Showing 1–48 of 48 results for author: Bombaci, I

Dark matter admixed neutron stars with a realistic nuclear equation of state from chiral nuclear interactions

Authors: Domenico Scordino, Ignazio Bombaci

Abstract: We study the effects of dark matter on the structural properties of neutron stars. In particular we investigate how the presence of a dark matter component influences the mass-radius relation, the value of the maximum mass of a neutron star and other stellar properties. To model ordinary matter we use a state-of-the-art equation of state of $β$-stable nuclear matter obtained using the Brueckner-Ha… ▽ More We study the effects of dark matter on the structural properties of neutron stars. In particular we investigate how the presence of a dark matter component influences the mass-radius relation, the value of the maximum mass of a neutron star and other stellar properties. To model ordinary matter we use a state-of-the-art equation of state of $β$-stable nuclear matter obtained using the Brueckner-Hartree-Fock quantum many-body approach starting from two-body and three-body nuclear interactions derived from chiral effective field theory. The dark matter component of the star is modeled as a non-self-annihilating system of spin $1/2$ fermions at zero temperature and its equation of state as an ideal relativistic Fermi gas. The equilibrium configurations of these dark matter admixed neutron stars (DANS) are calculated by solving a generalization of the Tolman-Oppenheimer-Volkoff equations to the case where the system consists of two perfect fluids interacting solely through gravity. We find that, depending on the dark matter particle mass $m_χ$, one can have somehow opposite effects on the stellar properties. In the case $m_χ= 1\, \mathrm{GeV}$, the stellar gravitational maximum mass $M_{max}$ decreases, whereas in the case $m_χ= 0.1\, \mathrm{GeV}$, $M_{max}$ increases with respect to the maximum mass of ordinary neutron stars. We also show that the presence of dark matter has indirect sizable effect on the proton fraction in the ordinary matter fluid and, in the case $m_χ= 1\, \mathrm{GeV}$, results in a decrease of the threshold gravitational mass $M_{tot}^{durca}$ for having direct URCA processes and fast stellar cooling. Finally we study the stability of dark matter admixed neutron stars with respect to radial perturbations. △ Less

Submitted 28 May, 2025; v1 submitted 29 May, 2024; originally announced May 2024.

Comments: Final version accepted for publication

Journal ref: Journal of High Energy Astrophysics, 45 (2025) 371-381

Effect of chiral nuclear forces on the neutrino mean free path in hot neutron matter

Authors: Isaac Vidana, Domenico Logoteta, Ignazio Bombaci

Abstract: We study the role of chiral nuclear forces on the propagation of neutrinos in hot neutron matter. In particular, we analyze the convergence of the dynamical structure factor and the neutrino mean free path with the order of the power counting of the chiral forces, as well as the role of the regulator cut-off of these forces in the determination of these quantities. Single-particle energies and che… ▽ More We study the role of chiral nuclear forces on the propagation of neutrinos in hot neutron matter. In particular, we analyze the convergence of the dynamical structure factor and the neutrino mean free path with the order of the power counting of the chiral forces, as well as the role of the regulator cut-off of these forces in the determination of these quantities. Single-particle energies and chemical potentials needed to calculate the dynamical structure factor are obtained within the Brueckner--Hartree--Fock approximation extended to finite temperature. Our results show that the dynamical structure factor and the neutrino mean free path depend on the cut-off only when the chiral potential is considered at leading order (LO) and next-to leading order (NLO), becoming this dependence strongly reduced at higher orders in the chiral power counting due to the role of three-nucleon forces that start to contribute at next-to-next-to leading order (N$^2$LO) being, in particular, almost negligible at next-to-next-to-next-to leading order (N$^3$LO). The neutrino mean free path is found to converge up to densities slightly below $\sim 0.15$ fm$^{-3}$ when increasing the order of the chiral power counting, although no signal of convergence is found for densities above this value. The uncertainty associated with our order-by-order nuclear many-body calculation of the neutrino mean free path is roughly estimated from the difference between the results obtained at N$^2$LO and N$^3$LO, finding that it varies from about a few centimeters at low densities up to a bit less than $2$ meters at the largest one considered in this work, $0.3$ fm$^{-3}$. △ Less

Submitted 21 June, 2022; originally announced June 2022.

Comments: 7 pages, 5 figures, 1 table

Benchmark calculations of infinite neutron matter with realistic two- and three-nucleon potentials

Authors: A. Lovato, I. Bombaci, D. Logoteta, M. Piarulli, R. B. Wiringa

Abstract: We present the equation of state of infinite neutron matter as obtained from highly-realistic Hamiltonians that include nucleon-nucleon and three-nucleon coordinate-space potentials. We benchmark three independent many-body methods: Brueckner-Bethe-Goldstone (BBG), Fermi hypernetted chain/single-operator chain (FHNC/SOC), and auxiliary-field diffusion Monte Carlo (AFDMC). We find them to provide s… ▽ More We present the equation of state of infinite neutron matter as obtained from highly-realistic Hamiltonians that include nucleon-nucleon and three-nucleon coordinate-space potentials. We benchmark three independent many-body methods: Brueckner-Bethe-Goldstone (BBG), Fermi hypernetted chain/single-operator chain (FHNC/SOC), and auxiliary-field diffusion Monte Carlo (AFDMC). We find them to provide similar equations of state when the Argonne $v_{18}$ and the Argonne $v_{6}^\prime$ nucleon-nucleon potentials are used in combination with the Urbana IX three-body force. Only at densities larger than about 1.5 the nuclear saturation density ($ρ_0 = 0.16\,\rm{fm}^{-3}$) the FHNC/SOC energies are appreciably lower than the other two approaches. The AFDMC calculations carried out with all of the Norfolk potentials fitted to reproduce the experimental trinucleon ground-state energies and $nd$ doublet scattering length yield unphysically bound neutron matter, associated with the formation of neutron droplets. Including tritium $β$-decay in the fitting procedure, as in the second family of Norfolk potentials, mitigates but does not completely resolve this problem. An excellent agreement between the BBG and AFDMC results is found for the subset of Norfolk interactions that do not make neutron-matter collapse, while the FHNC/SOC equations of state are moderately softer. △ Less

Submitted 21 February, 2022; originally announced February 2022.

Comments: 15 pages, 3 figures. arXiv admin note: text overlap with arXiv:1908.04426

Microscopic equation of state of hot nuclear matter for numerical relativity simulations

Authors: Domenico Logoteta, Albino Perego, Ignazio Bombaci

Abstract: A precise understanding of the equation of state (EOS) of dense and hot matter is key to modeling relativistic astrophysical environments, including core-collapse supernovae (CCSNe), protoneutron star (PNSs) evolution, and compact binary mergers. In this paper, we extend the microscopic zero-temperature BL (Bombaci and Logoteta) %nuclear equation of state nuclear EOS %derived by Bombaci and Logote… ▽ More A precise understanding of the equation of state (EOS) of dense and hot matter is key to modeling relativistic astrophysical environments, including core-collapse supernovae (CCSNe), protoneutron star (PNSs) evolution, and compact binary mergers. In this paper, we extend the microscopic zero-temperature BL (Bombaci and Logoteta) %nuclear equation of state nuclear EOS %derived by Bombaci and Logoteta to finite temperature and arbitrary nuclear composition. We employ this new EOS to describe hot $β$-stable nuclear matter and to compute various structural properties of nonrotating PNS. %protoneutron stars. We also apply the EOS to perform dynamical simulations of a spherically symmetric CCSN. The EOS is derived using the finite temperature extension of the Brueckner--Bethe--Goldstone quantum many-body theory in the Brueckner--Hartree--Fock approximation. Neutron star properties are computed by solving the Tolman--Oppenheimer--Volkoff structure equations numerically. The sperically symmetric CCSN simulations are performed using the AGILE-IDSA code. Our EOS models are able to reproduce typical features of both PNS and spherically symmetric CCSN simulations. In addition, our EOS model is consistent with present measured neutron star masses and particularly with the masses: $M = 2.01 \pm 0.04 \, M_{\odot}$ and $M = 2.14^{+0.20}_{-0.18} \, M_{\odot}$ of the neutron stars in PSR~J0348+0432 and PSR J0740+6620 respectively. Finally, we suggest a feasible mechanism to produce low-mass black holes ($M \sim 2M_{\odot}$) that could have far-reaching consequences for interpreting the gravitational wave event GW190814 as a BH--BH merger. △ Less

Submitted 7 December, 2020; originally announced December 2020.

Comments: Accepted for publication in A&A

Was GW190814 a black hole -- strange quark star system?

