Neutron-mirror neutron mixing and neutron stars

Abstract The oscillation of neutron n into mirror neutron $$n'$$ n ′ , its mass degenerate partner from dark mirror sector, can gradually transform the neutron stars into the mixed stars consisting in part of mirror dark matter. In quark stars $$n-n'$$ n - n ′ transitions are suppressed. W...

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Autores principales:	Zurab Berezhiani, Riccardo Biondi, Massimo Mannarelli, Francesco Tonelli
Formato:	article
Lenguaje:	EN
Publicado:	SpringerOpen 2021
Materias:	Astrophysics QB460-466 Nuclear and particle physics. Atomic energy. Radioactivity QC770-798
Acceso en línea:	https://doaj.org/article/2b8bbe9e261b41fcb36ac06f39a0a888
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spelling	oai:doaj.org-article:2b8bbe9e261b41fcb36ac06f39a0a8882021-11-28T12:12:08ZNeutron-mirror neutron mixing and neutron stars10.1140/epjc/s10052-021-09806-11434-60441434-6052https://doaj.org/article/2b8bbe9e261b41fcb36ac06f39a0a8882021-11-01T00:00:00Zhttps://doi.org/10.1140/epjc/s10052-021-09806-1https://doaj.org/toc/1434-6044https://doaj.org/toc/1434-6052Abstract The oscillation of neutron n into mirror neutron $$n'$$ n ′ , its mass degenerate partner from dark mirror sector, can gradually transform the neutron stars into the mixed stars consisting in part of mirror dark matter. In quark stars $$n-n'$$ n - n ′ transitions are suppressed. We study the structure of mixed stars and derive the mass-radius scaling relations between the configurations of purely neutron star and maximally mixed star (MMS) containing equal amounts of ordinary and mirror components. In particular, we show that the MMS masses can be at most $$M^{\mathrm{max}}_{NS}/\sqrt{2}$$ M NS max / 2 , where $$M^\mathrm{max}_{NS}$$ M NS max is a maximum mass of a pure neutron star allowed by a given equation of state. We evaluate $$n-n'$$ n - n ′ transition rate in neutron stars, and show that various astrophysical limits on pulsar properties exclude the transition times in a wide range $$10^{5}\,\text {year}< \tau _\varepsilon < 10^{15}\,\text {year}$$ 10 5 year < τ ε < 10 15 year . For short transition times, $$\tau _\varepsilon < 10^5$$ τ ε < 10 5 year, the different mixed stars of the same mass can have different radii, depending on their age, which possibility can be tested by the NICER measurements. We also discuss subtleties related with the possible existence of mixed quark stars, and possible implications for the gravitational waves from the neutron star mergers and associated electromagnetic signals.Zurab BerezhianiRiccardo BiondiMassimo MannarelliFrancesco TonelliSpringerOpenarticleAstrophysicsQB460-466Nuclear and particle physics. Atomic energy. RadioactivityQC770-798ENEuropean Physical Journal C: Particles and Fields, Vol 81, Iss 11, Pp 1-23 (2021)
institution	DOAJ
collection	DOAJ
language	EN
topic	Astrophysics QB460-466 Nuclear and particle physics. Atomic energy. Radioactivity QC770-798
spellingShingle	Astrophysics QB460-466 Nuclear and particle physics. Atomic energy. Radioactivity QC770-798 Zurab Berezhiani Riccardo Biondi Massimo Mannarelli Francesco Tonelli Neutron-mirror neutron mixing and neutron stars
description	Abstract The oscillation of neutron n into mirror neutron $$n'$$ n ′ , its mass degenerate partner from dark mirror sector, can gradually transform the neutron stars into the mixed stars consisting in part of mirror dark matter. In quark stars $$n-n'$$ n - n ′ transitions are suppressed. We study the structure of mixed stars and derive the mass-radius scaling relations between the configurations of purely neutron star and maximally mixed star (MMS) containing equal amounts of ordinary and mirror components. In particular, we show that the MMS masses can be at most $$M^{\mathrm{max}}_{NS}/\sqrt{2}$$ M NS max / 2 , where $$M^\mathrm{max}_{NS}$$ M NS max is a maximum mass of a pure neutron star allowed by a given equation of state. We evaluate $$n-n'$$ n - n ′ transition rate in neutron stars, and show that various astrophysical limits on pulsar properties exclude the transition times in a wide range $$10^{5}\,\text {year}< \tau _\varepsilon < 10^{15}\,\text {year}$$ 10 5 year < τ ε < 10 15 year . For short transition times, $$\tau _\varepsilon < 10^5$$ τ ε < 10 5 year, the different mixed stars of the same mass can have different radii, depending on their age, which possibility can be tested by the NICER measurements. We also discuss subtleties related with the possible existence of mixed quark stars, and possible implications for the gravitational waves from the neutron star mergers and associated electromagnetic signals.
format	article
author	Zurab Berezhiani Riccardo Biondi Massimo Mannarelli Francesco Tonelli
author_facet	Zurab Berezhiani Riccardo Biondi Massimo Mannarelli Francesco Tonelli
author_sort	Zurab Berezhiani
title	Neutron-mirror neutron mixing and neutron stars
title_short	Neutron-mirror neutron mixing and neutron stars
title_full	Neutron-mirror neutron mixing and neutron stars
title_fullStr	Neutron-mirror neutron mixing and neutron stars
title_full_unstemmed	Neutron-mirror neutron mixing and neutron stars
title_sort	neutron-mirror neutron mixing and neutron stars
publisher	SpringerOpen
publishDate	2021
url	https://doaj.org/article/2b8bbe9e261b41fcb36ac06f39a0a888
work_keys_str_mv	AT zurabberezhiani neutronmirrorneutronmixingandneutronstars AT riccardobiondi neutronmirrorneutronmixingandneutronstars AT massimomannarelli neutronmirrorneutronmixingandneutronstars AT francescotonelli neutronmirrorneutronmixingandneutronstars
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Neutron-mirror neutron mixing and neutron stars

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