Advances in High Energy Physics

Volume 2017, Article ID 1273931, 11 pages

https://doi.org/10.1155/2017/1273931

## Astrophysical Aspects of Neutrino Dynamics in Ultradegenerate Quark Gluon Plasma

Experimental High Energy Physics and Applications Group, Variable Energy Cyclotron Center, 1/AF Bidhannagar, Kolkata 700 064, India

Correspondence should be addressed to Souvik Priyam Adhya; moc.liamg@7002ayhdakivuos

Received 20 July 2016; Revised 31 December 2016; Accepted 19 February 2017; Published 16 March 2017

Academic Editor: Sally Seidel

Copyright © 2017 Souvik Priyam Adhya. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.

#### Abstract

The cardinal focus of the present review is to explore the role of neutrinos originating from the ultradense core of neutron stars composed of quark gluon plasma in the astrophysical scenario. The collective excitations of the quarks involving the neutrinos through the different kinematical processes have been studied. The cooling of the neutron stars as well as pulsar kicks due to asymmetric neutrino emission has been discussed in detail. Results involving calculation of relevant physical quantities like neutrino mean free path and emissivity have been presented in the framework of non-Fermi liquid behavior as applicable to ultradegenerate plasma.

#### 1. Introduction

Compact stars, in minutes or hours after their birth, rapidly cool down to temperatures of the order of from upper bounds of . The neutrinos produced in direct reactions at the core are essentially transported to the surface leading to the cooling of the neutron star (NS) [1–7]. It is well known that the matter density in the core of the neutron stars could well exceed up to a few times the nuclear matter saturation density. Thus, in this context, we can expect comparable proportions of up, down, and strange quarks [8, 9] which are quite truly the ground state of QCD at finite baryon density. In addition, at such high densities, the constituents of matter are relativistic which compels one to describe such matter in the framework of non-Fermi liquid (NFL) behavior. However, the magnetic interaction is suppressed in powers of for nonrelativistic system. In fact, due to the presence of the magnetic contribution, the long range transverse interactions in deconfined degenerate quark matter give rise to the NFL behavior manifested in the appearance of anomalous contribution to the low temperature limit of the quark self-energy. The breakdown of the Fermi liquid (FL) picture has drawn substantial theoretical interest primarily due to the detection of the NFL behavior in normal state of superconductors [10–13] and in the systems of strongly correlated electrons [14–16]. In a contemporary system such as the quark gluon plasma, at the limit of low temperature, the chromomagnetostatic fields are unscreened unlike the high temperature case. Thus, we find a logarithmic singularity in the inverse group velocity. This singularity is removed by taking into account hard dense loop (HDL) approximations to the propagators [17, 18]. This recently discovered phenomenon of NFL behavior relates itself to the modified quark dispersion relation. Therefore, for excitations close to the Fermi surface, NFL phenomena find important application in this realm of phase space. It has been shown that the NFL corrections to the quark self-energy enhance the neutrino emissivity of ungapped quark matter which may exist at the core of neutron stars [19]. Like emissivity, in dense quark matter, the neutrino mean free path (MFP) also receives significant NFL corrections as has been demonstrated in [20]. In many calculations, such corrections appear in the modification of the phase space giving rise to appreciable contributions to the well known FL terms. Knowledge of the neutrino emissivity showing NFL behavior from quark cores from the neutrino mean free path (MFP) in compact stars is an essential prerequisite for a comprehensive understanding of a host of interesting phenomena such as the cooling of the star. In view of these contemporary investigations, we here plan to present the neutrino MFP and corresponding emissivity in normal degenerate quark matter beyond leading logarithmic order and compare it with the leading order (LO) results. Here, LO refers to the anomalous logarithmic term that occurs as the first term in the non-Fermi liquid contribution to the fermion self-energy. The quantities such as MFP and emissivity of neutrinos calculated with this term are called the LO corrections. Next to leading order (NLO) terms include all other terms beyond the LO that contain the fractional powers of and up to . Quantities calculated with this correction are labeled as NLO corrections [21]. Knowing the specific heat of dense quark matter up to the order concerned, we investigate the cooling behavior of the neutron star with dense quark core. The important theoretical input required for the study of the emissivity and cooling is the neutrino MFP from such quark cores. In all these cases, the correction at the LO has been seen to involve term which has been dubbed as anomalous corrections in many of the literatures [21–23]. In [17, 18], it has been shown that the fermion damping rate and energy loss receive significant NFL correction from the LO terms. Similar behavior has also been reported while investigating quantities like drag, diffusion coefficients, and thermal relaxation time of electrons for relativistic degenerate plasma [24–26]. In fact, the specific heat of the quark matter is also modified due to such corrections beyond the FL order [27]. In this review, we will also present the specific heat of degenerate quark matter which receives significant correction due to the presence of the high external magnetic field while including the NFL corrections. Such high magnetic fields are present at the core of the NS. Thus, the inclusion of the magnetic field in the specific heat in the case of interacting plasma and its effect on the kick velocity of the NS are studied in detail. The mechanism for the generation of such phenomenal kicks is related to the polarization of the electrons leading to neutrino emission in a preferred direction. The magnetic field strength required has to be equal to or greater than , where and are the mass and charge of the electron. This leads to the formation of the neutrino and antineutrino emission cones which give rise to polarized neutrino emission opposite to the direction of the magnetic field producing the recoil velocity. We have used the electron polarization for different conditions of magnetic field and kick velocities which has been studied recently by Sagert et al. [28, 29], where the dependence of the kick velocity on the quark phase temperature and radius of the star with varying quark chemical potentials has also been investigated. In fact, experimental efforts like ROSAT, CHANDRA, and XMM have done a lot of measurements to understand the properties of the neutron stars [30, 31]. Thus, at initial times, the dominant cooling mechanism is by neutrinos only and, at later times, by thermal emission. In addition, if color superconductivity effects are taken into account, the neutrino emissivity and specific heat are then suppressed exponentially by a factor , where is the quasi-particle gap in the color-flavor locked (CFL) phase. However, the presence of the color superconductivity might lower the pulsar acceleration [28, 32].