Authors: I. Bombaci, A. Drago, D. Logoteta, G. Pagliara, I. Vidana

Abstract: We investigate the possibility that the low mass companion of the black hole in the source of GW190814 was a strange quark star. This possibility is viable within the so-called two-families scenario in which neutron stars and strange quark stars coexist. Strange quark stars can reach the mass range indicated by GW190814, $M\sim (2.5-2.67) M_\odot$ due to a large value of the adiabatic index, witho… ▽ More We investigate the possibility that the low mass companion of the black hole in the source of GW190814 was a strange quark star. This possibility is viable within the so-called two-families scenario in which neutron stars and strange quark stars coexist. Strange quark stars can reach the mass range indicated by GW190814, $M\sim (2.5-2.67) M_\odot$ due to a large value of the adiabatic index, without the need for a velocity of sound close to the causal limit. Neutron stars (actually hyperonic stars in the two-families scenario) can instead fulfill the presently available astrophysical and nuclear physics constraints which require a softer equation of state. In this scheme it is possible to satisfy both the request of very large stellar masses and of small radii while using totally realistic and physically motivated equations of state. Moreover it is possible to get a radius for a 1.4 $M_\odot$ star of the order or less than 11 km, which is impossible if only one family of compact stars exists. △ Less

Submitted 6 April, 2021; v1 submitted 4 October, 2020; originally announced October 2020.

Comments: 6 pages, 3 figures. Accepted on Phys. Rev. Letters

Journal ref: Phys. Rev. Lett. 126, 162702 (2021)

Benchmark calculations of pure neutron matter with realistic nucleon-nucleon interactions

Authors: M. Piarulli, I. Bombaci, D. Logoteta, A. Lovato, R. B. Wiringa

Abstract: We report benchmark calculations of the energy per particle of pure neutron matter as a function of the baryon density using three independent many-body methods: Brueckner-Bethe-Goldstone, Fermi hypernetted chain/single-operator chain, and auxiliary-field diffusion Monte Carlo. Significant technical improvements are implemented in the latter two methods. The calculations are made for two distinct… ▽ More We report benchmark calculations of the energy per particle of pure neutron matter as a function of the baryon density using three independent many-body methods: Brueckner-Bethe-Goldstone, Fermi hypernetted chain/single-operator chain, and auxiliary-field diffusion Monte Carlo. Significant technical improvements are implemented in the latter two methods. The calculations are made for two distinct families of realistic coordinate-space nucleon-nucleon potentials fit to scattering data, including the standard Argonne $v_{18}$ interaction and two of its simplified versions, and four of the new Norfolk $Δ$-full chiral effective field theory potentials. The results up to twice nuclear matter saturation density show some divergence among the methods, but improved agreement compared to earlier work. We find that the potentials fit to higher-energy nucleon-nucleon scattering data exhibit a much smaller spread of energies. △ Less

Submitted 12 August, 2019; originally announced August 2019.

Comments: 16 pages, 7 figures

Journal ref: Phys. Rev. C 101, 045801 (2020)

Impact of chiral hyperonic three-body forces on neutron stars

Authors: Domenico Logoteta, Isaac Vidana, Ignazio Bombaci

Abstract: We study the effect of the nucleon-nucleon-lambda (NN$Λ$) three-body force on neutron stars. In particular, we consider the NN$Λ$ force recently derived by the Jülich--Bonn--Munich group within the framework of chiral effective field theory at next-to-next-to-leading order. This force, together with realistic nucleon-nucleon, nucleon-nucleon-nucleon and nucleon-hyperon interactions, is used to cal… ▽ More We study the effect of the nucleon-nucleon-lambda (NN$Λ$) three-body force on neutron stars. In particular, we consider the NN$Λ$ force recently derived by the Jülich--Bonn--Munich group within the framework of chiral effective field theory at next-to-next-to-leading order. This force, together with realistic nucleon-nucleon, nucleon-nucleon-nucleon and nucleon-hyperon interactions, is used to calculate the equation of state and the structure of neutron stars within the many-body non-relativistic Brueckner-Hartree-Fock approach. Our results show that the inclusion of the NN$Λ$ force leads to an equation of state stiff enough such that the resulting neutron star maximum mass is compatible with the largest currently measured ($\sim 2\ M_\odot$) neutron star masses. Using a perturbative many-body approach we calculate also the separation energy of the $Λ$ in some hypernuclei finding that the agreement with the experimental data improves for the heavier ones when the effect of the NN$Λ$ force is taken into account. △ Less

Submitted 15 November, 2019; v1 submitted 27 June, 2019; originally announced June 2019.

Comments: 7 pages, 5 figures, 3 tables

Journal ref: Eur. Phys. J. A (2019) 55:207

Neutron star properties from optimized chiral nuclear interactions

Authors: Domenico Logoteta, Ignazio Bombaci

Abstract: We adopt two- and three-body nuclear forces derived at the next-to-next-to-leading-order (N2LO) in the framework of effective chiral perturbation theory (ChPT) to calculate the equation of state (EOS) of $β$-stable neutron star matter using the Brueckner--Hartree--Fock many-body approach. We use the recent optimized chiral two-body nuclear interaction at N2LO derived by \cite{ekstrom1} and two dif… ▽ More We adopt two- and three-body nuclear forces derived at the next-to-next-to-leading-order (N2LO) in the framework of effective chiral perturbation theory (ChPT) to calculate the equation of state (EOS) of $β$-stable neutron star matter using the Brueckner--Hartree--Fock many-body approach. We use the recent optimized chiral two-body nuclear interaction at N2LO derived by \cite{ekstrom1} and two different parametrizations of the three-body N2LO interaction: the first one is fixed to reproduce the saturation point of symmetric nuclear matter while the second one is fixed to reproduce the binding energies of light atomic nuclei. We show that in the second case the properties of nuclear matter are not well determined whereas in the first case various empirical nuclear matter properties around the saturation density are well reproduced. We also calculate the nuclear symmetry energy $E_{sym}$ as a function of the nucleonic density and compare our results with the empirical constraints obtained using the excitation energies of isobaric analog states in nuclei and the experimental data on the neutron skin thickness of heavy nuclei. We next calculate various neutron star properties and in particular the mass-radius and mass-central density relations. We find that the adopted interactions based on a fully microscopic framework, are able to provide an EOS which is consistent with the present data of measured neutron star masses and in particular with the mass $M=2.01\pm0.04 M_\odot$ of the neutron star in PSR J0348+0432. We finally consider the possible presence of hyperons in the stellar core and we find a softening of the EOS and a substantial reduction of the stellar maximum mass in agreement with similar calculations present in the literature. △ Less

Submitted 26 June, 2018; originally announced June 2018.

Comments: Accepted for publication in PASA

Correlations imposed by the unitary limit between few-nucleon systems, nuclear matter and neutron stars

Authors: A. Kievsky, M. Viviani, D. Logoteta, I. Bombaci, L. Girlanda

Abstract: The large values of the singlet and triplet two-nucleon scattering lengths locate the nuclear system close to the unitary limit. This particular position strongly constrains the low-energy observables in the three-nucleon system as depending on one parameter, the triton binding energy, and introduces correlations in the low energy sector of light nuclei. Here we analyze the propagation of these co… ▽ More The large values of the singlet and triplet two-nucleon scattering lengths locate the nuclear system close to the unitary limit. This particular position strongly constrains the low-energy observables in the three-nucleon system as depending on one parameter, the triton binding energy, and introduces correlations in the low energy sector of light nuclei. Here we analyze the propagation of these correlations to infinite nuclear matter showing that its saturation properties, the equation of state of $β$-stable nuclear matter and several properties of neutron stars, as their maximum mass, are well determined solely by a few number of low-energy quantities of the two- and three-nucleon systems. In this way we make a direct link between the universal behavior observed in the low-energy region of few-nucleon systems and fundamental properties of nuclear matter and neutron stars. △ Less

Submitted 31 July, 2018; v1 submitted 7 June, 2018; originally announced June 2018.

Comments: 5 pages, 3 figures

Journal ref: Phys. Rev. Lett. 121, 072701 (2018)

Equation of state of dense nuclear matter and neutron star structure from nuclear chiral interactions

Authors: Ignazio Bombaci, Domenico Logoteta

Abstract: We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and $β$-stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the $Δ(1232)$ isobar intermediate state. This EOS is provided in tabular form and i… ▽ More We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and $β$-stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the $Δ(1232)$ isobar intermediate state. This EOS is provided in tabular form and in parametrized form ready for use in numerical general relativity simulations of binary neutron star merging. Here we use our new EOS for $β$-stable nuclear matter to compute various structural properties of non-rotating neutron stars.The EOS is derived using the Brueckner--Bethe--Goldstone quantum many-body theory in the Brueckner--Hartree--Fock approximation. Neutron star properties are next computed solving numerically the Tolman--Oppenheimer--Volkov structure equations. Our EOS models are able to reproduce the empirical saturation point of symmetric nuclear matter, the symmetry energy $E_{sym}$, and its slope parameter $L$ at the empirical saturation density $n_{0}$. In addition, our EOS models are compatible with experimental data from collisions between heavy nuclei at energies ranging from a few tens of MeV up to several hundreds of MeV per nucleon. These experiments provide a selective test for constraining the nuclear EOS up to $\sim 4 n_0$. Our EOS models are consistent with present measured neutron star masses and particularly with the mass $M = 2.01 \pm 0.04 \, M_{\odot}$ of the neutron stars in PSR~J0348+0432. △ Less

Submitted 30 May, 2018; originally announced May 2018.

