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Universe
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Fundamental Processes in Neutron Stars and Supernovae
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Fundamental Processes in Neutron Stars and Supernovae

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Compact Objects".

Deadline for manuscript submissions: closed (30 April 2021) | Viewed by 8027

Special Issue Editors

Prof. Marcello Baldo

E-Mail Website
Guest Editor
INFN, Sez. Catania, via S. Sofia 64, 95123 Catania, Italy
Interests: nuclear physics; nuclear astrophysics; astrophysical compact objects; nuclear superfluidity; nuclear matter; many-body theory
Dr. Isaac Vidaña

E-Mail Website
Guest Editor
INFN Sezione di Catania, Dipartimento di Fisica, Università di Catania, Via Santa Sofia 64, I-95123 Catania, Italy
Interests: nuclear physics; neutron stars
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

In the last few years, we have made spectacular progress in our understanding of the physics of Neutron Stars and Supernovae, both from observations and from theory. Our understanding of these compact objects amply relies on our knowledge of the microphysics of the fundamental processes that determine their structure and dynamics. In this respect, both observations and theoretical analysis are crucial to improving our capacity to predict the rate and dynamics of each one of these processes, as well as to discovering new phenomena. The aim of this Special Issue of Universe is to report on the latest developments and to stimulate new ones in the field. These topics include but are not limited to the following:

  • transport in neutron stars and neutron star mergers;
  • neutrino trapping and emission in neutron stars;
  • neutrino emissions and dynamics in supernovae;
  • nucleosynthesis in supernovae simulations;
  • neutron star cooling;
  • gravitational waves from neutron star mergers;
  • gravitational waves from neutron star oscillations;
  • magnetic field structure and dynamics in neutron star formation;
  • and onset of quark matter in neutron stars

References

  1. The Physics and Astrophysics of Neutron Stars. In Astrophysics and Space Science Library; L Rezzolla, P. Pizzochero, D. I. Jones, N. Rea and I. Vidana; Springer: Berlin, Germany, 2018.
  2. A. G. Chaves and T. Hinderer, J.Phys. Probing the Equation of State of Neutron star Matter with Gravitational Waves from Binary Inspirals in Light of GW170817: a brief review. arXiv:123002 G46(2019).
  3. A. Arada et al. The Boltzmann-Radiation-hydrodynamics Simulations of the Core-collapse Supernova with the Different Equations of State: the Role of Nuclear Composition and the Behavior of Neutrinos. arXive:2003.08630 (2020).
  4. J. Bliss et al. Nuclear Physics Uncertainties in Neutrino-driven, Neutron-rich Supernova Ejecta. arXiv:2001.02085(2020).
  5. P. Shternin et al. In-medium Enhancement of the Modified Urca Neutrino Reaction Rates. PLB 2018

Prof. Marcello Baldo
Dr. Isaac Vidaña
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • Neutron Stars and Supernovae
  • Microphysics in Neutron Stars and Supernovae
  • Transport Processes
  • Cooling of Neutron Stars
  • Neutrino Dynamics
  • Neutron Star Mergers
  • Neutron Star Oscillations
  • Gravitational Waves
  • Collapse Dynamics in Supernovae

Published Papers (4 papers)

