Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies

Camelio, Giovanni; Lovato, Alessandro; Gualtieri, Leonardo; Benhar, Omar; Pons, José A.; Ferrari, Valeria

doi:10.1103/physrevd.96.043015

Cited by 73 publications

(64 citation statements)

References 60 publications

(176 reference statements)

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“…Thanks to its proximity of about 51 kpc to the Earth, neutrino burst events from the core collapse of the progenitor star could be recorded at the underground laboratories Irvine-Michigan-Brookhaven (IMB), Kamiokande II, and Baksan separately [1]. The observed burst duration of about 12 seconds, individual energies up to 40 MeV, as well as the integrated total energy of O(10 53 erg), confirmed the standard picture of neutrino cooling of the proto-neutron star (PNS) [2][3][4]. A proto-neutron star is formed when the collapsing stellar core of the progenitor star reaches nuclear saturation density.…”

Section: Introductionmentioning

confidence: 59%

Supernovae and Weinberg’s Higgs portal dark radiation and dark matter

2017

J. High Energ. Phys.

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The observed burst duration and energies of the neutrinos from Supernova 1987A strongly limit the possibility of any weakly-interacting light particle species being produced in the proto-neutron star (PNS) core and leading to efficient energy loss. We reexamine this constraint on Weinberg's Higgs portal model, in which the dark radiation particles (the Goldstone bosons) and the dark matter candidate (a Majorana fermion) interact with Standard Model (SM) fields solely through the mixing of the SM Higgs boson and a light Higgs boson. In order for the Goldstone bosons to freely stream out of the PNS core region, the Higgs portal coupling has to be about a factor of 4-9 smaller than the current collider bound inferred from the SM Higgs invisible decay width. We find that in the energy loss rate calculations, results obtained by using the one-pion exchange (OPE) approximation and the SP07 global fits for the nucleon-nucleon total elastic cross section differ only by a factor 3. The SN 1987A constraints surpass those set by laboratory experiments or by the energy loss arguments in other astrophysical objects such as the gamma-ray bursts, even with other nuclear uncertainties taken into account. Furthermore, the SN 1987A constraints are comparable to bounds from the latest dark matter direct search for low-mass WIMPs ( 10 GeV.)

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Section: Introductionmentioning

confidence: 59%

Supernovae and Weinberg’s Higgs portal dark radiation and dark matter

2017

J. High Energ. Phys.

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“…For comparison, the green line shows the profile of a hypermassive neutron star (HMNS) remnant 12.1 ms after a neutron star merger from the simulations of Sekiguchi et al (2011) using the STOS EOS. The orange and purple lines show the profiles of a proto-neutron star (PNS) 200 ms after the bounce in a core-collapse supernova simulation and at the end of de-leptonization in the same simulation, both with a bulk version of the LS EOS (Camelio et al 2017). thermal contribution, P th , is defined as P total − P cold for the same proton fraction.…”

Section: Overview Of Finite-temperature Eosmentioning

confidence: 99%

“…phase (Camelio et al 2017). We note that these profiles are not necessarily calculated at Y p = 0.1, but we include them nevertheless to show the approximate relevant temperatures and densities for such phenomena.…”

Section: Overview Of Finite-temperature Eosmentioning

confidence: 99%

Finite-temperature Extension for Cold Neutron Star Equations of State

Raithel

Özel

Psaltis

2019

ApJ

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Observations of isolated neutron stars place constraints on the equation of state (EOS) of cold, neutron-rich matter, while nuclear physics experiments probe the EOS of hot, symmetric matter. Many dynamical phenomena, such as core-collapse supernovae, the formation and cooling of protoneutron stars, and neutron star mergers, lie between these two regimes and depend on the EOS at finite temperatures for matter with varying proton fractions. In this paper, we introduce a new framework to accurately calculate the thermal pressure of neutron-proton-electron matter at arbitrary density, temperature, and proton fraction. This framework can be expressed using a set of five physicallymotivated parameters that span a narrow range of values for realistic EOS and are able to capture the leading-order effects of degenerate matter on the thermal pressure. We base two of these parameters on a new approximation of the Dirac effective mass, with which we reproduce the thermal pressure to within 30% for a variety of realistic EOS at densities of interest. Three additional parameters, based on the behavior of the symmetry energy near the nuclear saturation density, allow for the extrapolation of any cold EOS in β-equilibrium to arbitrary proton fractions. Our model thus allows a user to extend any cold nucleonic EOS, including piecewise-polytropes, to arbitrary temperature and proton fraction, for use in calculations and numerical simulations of astrophysical phenomena. We find that our formalism is able to reproduce realistic finite-temperature EOS with errors of 20% and offers a 1 − 3 orders-of-magnitude improvement over existing ideal-fluid models.

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“…Unlike a cold NS, the perturbative analyses in the case of a PNS are only a few [37][38][39][40]. This may come from the difficulty for providing the background model for the PNS.…”

Section: Introductionmentioning

confidence: 99%

Probing mass-radius relation of protoneutron stars from gravitational-wave asteroseismology

et al. 2017

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The gravitational-wave (GW) asteroseismology is a powerful technique for extracting interior information of compact objects. In this work, we focus on spacetime modes, the so-called w modes, of GWs emitted from a proto-neutron star (PNS) in the postbounce phase of core-collapse supernovae. Using results from recent three-dimensional supernova models, we study how to infer the properties of the PNS based on a quasi-normal mode analysis in the context of the GW asteroseismology. We find that the w 1 -mode frequency multiplied by the PNS radius is expressed as a linear function with respect to the ratio of the PNS mass to the PNS radius. This relation is insensitive to the nuclear equation of state (EOS) employed in this work. Combining with another universal relation of the f-mode oscillations, we point out that the time dependent mass-radius relation of the PNS can be obtained by observing both the f-and w 1 -mode GWs simultaneously. Our results suggest that the simultaneous detection of the two modes could provide a new probe into finite-temperature nuclear EOS that predominantly determines the PNS evolution.

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Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies

Cited by 73 publications

References 60 publications

Supernovae and Weinberg’s Higgs portal dark radiation and dark matter

Supernovae and Weinberg’s Higgs portal dark radiation and dark matter

Finite-temperature Extension for Cold Neutron Star Equations of State

Probing mass-radius relation of protoneutron stars from gravitational-wave asteroseismology

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