Journal ref: A&A 609, A128 (2018)

Two coexisting families of compact stars: observational implications for millisecond pulsars

Authors: Sudip Bhattacharyya, Ignazio Bombaci, Domenico Logoteta, Arun V. Thampan

Abstract: It is usually thought that a single equation of state (EoS) model "correctly" represents cores of all compact stars. Here we emphasize that two families of compact stars, viz., neutron stars and strange stars, can coexist in nature, and that neutron stars can get converted to strange stars through the nucleation process of quark matter in the stellar center. From our fully general relativistic num… ▽ More It is usually thought that a single equation of state (EoS) model "correctly" represents cores of all compact stars. Here we emphasize that two families of compact stars, viz., neutron stars and strange stars, can coexist in nature, and that neutron stars can get converted to strange stars through the nucleation process of quark matter in the stellar center. From our fully general relativistic numerical computations of the structures of fast-spinning compact stars, known as millisecond pulsars, we find that such a stellar conversion causes a simultaneous spin-up and decrease in gravitational mass of these stars. This is a new type of millisecond pulsar evolution through a new mechanism, which gives rise to relatively lower mass compact stars with higher spin rates. This could have implication for the observed mass and spin distributions of millisecond pulsars. Such a stellar conversion can also rescue some massive, spin-supported millisecond pulsars from collapsing into black holes. Besides, we extend the concept of critical mass $M_{\rm cr}$ for the neutron star sequence (Berezhiani et al. 2003; Bombaci et al. 2004) to the case of fast-spinning neutron stars, and point out that neutron star EoS models cannot be ruled out by the stellar mass measurement alone. Finally, we emphasize the additional complexity for constraining EoS models, for example, by stellar radius measurements using X-ray observations, if two families of compact stars coexist. △ Less

Submitted 7 September, 2017; originally announced September 2017.

Comments: 10 pages, 5 figures, accepted for publication in The Astrophysical Journal

Millisecond radio pulsars with known masses: parameter values and equation of state models

Authors: Sudip Bhattacharyya, Ignazio Bombaci, Debades Bandyopadhyay, Arun V. Thampan, Domenico Logoteta

Abstract: The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from… ▽ More The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from nucleonic, hyperonic, strange quark matter and hybrid classes, we numerically compute fast spinning stable stellar parameter values considering the full effect of general relativity. This first detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS. We estimate uncertainties on these computed values from the uncertainty of the measured mass, which could be useful to quantitatively constrain EoS models. We note that the largest value of the central density $ρ_{\rm c}$ in our catalogue is $\sim 5.8$ times the nuclear saturation density $ρ_{\rm sat}$, which is much less than the expected maximum value $13 ρ_{\rm sat}$. We argue that the $ρ_{\rm c}$-values of at most a small fraction of compact stars could be much larger than $5.8 ρ_{\rm sat}$. Besides, we find that the constraints on EoS models from accurate radius measurements could be significantly biased for some of our pulsars, if stellar $spinning$ configurations are not used to compute the theoretical radius values. △ Less

Submitted 12 January, 2017; originally announced January 2017.

Comments: 16 pages, 2 figures, 4 tables, accepted for publication in New Astronomy

Nuclear matter properties from local chiral interactions with $Δ$ isobar intermediate states

Authors: Domenico Logoteta, Ignazio Bombaci, Alejandro Kievsky

Abstract: Using two-nucleon and three-nucleon interactions derived in the framework of chiral perturbation theory (ChPT) with and without the explicit $Δ$ isobar contributions, we calculate the energy per particle of symmetric nuclear matter and pure neutron matter in the framework of the microscopic Brueckner-Hartree-Fock approach. In particular, we present for the first time nuclear matter calculations us… ▽ More Using two-nucleon and three-nucleon interactions derived in the framework of chiral perturbation theory (ChPT) with and without the explicit $Δ$ isobar contributions, we calculate the energy per particle of symmetric nuclear matter and pure neutron matter in the framework of the microscopic Brueckner-Hartree-Fock approach. In particular, we present for the first time nuclear matter calculations using the new fully local in coordinate-space two-nucleon interaction at the next-to-next-to-next-to-leading-order (N3LO) of ChPT with $Δ$ isobar intermediate states (N3LO$Δ$) recently developed by Piarulli et al. [arXiv:1606:06335]. We find that using this N3LO$Δ$ potential, supplemented with a local N2LO three-nucleon interaction with explicit $Δ$ isobar degrees of freedom, it is possible to obtain a satisfactory saturation point of symmetric nuclear matter. For this combination of two- and three-nucleon interactions we also calculate the nuclear symmetry energy and we compare our results with the empirical constraints on this quantity obtained using the excitation energies to isobaric analog states in nuclei and using experimental data on the neutron skin thickness of heavy nuclei, finding a very good agreement with these empirical constraints in all the considered nucleonic density range. In addition, we find that the explicit inclusion of $Δ$ isobars diminishes the strength of the three-nucleon interactions needed the get a good saturation point of symmetric nuclear matter. We also compare the results of our calculations with those obtained by other research groups using chiral nuclear interactions with different many-body methods, finding in many cases a very satisfactory agreement. △ Less

Submitted 2 September, 2016; originally announced September 2016.

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Authors: Sudip Bhattacharyya, Ignazio Bombaci, Domenico Logoteta, Arun V. Thampan

Abstract: For a set of equation of state (EoS) models involving interacting strange quark matter, characterized by an effective bag constant (B_eff) and a perturbative QCD corrections term (a_4), we construct fully general relativistic equilibrium sequences of rapidly spinning strange stars for the first time. Computation of such sequences is important to study millisecond pulsars and other fast spinning co… ▽ More For a set of equation of state (EoS) models involving interacting strange quark matter, characterized by an effective bag constant (B_eff) and a perturbative QCD corrections term (a_4), we construct fully general relativistic equilibrium sequences of rapidly spinning strange stars for the first time. Computation of such sequences is important to study millisecond pulsars and other fast spinning compact stars. Our EoS models can support a gravitational mass (M_G) and a spin frequency at least up to approximately 3.0 solar mass and approximately 1250 Hz respectively, and hence are fully consistent with measured M_G and spin frequency values. This paper reports the effects of B_eff and a_4 on measurable compact star properties, which could be useful to find possible ways to constrain these fundamental quark matter parameters, within the ambit of our EoS models. We confirm that a lower B_eff allows a higher mass. Besides, for known M_G and spin frequency, measurable parameters, such as stellar radius, radius-to-mass ratio and moment of inertia, increase with the decrease of B_eff. Our calculations also show that a_4 significantly affects the stellar rest mass and the total stellar binding energy. As a result, a_4 can have signatures in evolutions of both accreting and non-accreting compact stars, and the observed distribution of stellar mass and spin and other source parameters. Finally, we compute the parameter values of two important pulsars, PSR J1614-2230 and PSR J1748-2446ad, which may have implications to probe their evolutionary histories, and for constraining EoS models. △ Less

Submitted 22 January, 2016; originally announced January 2016.

Comments: 17 pages, 11 figures, 7 tables, accepted for publication in Monthly Notices of the Royal Astronomical Society

The Hyperon Puzzle in Neutron Stars

Authors: Ignazio Bombaci

Abstract: The so called "hyperon puzzle", i.e. the difficulty to reconcile the measured masses of neutron stars (NSs) with the presence of hyperons in their interiors, is one of the hot topics in astrophysics which is stimulating copious experimental and theoretical research in hypernuclear physics. After illustrating the origin of the hyperon puzzle, I discuss some of its possible solutions, and particular… ▽ More The so called "hyperon puzzle", i.e. the difficulty to reconcile the measured masses of neutron stars (NSs) with the presence of hyperons in their interiors, is one of the hot topics in astrophysics which is stimulating copious experimental and theoretical research in hypernuclear physics. After illustrating the origin of the hyperon puzzle, I discuss some of its possible solutions, and particularly those related to the role of hyperonic two- and three-body interactions on the equation of state of dense matter. Afterward, I discuss a possibility to circumvent the hyperon puzzle allowing for the presence of strangeness in NSs in the form of deconfined strange quark matter, and thus considering the so called quark stars, i.e. hybrid stars or strange stars. Finally I discuss the astrophysical consequences of the possible conversion process of an hadronic star to a quark star. △ Less

Submitted 19 January, 2016; originally announced January 2016.

Comments: Invited keynote talk at the Topical Session "Hyperon puzzle in Neutron Stars" at the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015), September 7-12, 2015, Sendai, Japan. arXiv admin note: text overlap with arXiv:1601.04559

Quark matter nucleation in neutron stars and astrophysical implications

Authors: Ignazio Bombaci, Domenico Logoteta, Isaac Vidana, Constanca Providencia

Abstract: A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. We investigate the quark deconfinement phase transition in cold (T = 0) and hot beta-stable hadronic matter. Assuming a first order phase transition, we calculate and compare the nucleation rate and the nucleation time due to quantum and thermal nucleation mechanisms. We show that above a… ▽ More A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. We investigate the quark deconfinement phase transition in cold (T = 0) and hot beta-stable hadronic matter. Assuming a first order phase transition, we calculate and compare the nucleation rate and the nucleation time due to quantum and thermal nucleation mechanisms. We show that above a threshold value of the central pressure a pure hadronic star (HS) (i.e. a compact star with no fraction of deconfined quark matter) is metastable to the conversion to a quark star (QS) (i.e. a hybrid star or a strange star). This process liberates an enormous amount of energy, of the order of 10^{53}~erg, which causes a powerful neutrino burst, likely accompanied by intense gravitational waves emission, and possibly by a second delayed (with respect to the supernova explosion forming the HS) explosion which could be the energy source of a powerful gamma-ray burst (GRB). This stellar conversion process populates the QS branch of compact stars, thus one has in the Universe two coexisting families of compact stars: pure hadronic stars and quark stars. We introduce the concept of critical mass M_{cr} for cold HSs and proto-hadronic stars (PHSs), and the concept of limiting conversion temperature for PHSs. We show that PHSs with a mass M < M_{cr} could survive the early stages of their evolution without decaying to QSs. Finally, we discuss the possible evolutionary paths of proto-hadronic stars. △ Less

Submitted 15 January, 2016; originally announced January 2016.