This review is based upon the recent works [19, 20, 28, 29, 33–35] where the authors have explored various aspects of the neutrino dynamics in reactions involving ultradegenerate quark matter. In this review, we discuss the mean free path of the neutrinos and emissivity of neutrinos from neutron star in Sections 2 and 3, respectively. In addition, we will present results to see how the cooling is affected when one considers the anomalous corrections into the calculable physical quantities in Section 3. In Section 4, we will extend this formalism and introduce the effect of the external magnetic field to calculate the specific heat capacity of degenerate quark matter. This quantity directly influences the kick velocity of pulsars (i.e., rapidly rotating neutron stars) which arises due to asymmetric neutrino emission. Finally, we will present the results and conclusions in Section 5.

#### 2. Neutrino Mean Free Path

##### 2.1. The Case of Degenerate Neutrinos

The dominant contribution to the mean free path as well as emission of neutrinos is given by the quark analog of decay and the electron capture reaction producing neutrinos [36–39]. The degenerate neutrinos refer to the case where the neutrino chemical potential () is much larger than the temperature:In addition, the quark-neutrino scattering process is given by

The corresponding mean free paths are denoted by and which are subsequently combined to obtain the total mean free path of the neutrinos:

The MFP of the neutrinos is related to the total interaction rate due to neutrino emission which is averaged over the initial quark spins and eventually summed over the final state phase space and spins. It is given by [36]where is the spin and color degeneracy, taken as , and , , and are the energy, momentum, and distribution function for the corresponding particle. The squared invariant amplitude is given by . Here, erg- is the weak coupling constant. The interaction involving strange quark is Cabibbo suppressed due to which the neutrino emission from strange quark matter can be neglected. We here consider the case of degenerate neutrinos (i.e., when ). So, in this case, both direct (1) and inverse (2) processes are relevant. Therefore, the equilibrium condition becomes . Now, the momentum integration, and , can be calculated aswhere we define . can be evaluated from the modified dispersion relation as follows [40]:We use the explicit form of the real part of the quark self-energy in the ultradegenerate limit as found in ([21, 27, 33]) which reads as follows:where , where NFL effects dominate. Neglecting the quark-quark interactions, the leading order result is obtained as [20, 33]The NLO result is evaluated as [33, 35, 41]where the constants , , and . For the evaluation of the constants, please refer to [33]. To arrive at the Fermi liquid result, one can use the free dispersion relation to arrive at [36]Quarks and electrons are considered to be massless in this framework, and the chemical equilibrium condition gives , which we use to derive (11). In addition, we have assumed that . The MFP for the quark-neutrino scattering process, for each quark component of flavor or , is calculated which will contribute to the total neutrino flux. Proceeding in a similar way, we obtain [20, 33, 36–39, 41]where is the number density of quark of flavor and [38, 39] and is defined in [20] where if and if . and are the vector and axial vector coupling constants which are given in detail in Table (II) of [36–39]. The contributions from the Fermi liquid (FL), LO, and NLO are added to obtain the MFP of the neutrinos.

##### 2.2. The Case of Nondegenerate Neutrinos

We now derive MFP for nondegenerate neutrinos (i.e., when ) beyond the Fermi liquid contribution. For nondegenerate neutrinos, the inverse process (2) is not considered as, for untrapped case, the reverse reaction is assumed to be zero. Hence, we neglect the second term in the curly braces of (5) [36]. Including the strong interactions between the quarks results in a nonvanishing squared matrix amplitude. The neutrino momentum in energy conserving relation due to the thermal production of the neutrinos can safely be neglected [36]. The Fermi liquid case, LO, and NLO are given as [20, 33, 36, 37, 41]where the constants are evaluated as , , and [33]. In the nondegenerate case, the FL term is proportional to and is not the same as the free Fermi gas. However, for the degenerate case, the FL term contributes at the order . The difference arises due to the evaluation of the squared matrix element for the nondegenerate case where [19].