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Research

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20 pages, 715 KiB  
Article
Transport Coefficients of Hyperonic Neutron Star Cores
by Peter Shternin and Isaac Vidaña
Universe 2021, 7(6), 203; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7060203 - 20 Jun 2021
Cited by 4 | Viewed by 1395
Abstract
We consider transport properties of the hypernuclear matter in neutron star cores. In particular, we calculate the thermal conductivity, the shear viscosity, and the momentum transfer rates for npΣ−Λeμ composition of dense matter in β–equilibrium for baryon [...] Read more.
We consider transport properties of the hypernuclear matter in neutron star cores. In particular, we calculate the thermal conductivity, the shear viscosity, and the momentum transfer rates for npΣ−Λeμ composition of dense matter in β–equilibrium for baryon number densities in the range 0.1–1 fm−3. The calculations are based on baryon interactions treated within the framework of the non-relativistic Brueckner-Hartree-Fock theory. Bare nucleon-nucleon (NN) interactions are described by the Argonne v18 phenomenological potential supplemented with the Urbana IX three-nucleon force. Nucleon-hyperon (NY) and hyperon-hyperon (YY) interactions are based on the NSC97e and NSC97a models of the Nijmegen group. We find that the baryon contribution to transport coefficients is dominated by the neutron one as in the case of neutron star cores containing only nucleons. In particular, we find that neutrons dominate the total thermal conductivity over the whole range of densities explored and that, due to the onset of Σ− which leads to the deleptonization of the neutron star core, they dominate also the shear viscosity in the high density region, in contrast with the pure nucleonic case where the lepton contribution is always the dominant one. Full article
(This article belongs to the Special Issue Fundamental Processes in Neutron Stars and Supernovae)
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21 pages, 442 KiB  
Article
Heating in Magnetar Crusts from Electron Captures
by Nicolas Chamel, Anthea Francesca Fantina, Lami Suleiman, Julian-Leszek Zdunik and Pawel Haensel
Universe 2021, 7(6), 193; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7060193 - 08 Jun 2021
Cited by 8 | Viewed by 1950
Abstract
The persistent thermal luminosity of magnetars and their outbursts suggest the existence of some internal heat sources located in their outer crust. The compression of matter accompanying the decay of the magnetic field may trigger exothermic electron captures and, possibly, pycnonuclear fusions of [...] Read more.
The persistent thermal luminosity of magnetars and their outbursts suggest the existence of some internal heat sources located in their outer crust. The compression of matter accompanying the decay of the magnetic field may trigger exothermic electron captures and, possibly, pycnonuclear fusions of light elements that may have been accreted onto the surface from the fallback of supernova debris, from a disk or from the interstellar medium. This scenario bears some resemblance to deep crustal heating in accreting neutron stars, although the matter composition and the thermodynamic conditions are very different. The maximum possible amount of heat that can be released by each reaction and their locations are determined analytically taking into account the Landau–Rabi quantization of electron motion. Numerical results are also presented using experimental, as well as theoretical nuclear data. Whereas the heat deposited is mainly determined by atomic masses, the locations of the sources are found to be very sensitive to the magnetic field strength, thus providing a new way of probing the internal magnetic field of magnetars. Most sources are found to be concentrated at densities 1010–1011 g cm−3 with heat power W∞∼1035–1036 erg/s, as found empirically by comparing cooling simulations with observed thermal luminosity. The change of magnetic field required to trigger the reactions is shown to be consistent with the age of known magnetars. This suggests that electron captures and pycnonuclear fusion reactions may be a viable heating mechanism in magnetars. The present results provide consistent microscopic inputs for neutron star cooling simulations, based on the same model as that underlying the Brussels-Montreal unified equations of state. Full article
(This article belongs to the Special Issue Fundamental Processes in Neutron Stars and Supernovae)
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15 pages, 1759 KiB  
Article
A New Mass Model for Nuclear Astrophysics: Crossing 200 keV Accuracy
by Matthew Shelley and Alessandro Pastore
Universe 2021, 7(5), 131; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7050131 - 04 May 2021
Cited by 19 | Viewed by 1792
Abstract
By using a machine learning algorithm, we present an improved nuclear mass table with a root mean square deviation of less than 200 keV. The model is equipped with statistical error bars in order to compare with available experimental data. We use the [...] Read more.
By using a machine learning algorithm, we present an improved nuclear mass table with a root mean square deviation of less than 200 keV. The model is equipped with statistical error bars in order to compare with available experimental data. We use the resulting model to predict the composition of the outer crust of a neutron star. By means of simple Monte Carlo methods, we propagate the statistical uncertainties of the mass model to the equation of state of the system. Full article
(This article belongs to the Special Issue Fundamental Processes in Neutron Stars and Supernovae)
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Review

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24 pages, 613 KiB  
Review
A Gravitational-Wave Perspective on Neutron-Star Seismology
by Nils Andersson
Universe 2021, 7(4), 97; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7040097 - 11 Apr 2021
Cited by 23 | Viewed by 2233
Abstract
We provide a bird’s-eye view of neutron-star seismology, which aims to probe the extreme physics associated with these objects, in the context of gravitational-wave astronomy. Focussing on the fundamental mode of oscillation, which is an efficient gravitational-wave emitter, we consider the seismology aspects [...] Read more.
We provide a bird’s-eye view of neutron-star seismology, which aims to probe the extreme physics associated with these objects, in the context of gravitational-wave astronomy. Focussing on the fundamental mode of oscillation, which is an efficient gravitational-wave emitter, we consider the seismology aspects of a number of astrophysically relevant scenarios, ranging from transients (like pulsar glitches and magnetar flares), to the dynamics of tides in inspiralling compact binaries and the eventual merged object and instabilities acting in isolated, rapidly rotating, neutron stars. The aim is not to provide a thorough review, but rather to introduce (some of) the key ideas and highlight issues that need further attention. Full article
(This article belongs to the Special Issue Fundamental Processes in Neutron Stars and Supernovae)
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