Comments: Invited review paper accepted for publication in EPJ A, Topical Issue on "Exotic Matter in Neutron Stars"

Comparative study of three-nucleon force models in nuclear matter

Authors: Domenico Logoteta, Isaac Vidaña, Ignazio Bombaci, Alejandro Kievsky

Abstract: We calculate the energy per particle of symmetric nuclear matter and pure neutron matter using the microscopic many-body Brueckner-Hartree-Fock (BHF) approach and employing the Argonne V18 (AV18) nucleon-nucleon (NN) potential supplemented with two different three-nucleon force models recently constructed to reproduce the binding energy of $^3$H, $^3$He and $^4$He nuclei as well as the neutron-deu… ▽ More We calculate the energy per particle of symmetric nuclear matter and pure neutron matter using the microscopic many-body Brueckner-Hartree-Fock (BHF) approach and employing the Argonne V18 (AV18) nucleon-nucleon (NN) potential supplemented with two different three-nucleon force models recently constructed to reproduce the binding energy of $^3$H, $^3$He and $^4$He nuclei as well as the neutron-deuteron doublet scattering length. We find that none of these new three-nucleon force models is able to reproduce simultaneously the empirical saturation point of symmetric nuclear matter and the properties of three- and four-nucleon systems. △ Less

Submitted 4 February, 2015; originally announced February 2015.

Quark deconfinement transition in neutron stars with the field correlator method

Authors: Domenico Logoteta, Ignazio Bombaci

Abstract: A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. In this article, we perform a study of the hadron-quark phase transition in cold (T = 0) neutron star matter and we calculate various structural properties of hybrid stars. For the quark phase, we make use of an equation of state (EOS) derived with the field correlator method (FCM) recentl… ▽ More A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. In this article, we perform a study of the hadron-quark phase transition in cold (T = 0) neutron star matter and we calculate various structural properties of hybrid stars. For the quark phase, we make use of an equation of state (EOS) derived with the field correlator method (FCM) recently extended to the case of nonzero baryon density. For the hadronic phase, we consider both pure nucleonic and hyperonic matter, and we derive the corresponding EOS within a relativistic mean field approach. We make use of measured neutron star masses, and particularly the mass $M = 1.97 \pm 0.04 \, M_\odot$ of PSR J1614 -2230 to constrain the values of the gluon condensate $G_2$, which is one of the EOS parameters within the FCM. We find that the values of $G_2$ extracted from the mass measurement of PSR J1614 -2230 are consistent with the values of the same quantity derived within the FCM from recent lattice QCD calculations of the deconfinement transition temperature at zero baryon chemical potential. The FCM thus provides a powerful tool to link numerical calculations of QCD on a space-time lattice with measured neutron star masses. △ Less

Submitted 31 August, 2013; originally announced September 2013.

Comments: PHYSICAL REVIEW D (in press). arXiv admin note: substantial text overlap with arXiv:1212.5907

Journal ref: Phys. Rev. D 88, 063001 (2013)

Quark matter nucleation with a microscopic hadronic equation of state

Authors: Domenico Logoteta, Constança Providência, Isaac Vidana, Ignazio Bombaci

Abstract: The nucleation process of quark matter in cold (T = 0) stellar matter is investigated using the microscopic Brueckner-Hartree-Fock approach to describe the hadronic phase, and the MIT bag model, the Nambu-Jona-Lasinio, and the Chromo Dielectric models to describe the deconfined phase of quark matter. The consequences of the nucleation process for neutron star physics are outlined. Hyperonic stars… ▽ More The nucleation process of quark matter in cold (T = 0) stellar matter is investigated using the microscopic Brueckner-Hartree-Fock approach to describe the hadronic phase, and the MIT bag model, the Nambu-Jona-Lasinio, and the Chromo Dielectric models to describe the deconfined phase of quark matter. The consequences of the nucleation process for neutron star physics are outlined. Hyperonic stars are metastable only for some of the quark matter equations of state considered. The effect of an hyperonic three body force on the metastability of compact stars is estimated, and it is shown that, except for the Nambu-Jona-Lasinio model and the MIT bag model with a large bag pressure, the other models predict the formation of hybrid stars with a maximum mass not larger than \sim 1.62 M\odot . △ Less

Submitted 26 April, 2012; originally announced April 2012.

Chiral model approach to quark matter nucleation in neutron stars

Authors: Domenico Logoteta, Ignazio Bombaci, Constança Providência, Isaac Vidana

Abstract: The nucleation process of quark matter in both cold and hot dense hadronic matter is investigated using a chiral approach to describe the quark phase. We use the Nambu-Jona-Lasinio and the Chromo Dielectric models to describe the deconfined phase and the non-linear Walecka model for the hadronic one. The effect of hyperons on the transition phase between hadronic and quark matter is studied. The c… ▽ More The nucleation process of quark matter in both cold and hot dense hadronic matter is investigated using a chiral approach to describe the quark phase. We use the Nambu-Jona-Lasinio and the Chromo Dielectric models to describe the deconfined phase and the non-linear Walecka model for the hadronic one. The effect of hyperons on the transition phase between hadronic and quark matter is studied. The consequences of the nucleation process for neutron star physics are outlined. △ Less

Submitted 19 March, 2012; originally announced March 2012.

Journal ref: Physical Review D 85, 023003 (2012)

Effects of quark matter nucleation on the evolution of proto-neutron stars

Authors: Ignazio Bombaci, Domenico Logoteta, Constanca Providencia, Isaac Vidana

Abstract: (Abridged) A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. If this deconfinement phase transition is of the first order then it will be triggered by the nucleation of a critical size drop of the stable quark phase in the metastable hadronic phase. Within these circumstances it has been shown that cold pure hadronic compact stars above a… ▽ More (Abridged) A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. If this deconfinement phase transition is of the first order then it will be triggered by the nucleation of a critical size drop of the stable quark phase in the metastable hadronic phase. Within these circumstances it has been shown that cold pure hadronic compact stars above a threshold value of their gravitational mass are metastable with respect to the "decay" to quark stars (compact stars made at least in part of quark matter). This stellar conversion process liberates a huge amount of energy, and it could be the energy source of some of the long GRBs. The main goal of the present work is to establish whether a newborn hadronic star (proto-hadronic star) could survive the early stages of its evolution without "decaying" to a quark star. To this aim, we study the nucleation process of quark matter in hot beta-stable hadronic matter, with and without trapped neutrinos. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences of quark matter nucleation for the physics and the evolution of proto-neutron stars. We introduce the new concept of limiting conversion temperature and critical mass M_cr for proto-hadronic stars, and we show that proto-hadronic stars with a mass M < M_cr could survive the early stages of their evolution without decaying to a quark star. We extend the concept of maximum mass of a "neutron star" with respect to the classical one introduced by Oppenheimer & Volkoff to account for the existence of two distinct families of compact stars (hadronic stars and quark stars) as predicted by the present scenario. △ Less

Submitted 8 February, 2011; originally announced February 2011.

Comments: Accepted for publication in Astronomy and Astrophysics

Journal ref: Astronomy and Astrophysics, 528, A71 (2011)

Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars

Authors: Isaac Vidana, Domenico Logoteta, Constanza Providencia, Artur Polls, Ignazio Bombaci

Abstract: A model based on a microscopic Brueckner--Hartree--Fock approach of hyperonic matter supplemented with additional simple phenomenological density-dependent contact terms is employed to estimate the effect of hyperonic three-body forces on the maximum mass of neutron stars. Our results show that although hyperonic three-body forces can reconcile the maximum mass of hyperonic stars with the current… ▽ More A model based on a microscopic Brueckner--Hartree--Fock approach of hyperonic matter supplemented with additional simple phenomenological density-dependent contact terms is employed to estimate the effect of hyperonic three-body forces on the maximum mass of neutron stars. Our results show that although hyperonic three-body forces can reconcile the maximum mass of hyperonic stars with the current limit of $1.4-1.5 M_\odot$, they are unable to provide the repulsion needed to make the maximum mass compatible with the observation of massive neutron stars, such as the recent measurements of the unusually high masses of the millisecond pulsars PSR J1614-2230 ($1.97 \pm 0.04 M_\odot$) and PSR J1903+0327 ($1.667 \pm 0.021 M_\odot$). △ Less

Submitted 3 March, 2011; v1 submitted 29 June, 2010; originally announced June 2010.