Similarly, for the scattering of nondegenerate neutrinos in quark matter with appropriate phase space corrections, we obtain [20, 33, 36–39, 41]where , , and [33]. Here, it has been assumed that . Thus, the total MFP for nondegenerate neutrinos is obtained by summing up the contributions from the absorption and scattering parts to get the expression of the MFP of the nondegenerate neutrinos up to the NLO terms.

#### 3. Neutrino Emissivity

In this section, we focus on the calculation of the neutrino emissivity from the neutrino MFP. For our calculation, we consider the MFP of nondegenerate neutrinos. The total emissivity of the nondegenerate neutrinos is obtained by multiplying the neutrino energy with the inverse of the MFP with appropriate factors and integrated over the neutrino momentum given byThe total NFL correction can be obtained aswhereis the usual Fermi liquid contribution which agrees with the result presented in [36]. At the LO, we have obtained [19, 33, 41] The NLO contribution to the neutrino emissivity is [33, 35, 41]where the constants are , , , and [33]. The NFL correction which appears in the phase space integral of the MFP [20] and gradually in the expression of the emissivity [19] is actually related to the unscreened magnetic/transverse interaction. The factor of can be understood as one power of is obtained from phase space integral of a degenerate fermion and from the phase space integral of the neutrino. One power of from the energy conserving function is canceled by a power from the emitted neutrino energy. For excitations lying close to the Fermi surface, the angular integrals provide no temperature dependence.

##### 3.1. Emissivity of Neutrinos from Analogous Processes

In addition to the abovementioned quark direct process, there are contributions from other processes in different domain of density and momentum of the constituent particles. For example, the neutrino emissivity from modified quark URCA process is given as [36]In lower densities, dominant neutrino emission mechanisms are the one-nucleon processes (e.g., ), called nucleon direct URCA (DU) reactions. Their emissivity is [36]where is the nucleon density measured in units of the nuclear matter saturation density . The DU processes are operative only when the proton fraction exceeds a critical value of 11–14%. Another similar process of quite interest is the two-nucleon interactions (in the presence of a bystander particle) (e.g., ), called modified Urca (MU) processes with the emissivity [36]However, other different processes, the nuclear Bremsstrahlung reactions, such as (nB), (npB), and (pB), have an order of magnitude smaller emission rates than the MU processes. In addition, quark matter at asymptotically high density is in the color-flavor locked (CFL) phase [42] of color superconductivity (CSC). The CSC phases at moderate density are still unclear due to the complicated nonperturbative effect. Various candidates have been proposed, such as two-flavor CSC (2SC) [43], gapless 2SC [44, 45], gapless CFL (gCFL) [46], crystalline CSC [47], and spin-1 CSC [48–54]. Neutrino emission from CSC quark matter is exponentially suppressed at low temperature, if the quasi-particle spectra are fully gapped [55–60]. Similar to nuclear matter, the pair breaking and recombination effect results in an emissivity of at temperature close to [61]. The emissivity behaves as for gCFL [55] and for g2SC (see, e.g., Table of [19]).

#### 4. Cooling Behavior of Neutron Star with Dense Quark Core

The results of the MFP of neutrinos with the temperature have been presented in Figure 1. A quark chemical potential of MeV is considered for the process. This agrees well with the high density ~6 ( is the nuclear matter saturation density) at the core. We have taken and . In Figure 1(a), we note that there is a considerable decrease in MFP of degenerate neutrinos due to NLO corrections over the Fermi liquid result. In Figure 1(b), LO correction is compared with the NLO correction and it is seen that the MFP with NLO correction is reduced marginally as compared to LO correction. Similar features have been observed in the case of the MFP of nondegenerate neutrinos as displayed in Figure 2. This modest difference in the MFP between NFL LO and NLO corrections also leads to marginal difference in the emissivity for the two cases. This is shown in Figure 3. These small reductions are reflected in the marginally enhanced emissivity of the nondegenerate neutrinos which has been shown in Figure 3(a). We note that there is a modest increase in the emissivity of the neutrinos. The complicated cooling equation has to be solved numerically as shown in Figure 3(b). The temperature of the neutron star with a quark matter core shows dependency on time. To analyze the cooling of the star [31, 62, 63], the specific heat capacity of the quark matter core needs to be taken into consideration along with the emissivity via the cooling process [19, 36]. We have considered the NFL contribution to the specific heat capacity to compute our results. We observe that the cooling of neutron star is marginally faster in case of NFL (NLO) as compared to the Fermi liquid result (shown in Figure 3). In addition, it is found that the cooling process from the quark core is much faster than the case where the nuclear matter is considered to be present at the core. This influence of magnetic interaction has a significant effect on the cooling behavior of the neutron star, which in the present case is modified due to incorporation of the NFL contribution beyond LO. This leads to marginally faster cooling of the neutron star due to neutrino emission URCA processes and the quark-neutrino scattering reaction.