Radio SNRs in the Magellanic Clouds as probes of shock microphysics

Supernova remnants (SNRs) in Local Group galaxies offer unique insights into the origin of different types of supernovae. In order to take full advantage of these insights, one must understand the intrinsic and environmental diversity of SNRs in the context of their host galaxies. We introduce a semi-analytic model that reproduces the statistical properties of a radio continuum-selected SNR population, taking into account the detection limits of radio surveys, the range of SN kinetic energies, the measured ISM and stellar mass distribution in the host galaxy from multi-wavelength images and the current understanding of electron acceleration and magnetic field amplification in SNR shocks from first-principle kinetic simulations. Applying our model to the SNR population in M33, we reproduce the SNR radio luminosity function with a median SN rate of ∼ 3.1 × 10 −3 per year and an electron acceleration efficiency, e ∼ 4.2 × 10 −3 . We predict that the radio visibility times of ∼ 70% of M33 SNRs will be determined by their Sedov-Taylor lifetimes, and correlated with the measured ISM column density, N H (t vis ∝ N −a H , with a ∼ 0.33) while the remaining will have visibility times determined by the detection limit of the radio survey. These observational constraints on the visibility time of SNRs will allow us to use SNR catalogs as 'SN surveys' to calculate SN rates and delay time distributions in the Local Group.

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Supernova remnants in the Local Group – I. A model for the radio luminosity function and visibility times of supernova remnants

Sarbadhicary

Badenes

Chomiuk

et al. 2016

Monthly Notices of the Royal Astronomical Society

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Cosmic magnetism in centimeter- and meter-wavelength radio astronomy

Akahori

Nakanishi

Sofue

et al. 2017

Publications of the Astronomical Society of Japan

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Magnetic field is ubiquitous in the Universe and it plays essential roles in various astrophysical phenomena, yet its real origin and evolution are poorly known. This article reviews current understanding of magnetic fields in the interstellar medium, the Milky Way Galaxy, external galaxies, active galactic nuclei, clusters of galaxies, and the cosmic web. Particularly, the review concentrates on the achievements that have been provided by centimeter and meter wavelength radio observations. The article also introduces various methods to analyze linear polarization data, including synchrotron radiation, Faraday rotation, depolarization, and Faraday tomography.

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Survival Times of Supramassive Neutron Stars Resulting from Binary Neutron Star Mergers

Beniamini

2021

ApJ

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A binary neutron star (BNS) merger can lead to various outcomes, from indefinitely stable neutron stars, through supramassive neutron stars (SMNSs) or hypermassive neutron stars supported only temporarily against gravity, to black holes formed promptly after the merger. Up-to-date constraints on the BNS total mass and the neutron star equation of state suggest that a long-lived SMNS may form in ∼0.45-0.9 of BNS mergers. A maximally rotating SMNS needs to lose ∼(3-6) × 10 52 erg of its rotational energy before it collapses, on a fraction of the spin-down timescale. An SMNS formation imprints on the electromagnetic counterparts to the BNS merger. However, a comparison with observations reveals tensions. First, the distribution of collapse times is too wide and that of released energies too narrow (and the energy itself too large) to explain the observed distributions of internal X-ray plateaus, invoked as evidence for SMNS-powered energy injection. Second, the immense energy injection into the blast wave should lead to extremely bright radio transients, which previous studies found to be inconsistent with deep radio observations of short gamma-ray bursts (GRBs). Furthermore, we show that upcoming all-sky radio surveys will constrain the extracted energy distribution, independently of a GRB jet formation. Our results can be self-consistently understood, provided that most BNS merger remnants collapse shortly after formation (even if their masses are low enough to allow for SMNS formation). This naturally occurs if the remnant retains half or less of its initial energy by the time it enters solid-body rotation.Unified Astronomy Thesaurus concepts: Gamma-ray bursts (629); Neutron stars (1108); Gravitational waves (678)

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Radio SNRs in the Magellanic Clouds as probes of shock microphysics

Cited by 3 publications

References 36 publications

Supernova remnants in the Local Group – I. A model for the radio luminosity function and visibility times of supernova remnants

Supernova remnants in the Local Group – I. A model for the radio luminosity function and visibility times of supernova remnants

Cosmic magnetism in centimeter- and meter-wavelength radio astronomy

Survival Times of Supramassive Neutron Stars Resulting from Binary Neutron Star Mergers

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