Comments: 6 pages, 1 figure, 2 tables. Accepted for publication in EPL

Journal ref: Europhys.Lett.94:11002,2011

An analytic parametrization of the hyperonic matter equation of state

Authors: Isaac Vidana, Domenico Logoteta, Constanza Providencia, Artur Polls, Ignazio Bombaci

Abstract: An analytic parametrization of the hyperonic matter equation of state based on microscopic Brueckner-Hartree-Fock calculations has been constructed using the realistic Argonne V18 nucleon-nucleon potential plus a three-body force of Urbana type, and three models of the hyperon-nucleon interaction: the Nijmegen soft-core models NSC89 and NSC97e, and the most recent meson-exchange potential of the J… ▽ More An analytic parametrization of the hyperonic matter equation of state based on microscopic Brueckner-Hartree-Fock calculations has been constructed using the realistic Argonne V18 nucleon-nucleon potential plus a three-body force of Urbana type, and three models of the hyperon-nucleon interaction: the Nijmegen soft-core models NSC89 and NSC97e, and the most recent meson-exchange potential of the Juelich group. The construction of this parametrization is based on a simple phase-space analysis and reproduces with good accuracy the results of the microscopic calculations with a small number of parameters. This parametrization allows for rapid calculations that accurately mimic the microscopic results, being therefore, very useful from a practical point of view. △ Less

Submitted 22 April, 2010; originally announced April 2010.

Comments: 10 pages, 4 figures, 3 tables

Quark matter nucleation in hot hadronic matter

Authors: I. Bombaci, D. Logoteta, P. K. Panda, C. Providencia, I. Vidana

Abstract: We study the quark deconfinement phase transition in hot $β$-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron-quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates… ▽ More We study the quark deconfinement phase transition in hot $β$-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron-quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences for the physics of proto-neutron stars. We introduce the concept of limiting conversion temperature and critical mass $M_{cr}$ for proto-hadronic stars, and we show that proto-hadronic stars with a mass $M < M_{cr}$ could survive the early stages of their evolution without decaying to a quark star. △ Less

Submitted 21 October, 2009; originally announced October 2009.

Journal ref: Phys.Lett.B680:448-452,2009

Quark matter in compact stars: astrophysical implications and possible signatures

Authors: I. Bombaci

Abstract: After a brief non technical introduction of the basic properties of strange quark matter (SQM) in compact stars, we consider some of the late important advances in the field, and discuss some recent astrophysical observational data that could shed new light on the possible presence of SQM in compact stars. We show that above a threshold value of the gravitational mass a neutron star (pure hadron… ▽ More After a brief non technical introduction of the basic properties of strange quark matter (SQM) in compact stars, we consider some of the late important advances in the field, and discuss some recent astrophysical observational data that could shed new light on the possible presence of SQM in compact stars. We show that above a threshold value of the gravitational mass a neutron star (pure hadronic star) is metastable to the decay (conversion) to an hybrid neutron star or to a strange star. We explore the consequences of the metastability of "massive" neutron stars and of the existence of stable compact "quark" stars (hybrid neutron stars or strange stars) on the concept of limiting mass of compact stars, and we give an extension of this concept with respect to the "classical" one given in 1939 by Oppenheimer and Volkoff. △ Less

Submitted 24 September, 2008; originally announced September 2008.

Comments: Invited talk at "the Eleventh Marcel Grossman Meeting on General Relativity", Berlin 2006

Metastability of hadronic compact stars

Authors: I. Bombaci, P. K. Panda, C. Providencia, I. Vidana

Abstract: Pure hadronic compact stars, above a threshold value of their gravitational mass (central pressure), are metastable to the conversion to quark stars (hybrid or strange stars). In this paper, we present a systematic study of the metastability of pure hadronic compact stars using different relativistic models for the equation of state (EoS). In particular, we compare results for the quark-meson co… ▽ More Pure hadronic compact stars, above a threshold value of their gravitational mass (central pressure), are metastable to the conversion to quark stars (hybrid or strange stars). In this paper, we present a systematic study of the metastability of pure hadronic compact stars using different relativistic models for the equation of state (EoS). In particular, we compare results for the quark-meson coupling (QMC) model with those for the Glendenning--Moszkowski parametrization of the non-linear Walecka model (NLWM). For QMC model, we find large values ($M_{cr} = 1.6$ -- $1.9 M_\odot$) for the critical mass of the hadronic star sequence and we find that the formation of a quark star is only possible with a soft quark matter EoS. For the Glendenning--Moszkowski parametrization of the NLWM, we explore the effect of different hyperon couplings on the critical mass and on the stellar conversion energy. We find that increasing the value of the hyperon coupling constants shifts the bulk transition point for quark deconfinement to higher densities, increases the stellar metastability threshold mass and the value of the critical mass, and thus makes the formation of quark stars less likely. For the largest values of the hyperon couplings we find a critical mass which may be as high as 1.9 - 2.1 $M_\odot$. These stellar configurations, which contain a large central hyperon fraction ($f_{Y,cr} \sim 30 %$), would be able to describe highly-massive compact stars, such as the one associated to the millisecond pulsars PSR B1516+02B with a mass $M = 1.94^{+ 0.17}_{- 0.19} M_{\odot}$. △ Less

Submitted 13 February, 2008; originally announced February 2008.

Comments: 15 pages, 7 figures, 3 Tables. Accepted for publication in Phys. Rev. D

Journal ref: Phys.Rev.D77:083002,2008

Equation of state for asymmetric nuclear matter with infinite-order summation of ring diagrams

Authors: J. Shamanna, T. T. S. Kuo, I. Bombaci, Subhankar Ray

Abstract: The particle-particle hole-hole ring-diagram summation method is employed to obtain the equation of state of asymmetric nuclear matter over a wide range of asymmetry fraction. Compared with Brueckner Hartree-Fock and model-space Brueckner Hartree-Fock calculations, this approach gives a softer equation of state, increased symmetry energy and a lower value for the incompressibility modulus which… ▽ More The particle-particle hole-hole ring-diagram summation method is employed to obtain the equation of state of asymmetric nuclear matter over a wide range of asymmetry fraction. Compared with Brueckner Hartree-Fock and model-space Brueckner Hartree-Fock calculations, this approach gives a softer equation of state, increased symmetry energy and a lower value for the incompressibility modulus which agrees quite well with the values used in the hydrodynamical model for the supernovae explosion. △ Less

Submitted 6 September, 2005; originally announced September 2005.

Comments: 14 pages, 10 figures

Microscopic calculations of spin polarized neutron matter at finite temperature

Authors: I. Bombaci, A. Polls, A. Ramos, A. Rios, I. Vidana

Abstract: The properties of spin polarized neutron matter are studied both at zero and finite temperature within the framework of the Brueckner--Hartree--Fock formalism, using the Argonne v18 nucleon-nucleon interaction. The free energy, energy and entropy per particle are calculated for several values of the spin polarization, densities and temperatures together with the magnetic susceptibility of the sy… ▽ More The properties of spin polarized neutron matter are studied both at zero and finite temperature within the framework of the Brueckner--Hartree--Fock formalism, using the Argonne v18 nucleon-nucleon interaction. The free energy, energy and entropy per particle are calculated for several values of the spin polarization, densities and temperatures together with the magnetic susceptibility of the system. The results show no indication of a ferromagnetic transition at any density and temperature. △ Less

Submitted 6 June, 2005; originally announced June 2005.

Comments: 19 pages, 5 figures

Journal ref: Phys.Lett. B632 (2006) 638-643

Deconfinement and color superconductivity in cold neutron stars

Authors: G. Lugones, I. Bombaci

Abstract: We study the deconfinement transition of hadronic matter into quark matter in neutron star conditions in the light of color superconductivity. Deconfinement is considered to be a first order phase transition that conserves color and flavor. It gives a short-lived {($τ\sim τ_{weak}$)} transitory colorless-quark-phase that is {\it not} in $β$-equilibrium. We deduce the equations governing deconfin… ▽ More We study the deconfinement transition of hadronic matter into quark matter in neutron star conditions in the light of color superconductivity. Deconfinement is considered to be a first order phase transition that conserves color and flavor. It gives a short-lived {($τ\sim τ_{weak}$)} transitory colorless-quark-phase that is {\it not} in $β$-equilibrium. We deduce the equations governing deconfinement when quark pairing is allowed and find the regions of the parameter space (pairing gap $Δ$ versus bag constant $B$) where deconfinement is possible inside cold neutron stars. We show that for a wide region of ($B,Δ$) a pairing pattern is reachable within a strong interaction timescale, and the resulting ``2SC-like'' phase is preferred energetically to the unpaired phase. We also show that although $β$-stable hybrid star configurations are known to be possible for a wide region of the ($B,Δ$)-space, many of these configurations could not form in practice because deconfinement is forbidden, i.e. the here studied non-$β$-stable \emph{intermediate} state cannot be reached. △ Less

Submitted 15 September, 2005; v1 submitted 25 April, 2005; originally announced April 2005.

