for a superfluid Fermi-liquid at finite temperature to the case of timelike momentum transfer typical of the problem of neutrino emission from neutron stars. A space-like kinematics is also analysed for completeness and compared with known results. We use the obtained response functions to derive the neutrino energy losses caused by recombination of broken pairs in the electrically neutral superfluid baryon matter. We find that the dominant neutrino radiation occurs through the axial-vector neutral currents. The emissivity is found to be of the same order as in the BCS approximation, but the details of its temperature dependence are modified by the Fermi-liquid interactions. The role of electromagnetic correlations in the pairing case of protons interacting with the electron background is discussed in the conclusion.

astro-ph.HE↗
arXiv2008

BCS approximation to the effective vector vertex of superfluid fermions

We examine the effective interaction of nonrelativistic fermions with an external vector field in superfluid systems. In contrast to the complicated vertex equation, usually used in this case, we apply the approach which does not employ an explicit form of the pairing interaction. This allows to obtain a simple analytic expression for the vertex function only in terms of the order parameter and other macroscopic parameters of the system. We use this effective vertex to analyze the linear response function of the superfluid medium at finite temperatures. At the time-like momentum transfer, the imaginary part of the response function is found to be proportional to the fourth power of small Fermi velocity, i.e. the energy losses through vector currents are strongly suppressed. As an application, we calculate the neutrino energy losses through neutral weak currents caused by the pair recombination in the superfluid neutron matter at temperatures lower than the critical one for S-wave pairing. This approach confirms a strong suppression of the neutrino energy losses as predicted in Ref.[4].

astro-ph↗
arXiv2006

Neutrino emission due to Cooper pairing in neutron stars

Neutrino emission caused by Cooper pairing of baryons in neutron stars is recalculated by accurately taking into account for conservation of the vector weak current. The vector current contribution to the neutrino emissivity is found to be several orders of magnitude smaller than that obtained before by different authors. Therefore, the neutrino energy losses due to singlet-state pairing of baryons can in practice be neglected in simulations of neutron star cooling. This makes negligible the neutrino radiation from pairing of protons or hyperons. The neutrino radiation from triplet pairing takes place through axial weak currents. For these states, when the total momentum projection is $m_{j}=0$, the vanishing of the vector weak current contribution results in the suppression of the neutrino energy losses by about 25%. The neutrino emissivity due to triplet pairing with $| m_{j}| =2$ is suppressed by about a factor of 3, caused by the collective contribution of spin-density fluctuations in the condensate.

astro-ph↗
arXiv2006

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

Neutrino emission caused by singlet Cooper pairing of baryons in neutron stars is recalculated by accurately taking into account for conservation of the vector weak currents. The neutrino emissivity via the vector weak currents is found to be several orders of magnitude smaller than that obtained before by different authors. This makes unimportant the neutrino radiation from singlet pairing of protons or hyperons.

astro-ph↗
arXiv2004

Neutrino-pair bremsstrahlung from nucleons in the condensed pion field: revisited

At temperatures less than a few MeV, the efficiency of the neutrino-pair bremsstrahlung from nucleons interracting with the condensed pion field is much less than previously estimated by other authors. The physical reason for this is a periodic structure of the developed pion condensate. The repeated interactions of a nucleon with the periodic pion field modify the nucleon spectrum, which is split into two bands. The energy gap between the bands is about a few MeV or larger, even if the amplitude of the pion field is small compared with the pion mass.

astro-ph↗
arXiv2003

On relativistic approaches to the pion self-energy in nuclear matter

We argue that, in contrast to the non-relativistic approach, a relativistic evaluation of the nucleon--hole and delta-isobar--nucleon hole contributions to the pion self-energy incorporates the s-wave scattering, which requires a more accurate evaluation. Therefore relativistic approach containing only these diagrams does not describe appropriately the pion self-energy in isospin symmetric nuclear matter. We conclude that, a correct relativistic approach to the pion self-energy should involve a more sophisticated calculation in order to satisfy the known experimental results on the near-threshold behaviour of the pion-nucleon (forward) scattering amplitude.

nucl-th↗
arXiv2003

Relativistic short-range correlation effects on the pion dynamics in nuclear matter

Replicated theoretical attempts of relativistic approaches to the pion self-energy in nuclear matter yield unphysical pion spectra. We demonstrate the crucial dependence of the calculated pion spectra on the correct relativistic accounting for the short-range correlation effects on the pion self-energy in the medium. To do this, we simulate the short-range interactions by phenomenological contact terms in the relativistic Lagrangian density, and derive the pion self-energy by carefully taking into account the relativistic kinematics. The obtained spectrum for the pion-like excitations in cold nuclear matter shows physically meaningful branches, in contrast to those obtained before by different authors by the use of simplified relativistic approaches to the short-range correlations.

nucl-th↗
arXiv2002

Direct Urca processes in superdense cores of neutron stars

We use the field theoretical model to perform relativistic calculations of neutrino energy losses caused by the direct Urca processes on nucleons in the degenerate baryon matter. By our analysis, in a free nucleon gas under beta equilibrium, the direct neutron decay is forbidden if the number density of neutrons exceeds the critical value $n_{n}^{c}=5.9\times 10^{31} cm^{-3}$. In superdense nuclear matter, $n>n_{0}$, the weak decay of neutrons is possible only due to strong interactions, caused by an exchange of isovector mesons. Mean field of isovector mesons in the medium creates a large energy gap between spectrums of protons and neutrons, which is required by kinematics of beta decay. Our expression for the neutrino energy losses, obtained in the mean field approximation, incorporates the effects of nucleon recoil, parity violation, weak magnetism, and pseudoscalar interaction. For numerical testing of our formula, we use a self-consistent relativistic model of the multicomponent baryon matter. The relativistic emissivity of the direct Urca reactions is found substantially larger than predicted in the non-relativistic approach. We found that, due to weak magnetism effects, relativistic emissivities increase by approximately 40-50%.

hep-ph↗