Comments: Version to appear in Phys. Rev. D (10 pages, 6 figures)

Journal ref: Phys.Rev.D72:065021,2005

Spin-orbit and tensor interactions in homogeneous matter of nucleons: accuracy of modern many-body theories

Authors: I. Bombaci, A. Fabrocini, A. Polls, I. Vidana

Abstract: We study the energy per particle of symmetric nuclear matter and pure neutron matter using realistic nucleon--nucleon potentials having non central tensor and spin--orbit components, up to three times the empirical nuclear matter saturation density, $ρ_0=0.16$ fm$^{-3}$. The calculations are carried out within the frameworks of the Brueckner--Bethe--Goldstone (BBG) and Correlated Basis Functions… ▽ More We study the energy per particle of symmetric nuclear matter and pure neutron matter using realistic nucleon--nucleon potentials having non central tensor and spin--orbit components, up to three times the empirical nuclear matter saturation density, $ρ_0=0.16$ fm$^{-3}$. The calculations are carried out within the frameworks of the Brueckner--Bethe--Goldstone (BBG) and Correlated Basis Functions (CBF) formalisms, in order to ascertain the accuracy of the methods. The two hole--line approximation, with the continuous choice for the single particle auxiliary potential, is adopted for the BBG approach, whereas the variational Fermi Hypernetted Chain/Single Operator Chain theory, corrected at the second order perturbative expansion level, is used in the CBF one. The energies are then compared with the available Quantum and Variational Monte Carlo results in neutron matter and with the BBG, up to the three hole--line diagrams. For neutron matter and potentials without spin--orbit components all methods, but perturbative CBF, are in reasonable agreement up to $ρ\sim$ 3 $ρ_0$. After the inclusion of the LS interactions, we still find agreement around $ρ_0$, whereas it is spoiled at larger densities. The spin--orbit potential lowers the energy of neutron matter at $ρ_0$ by $\sim$ 3--4 MeV per nucleon. In symmetric nuclear matter, the BBG and the variational results are in agreement up to $\sim$ 1.5 $ρ_0$. Beyond this density, and in contrast with neutron matter, we find good agreement only for the potential having spin--orbit components. △ Less

Submitted 24 January, 2005; v1 submitted 15 November, 2004; originally announced November 2004.

Comments: 18 pages, 4 tables. Accepted in PLB

Journal ref: Phys.Lett. B609 (2005) 232-240

Quark deconfinement and neutrino trapping in compact stars

Authors: I. Vidana, I. Bombaci, I. Parenti

Abstract: We study the role played by neutrino trapping on the hadron star (HS) to quark star (QS) conversion mechanism proposed recently by Berezhiani and collaborators. We find that the nucleation of quark matter drops inside hadron matter, and therefore the conversion of a HS into a QS, is strongly inhibit by the presence of neutrinos. We study the role played by neutrino trapping on the hadron star (HS) to quark star (QS) conversion mechanism proposed recently by Berezhiani and collaborators. We find that the nucleation of quark matter drops inside hadron matter, and therefore the conversion of a HS into a QS, is strongly inhibit by the presence of neutrinos. △ Less

Submitted 12 November, 2004; originally announced November 2004.

Comments: 3 pages, 3 figures. Talk given at the VIII International Conference on Strangeness in Quark Matter. Cape Town, South Africa, Septembre 2004

Journal ref: J.Phys. G31 (2005) S1165-S1170

Quark deconfinement and implications for the radius and the limiting mass of compact stars

Authors: Ignazio Bombaci, Irene Parenti, Isaac Vidaña

Abstract: We study the consequences of the hadron-quark deconfinement phase transition in stellar compact objects when finite size effects between the deconfined quark phase and the hadronic phase are taken into account. We show that above a threshold value of the central pressure (gravitational mass) a neutron star is metastable to the decay (conversion) to a hybrid neutron star or to a strange star. The… ▽ More We study the consequences of the hadron-quark deconfinement phase transition in stellar compact objects when finite size effects between the deconfined quark phase and the hadronic phase are taken into account. We show that above a threshold value of the central pressure (gravitational mass) a neutron star is metastable to the decay (conversion) to a hybrid neutron star or to a strange star. The "mean-life time" of the metastable configuration dramatically depends on the value of the stellar central pressure. We explore the consequences of the metastability of ``massive'' neutron stars and of the existence of stable compact quark stars (hybrid neutron stars or strange stars) on the concept of limiting mass of compact stars. We discuss the implications of our scenario on the interpretation of the stellar mass and radius extracted from the spectra of several X-ray compact sources. Finally, we show that our scenario implies, as a natural consequence a two step-process which is able to explain the inferred ``delayed'' connection between supernova explosions and GRBs, giving also the correct energy to power GRBs. △ Less

Submitted 17 February, 2004; originally announced February 2004.

Comments: 34 pages, 10 figures

Journal ref: Astrophys.J.614:314-325,2004

Strangeness in Neutron Stars

Authors: Ignazio Bombaci

Abstract: We discuss the role of strangeness on the internal constitution and structural properties of neutron stars. In particular, we report on recent calculations of hyperon star properties derived from microscopic equations of state for hyperonic matter. Next, we discuss the possibility of having a strange quark matter core in a neutron star, or the possible existence of strange quark matter stars, th… ▽ More We discuss the role of strangeness on the internal constitution and structural properties of neutron stars. In particular, we report on recent calculations of hyperon star properties derived from microscopic equations of state for hyperonic matter. Next, we discuss the possibility of having a strange quark matter core in a neutron star, or the possible existence of strange quark matter stars, the so-called strange stars. △ Less

Submitted 17 December, 2003; originally announced December 2003.

Comments: Invited review talk at the VIII International Conference on Hypernuclear and Strange Particle Physics, Jefferson Lab, Newport News, Virginia, October 14-18, 2003. 10 pages, 5 figures

Report number: DF/UNIPI/Th/031217a

Journal ref: Nucl.Phys. A754 (2005) 335-344

Microscopic calculation of neutrino mean free path inside hot neutron matter

Authors: Jerome Margueron, Isaac Vidana, Ignazio Bombaci

Abstract: We calculate the neutrino mean free path and the Equation of State of pure neutron matter at finite temperature within a selfconsistent scheme based on the Brueckner--Hartree--Fock approximation. We employ the nucleon-nucleon part of the recent realistic baryon-baryon interaction (model NSC97e) constructed by the Nijmegen group. The temperatures considered range from 10 to 80 MeV. We report on t… ▽ More We calculate the neutrino mean free path and the Equation of State of pure neutron matter at finite temperature within a selfconsistent scheme based on the Brueckner--Hartree--Fock approximation. We employ the nucleon-nucleon part of the recent realistic baryon-baryon interaction (model NSC97e) constructed by the Nijmegen group. The temperatures considered range from 10 to 80 MeV. We report on the calculation of the mean field, the residual interaction and the neutrino mean free path including short and long range correlations given by the Brueckner--Hartree--Fock plus Random Phase Approximation (BHF+RPA) framework. This is the first fully consistent calculation in hot neutron matter dedicated to neutrino mean free path. We compare systematically our results to those obtain with the D1P Gogny effective interaction, which is independent of the temperature. The main differences between the present calculation and those with nuclear effective interactions come from the RPA corrections to BHF (a factor of about 8) while the temperature lack of consistency accounts for a factor of about 2. △ Less

Submitted 17 July, 2003; originally announced July 2003.

Journal ref: Phys.Rev. C68 (2003) 055806

Gamma Ray Bursts from delayed collapse of neutron stars to quark matter stars

Authors: Z. Berezhiani, I. Bombaci, A. Drago, F. Frontera, A. Lavagno

Abstract: We propose a model to explain how a Gamma Rays Burst can take place days or years after a supernova explosion. Our model is based on the conversion of a pure hadronic star (neutron star) into a star made at least in part of deconfined quark matter. The conversion process can be delayed if the surface tension at the interface between hadronic and deconfined-quark-matter phases is taken into accou… ▽ More We propose a model to explain how a Gamma Rays Burst can take place days or years after a supernova explosion. Our model is based on the conversion of a pure hadronic star (neutron star) into a star made at least in part of deconfined quark matter. The conversion process can be delayed if the surface tension at the interface between hadronic and deconfined-quark-matter phases is taken into account. The nucleation time (i.e. the time to form a critical-size drop of quark matter) can be extremely long if the mass of the star is small. Via mass accretion the nucleation time can be dramaticaly reduced and the star is finally converted into the stable configuration. A huge amount of energy, of the order of 10$^{52}$--10$^{53}$ erg, is released during the conversion process and can produce a powerful Gamma Ray Burst. The delay between the supernova explosion generating the metastable neutron star and the new collapse can explain the delay proposed in GRB990705 and in GRB011211. △ Less

Submitted 13 February, 2003; v1 submitted 12 September, 2002; originally announced September 2002.

Comments: AAS LaTeX, 12 pages, 1 figure, 2 tables Added references and comments

Journal ref: Astrophys.J.586:1250-1253,2003

Microscopic study of neutrino trapping in hyperon stars

Authors: I. Vidaña, I. Bombaci, A. Polls, A. Ramos

Abstract: Employing the most recent parametrization of the baryon-baryon interaction of the Nijmegen group, we investigate, in the framework of the Brueckner--Bethe--Goldstone many-body theory at zero temperature, the influence of neutrino trapping on the composition, equation of state, and structure of neutron stars, relevant to describe the physical conditions of a neutron star immediately after birth (… ▽ More Employing the most recent parametrization of the baryon-baryon interaction of the Nijmegen group, we investigate, in the framework of the Brueckner--Bethe--Goldstone many-body theory at zero temperature, the influence of neutrino trapping on the composition, equation of state, and structure of neutron stars, relevant to describe the physical conditions of a neutron star immediately after birth (protoneutron star). We find that the presence of neutrinos changes significantly the composition of matter delaying the appearance of hyperons and making the equation of state stiffer. We explore the consequences of neutrino trapping on the early evolution of a neutron star and on the nature of the final compact remnant left by the supernova explosion. △ Less

Submitted 30 July, 2003; v1 submitted 4 September, 2002; originally announced September 2002.

Comments: Astronomy & Astrophysics, 399, 687-693 (2003)

Equation of state and magnetic susceptibility of spin polarized isospin asymmetric nuclear matter

Authors: I. Vidana, I. Bombaci

Abstract: Properties of spin polarized isospin asymmetric nuclear matter are studied within the framework of the Brueckner--Hartree--Fock formalism. The single-particle potentials of neutrons and protons with spin up and down are determined for several values of the neutron and proton spin polarizations and the asymmetry parameter. It is found an almost linear and symmetric variation of the single-particl… ▽ More Properties of spin polarized isospin asymmetric nuclear matter are studied within the framework of the Brueckner--Hartree--Fock formalism. The single-particle potentials of neutrons and protons with spin up and down are determined for several values of the neutron and proton spin polarizations and the asymmetry parameter. It is found an almost linear and symmetric variation of the single-particle potentials as increasing these parameters. An analytic parametrization of the total energy per particle as a function of the asymmetry and spin polarizations is constructed. This parametrization is employed to compute the magnetic susceptibility of nuclear matter for several values of the asymmetry from neutron to symmetric matter. The results show no indication of a ferromagnetic transition at any density for any asymmetry of nuclear matter. △ Less

Submitted 22 March, 2002; originally announced March 2002.

Comments: 23 pages, 8 figures, 2 tables (submitted to Phys. Rev. C)

Journal ref: Phys.Rev. C66 (2002) 045801

Timing evolution of accreting strange stars

Authors: D. Blaschke, I. Bombaci, H. Grigorian, G. Poghosyan

Abstract: It has been suggested that the QPO phenomenon in LMXB's could be explained when the central compact object is a strange star. In this work we investigate within a standard model for disk accretion whether the observed clustering of spin frequencies in a narrow band is in accordance with this hypothesis. We show that frequency clustering occurs for accreting strange stars when typical values of t… ▽ More It has been suggested that the QPO phenomenon in LMXB's could be explained when the central compact object is a strange star. In this work we investigate within a standard model for disk accretion whether the observed clustering of spin frequencies in a narrow band is in accordance with this hypothesis. We show that frequency clustering occurs for accreting strange stars when typical values of the parameters of magnetic field initial strength and decay time, accretion rate are chosen. In contrast to hybrid star accretion no mass clustering effect is found. △ Less

Submitted 10 January, 2002; v1 submitted 19 October, 2001; originally announced October 2001.

Comments: 10 pages, 3 figures, version accepted for publication in New Astronomy

Report number: MPG-VT-UR 222/01

Journal ref: New Astron. 7 (2002) 107-112

Asymmetric Nuclear Matter from Extended Brueckner-Hartree-Fock Approach

Authors: W. Zuo, I. Bombaci, U. Lombardo

Abstract: The properties of isospin-asymmetric nuclear matter have been investigated in the framework of the extended Brueckner-Hartree-Fock approximation at zero temperature. Self-consistent calculations using the Argonne $V_{14}$ interaction are reported for several asymmetry parameters $β= \frac{N - Z}{A}$ ranging from symmetric nuclear matter to pure neutron matter. The binding energy per nucleon fulf… ▽ More The properties of isospin-asymmetric nuclear matter have been investigated in the framework of the extended Brueckner-Hartree-Fock approximation at zero temperature. Self-consistent calculations using the Argonne $V_{14}$ interaction are reported for several asymmetry parameters $β= \frac{N - Z}{A}$ ranging from symmetric nuclear matter to pure neutron matter. The binding energy per nucleon fulfills the $β^2$ law in the whole asymmetry range. The symmetry energy is calculated for different densities and discussed in comparison with other predictions. At the saturation point it is in fairly good agreement with the empirical value. The present approximation, based on the Landau definition of quasiparticle energy, is investigated in terms of the Hugenholtz-Van Hove theorem, which is proved to be fulfilled with a good accuracy at various asymmetries. The isospin dependence of the single-particle properties is discussed, including mean field, effective mass, and mean free path of neutrons and protons. The isospin effects in nuclear physics and nuclear astrophysics are briefly discussed. △ Less

Submitted 15 February, 2001; originally announced February 2001.

Comments: 26 pages, 11 figures

Journal ref: Phys.Rev. C60 (1999) 024605

Rapidly rotating strange stars for a new equation of state of strange quark matter

Authors: I. Bombaci, A. V. Thampan, B. Datta

Abstract: For a new equation of state of strange quark matter, we construct equilibrium sequences of rapidly rotating strange stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. We also calculate equilibrium sequences for a constant value of $Ω$ corresponding to the most rapidly rotating pulsar PSR 1937 + 21. In addition to this, we calc… ▽ More For a new equation of state of strange quark matter, we construct equilibrium sequences of rapidly rotating strange stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. We also calculate equilibrium sequences for a constant value of $Ω$ corresponding to the most rapidly rotating pulsar PSR 1937 + 21. In addition to this, we calculate the radius of the marginally stable orbit and its dependence on $Ω$, relevant for modeling of kilo-Hertz quasi-periodic oscillations in X-ray binaries. △ Less

Submitted 20 September, 2000; originally announced September 2000.

Comments: Two figures, uses psbox.tex and emulateapj5.sty

Report number: IUCAA-17/00

Journal ref: Astrophys.J. 541 (2000) L71

Do strange stars exist in the Universe?

Authors: Ignazio Bombaci

Abstract: Definitely, an affirmative answer to this question would have implications of fundamental importance for astrophysics (a new class of compact stars), and for the physics of strong interactions (deconfined phase of quark matter, and strange matter hypothesis). In the present work, we use observational data for the newly discovered millisecond X-ray pulsar SAX J1808.4-3658 and for the atoll source… ▽ More Definitely, an affirmative answer to this question would have implications of fundamental importance for astrophysics (a new class of compact stars), and for the physics of strong interactions (deconfined phase of quark matter, and strange matter hypothesis). In the present work, we use observational data for the newly discovered millisecond X-ray pulsar SAX J1808.4-3658 and for the atoll source 4U 1728-34 to constrain the radius of the underlying compact stars. Comparing the mass-radius relation of these two compact stars with theoretical models for both neutron stars and strange stars, we argue that a strange star model is more consistent with SAX J1808.4-3658 and 4U 1728-34, and suggest that they are likely strange star candidates. △ Less

Submitted 29 February, 2000; originally announced February 2000.

Comments: In memory of Bhaskar Datta. -- Invited talk at the Pacific Rim Conference on Stellar Astrophysics (Hong Kong, aug. 1999)

Conversion of neutron stars to strange stars as the central engine of gamma-ray bursts

Authors: Ignazio Bombaci, Bhaskar Datta

Abstract: We study the conversion of a neutron star to a strange star as a possible energy source for gamma-ray bursts. We use different recent models for the equation of state of neutron star matter and strange quark matter. We show that the total amount of energy liberated in the conversion is in the range of (1-4) 10^{53} ergs (one order of magnitude larger than previous estimates) and is in agreement… ▽ More We study the conversion of a neutron star to a strange star as a possible energy source for gamma-ray bursts. We use different recent models for the equation of state of neutron star matter and strange quark matter. We show that the total amount of energy liberated in the conversion is in the range of (1-4) 10^{53} ergs (one order of magnitude larger than previous estimates) and is in agreement with the energy required to power gamma-ray burst sources at cosmological distances. △ Less

Submitted 27 January, 2000; originally announced January 2000.

Comments: ApJ, 530, 2000 February 20, Lxxx (in press)

Journal ref: Astrophys.J. 530 (2000) L69

Possible signatures for strange stars in stellar X-ray binaries

Authors: Bhaskar Datta, Arun V. Thampan, Ignazio Bombaci

Abstract: Kilohertz quasi-periodic brightness oscillations (kHz QPOs) observed in certain X-ray burst sources may represent Keplerian frequencies in the inner regions of the accretion disk in such systems. If this assumption is strictly adhered to, we show here that if the central accretor in stellar X-ray burst sources is a strange star (made up of u, d and s quarks in beta equilibrium, referred to as st… ▽ More Kilohertz quasi-periodic brightness oscillations (kHz QPOs) observed in certain X-ray burst sources may represent Keplerian frequencies in the inner regions of the accretion disk in such systems. If this assumption is strictly adhered to, we show here that if the central accretor in stellar X-ray burst sources is a strange star (made up of u, d and s quarks in beta equilibrium, referred to as strange matter) then the calculated QPO frequencies are reconcilable with the observed QPO frequencies (corresponding to the highest frequency of 1.22 kHz, observed so far from the source 4U 1636-53) only for particular values of the QCD-related parameters which describe the equation of state of strange matter. We demonstrate that QPO frequencies in the very high range (1.9-3.1) kHz can be understood in terms of a (non- magnetized) strange star X-ray binary (SSXB) rather than a neutron star X-ray binary (NSXB). Future discovery of such high frequency QPOs from X-ray burst sources will constitute a new astrophysical di- agnostic for identifying solar mass range stable strange stars in our galaxy. △ Less

Submitted 8 December, 1999; originally announced December 1999.

Comments: 4 pages, 2 figs., uses psbox.tex, submitted to A&A

Is SAX J1808.4-3658 a Strange Star ?

Authors: X. -D. Li, I. Bombaci, Mira Dey, Jishnu Dey, E. P. J. van den Heuvel

Abstract: One of the most important questions in the study of compact objects is the nature of pulsars, including whether they are composed of $β$-stable nuclear matter or strange quark matter. Observations of the newly discovered millisecond X-ray pulsar \sax with the Rossi X-Ray Timing Explorer place firm constraint on the radius of the compact star. Comparing the mass - radius relation of \sax with the… ▽ More One of the most important questions in the study of compact objects is the nature of pulsars, including whether they are composed of $β$-stable nuclear matter or strange quark matter. Observations of the newly discovered millisecond X-ray pulsar \sax with the Rossi X-Ray Timing Explorer place firm constraint on the radius of the compact star. Comparing the mass - radius relation of \sax with the theoretical mass - radius relation for neutron stars and for strange stars, we find that a strange star model is more consistent with SAX J1808.4-3658, and suggest that it is a likely strange star candidate. △ Less

Submitted 21 May, 1999; v1 submitted 16 May, 1999; originally announced May 1999.

Comments: 5 pages, Latex, 1 figure, corrected for some typos

Journal ref: Phys.Rev.Lett. 83 (1999) 3776-3779

Strange Stars with Realistic Quark Vector Interaction and Phenomenological Density-dependent Scalar Potential

Authors: Mira Dey, Ignazio Bombaci, Jishnu Dey, Subharthi Ray, B. C. Samanta

Abstract: We derive an equation of state (EOS) for strange matter, starting from an interquark potential which (i) has asymptotic freedom built into it, (ii) shows confinement at zero baryon density and deconfinement at high density and (iii) gives a stable configuration for chargeless, beta--stable quark matter. This EOS is then used to calculate the structure of Strange Stars, and in particular their ma… ▽ More We derive an equation of state (EOS) for strange matter, starting from an interquark potential which (i) has asymptotic freedom built into it, (ii) shows confinement at zero baryon density and deconfinement at high density and (iii) gives a stable configuration for chargeless, beta--stable quark matter. This EOS is then used to calculate the structure of Strange Stars, and in particular their mass-radius relation. Our present results confirm and reinforce the recent claim by Li et al (Astron. and Astrophys. 303 (1995) L1) and Bombaci (Phys.Rev. C55 (1997) 1587) that the compact objects associated with the x-ray pulsar Her X-1, and with the x-ray burster 4U 1820-30 are strange stars. △ Less

Submitted 6 October, 1998; v1 submitted 5 October, 1998; originally announced October 1998.

Comments: 11 Pages, 2 figures, On-line abstract changed and full reference given instead of tex- type. E-mail : bombaci@pi.infn.it, deyjm@giascl01.vsnl.net.in, Physics Letters B (in press)

Journal ref: Phys.Lett. B438 (1998) 123-128; Addendum-ibid. B447 (1999) 352-353

Microscopic nuclear equation of state with three-body forces and neutron star structure

Authors: M. Baldo, I. Bombaci, G. F. Burgio

Abstract: We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter, derived from the Brueckner-Bethe-Goldstone many-body theory with explicit three-body forces. We use the Argonne AV14 and the Paris two-body nuclear force, implemented by the Urbana model for the three-body force. We obtain a maximum mass configuration wit… ▽ More We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter, derived from the Brueckner-Bethe-Goldstone many-body theory with explicit three-body forces. We use the Argonne AV14 and the Paris two-body nuclear force, implemented by the Urbana model for the three-body force. We obtain a maximum mass configuration with $ M_{max} = 1.8 M_{\sun}$ ($M_{max} = 1.94 M_{\sun}$) when the AV14 (Paris) interaction is used. They are both consistent with the observed range of NS masses. The onset of direct Urca processes occurs at densities $n \geq 0.65~fm^{-3}$ for the AV14 potential and $n \geq 0.54~fm^{-3}$ for the Paris potential. Therefore, NS's with masses above $M^{Urca} = 1.4 M_{\sun}$ for the AV14 and $M^{Urca} = 1.24 M_{\sun}$ for the Paris potential can undergo very rapid cooling, depending on the strength of superfluidity in the interior of the NS. The comparison with other microscopic models for the EOS shows noticeable differences. △ Less

Submitted 25 July, 1997; originally announced July 1997.

Comments: LaTeX, 10 pages, 7 figures included, accepted for publication in Astronomy & Astrophysics

Report number: INFN-CT-06/97

Microscopic Nuclear Equation of State with Three-Body Forces and Neutron Star Structure

Authors: M. Baldo, G. F. Burgio, I. Bombaci

Abstract: We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter. The EOS is computed in the framework of the Brueckner--Bethe--Goldstone many--body theory. We introduce three-body forces in order to reproduce the correct saturation point of nuclear matter. A microscopic well behaved EOS is derived. We obtain a maximum… ▽ More We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter. The EOS is computed in the framework of the Brueckner--Bethe--Goldstone many--body theory. We introduce three-body forces in order to reproduce the correct saturation point of nuclear matter. A microscopic well behaved EOS is derived. We obtain a maximum mass configuration with $M_{max} = 1.8 M_\odot$, a radius $R = 9.7$ km and a central density $n_c = 1.34~fm^{-3}$. We find the proton fraction exceeds the critical value $x^{Urca}$, for the onset of direct Urca processes, at densities $n \geq 0.45~fm^{-3}$. Therefore, in our model, NS's with masses above $M^{Urca} = 0.96 M_\odot$ can undergo very rapid cooling depending on whether or not nucleon superfluidity in the interior of the NS takes place. A comparison with other microscopic models for the EOS is done, and neutron star structure is calculated for these models too. △ Less

Submitted 10 July, 1996; originally announced July 1996.

Comments: LaTeX, 10 pages, 4 Postscript figures included

Report number: INFN-CT-08/96

Composition and Structure of Protoneutron Stars

Authors: Madappa Prakash, Ignazio Bombaci, Manju Prakash, Paul J. Ellis, James M. Lattimer, Roland Knorren

Abstract: We investigate the structure of neutron stars shortly after they are born, when the entropy per baryon is of order 1 or 2 and neutrinos are trapped on dynamical timescales. In all cases, the thermal effects for an entropy per baryon of order 2 or less are small when considering the maximum neutron star mass. Neutrino trapping, however, significantly changes the maximum mass due to the abundance… ▽ More We investigate the structure of neutron stars shortly after they are born, when the entropy per baryon is of order 1 or 2 and neutrinos are trapped on dynamical timescales. In all cases, the thermal effects for an entropy per baryon of order 2 or less are small when considering the maximum neutron star mass. Neutrino trapping, however, significantly changes the maximum mass due to the abundance of electrons. When matter is allowed to contain only nucleons and leptons, trapping decreases the maximum mass by an amount comparable to, but somewhat larger than, the increase due to finite entropy. When matter is allowed to contain strongly interacting negatively charged particles, in the form of strange baryons, a kaon condensate, or quarks, trapping instead results in an increase in the maximum mass of order $0.2M_\odot$, which adds to the effects of finite entropy. The presence of negatively-charged particles has two major implications. First, the value of the maximum mass will decrease during the early evolution of a neutron star as it loses trapped neutrinos, so that if a black hole forms, it either does so immediately after the bounce or it is delayed for a neutrino diffusion timescale of $\sim 10$ s. The latter case is most likely if the maximum mass of the hot star with trapped neutrinos is near $1.5M_\odot$. In the absence of negatively-charged hadrons, black hole formation would be due to accretion and therefore is likely to occur only immediately after bounce. Second, the appearance of hadronic negative charges results in a general softening of the equation of state that may be observable in the neutrino luminosities and average energies. Further, these additional negative charges decrease the electron fraction and may be observed in the relative excess of electron neutrinos compared to other neutrinos. △ Less

Submitted 27 March, 1996; originally announced March 1996.

Comments: 83 pages, 30 postscript figures, Physics Reports, to be published

Report number: SUNY-NTG-96-11; NUC-MINN-93/23-T

Journal ref: Phys.Rept. 280 (1997) 1-77