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• W3216956546 abstract "Abstract The oscillation of neutron n into mirror neutron $$n'$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:msup> <mml:mi>n</mml:mi> <mml:mo>′</mml:mo> </mml:msup> </mml:math> , 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 $$n-n'$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:mrow> <mml:mi>n</mml:mi> <mml:mo>-</mml:mo> <mml:msup> <mml:mi>n</mml:mi> <mml:mo>′</mml:mo> </mml:msup> </mml:mrow> </mml:math> 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 $$M^{mathrm{max}}_{NS}/sqrt{2}$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:mrow> <mml:msubsup> <mml:mi>M</mml:mi> <mml:mrow> <mml:mi>NS</mml:mi> </mml:mrow> <mml:mi>max</mml:mi> </mml:msubsup> <mml:mo>/</mml:mo> <mml:msqrt> <mml:mn>2</mml:mn> </mml:msqrt> </mml:mrow> </mml:math> , where $$M^mathrm{max}_{NS}$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:msubsup> <mml:mi>M</mml:mi> <mml:mrow> <mml:mi>NS</mml:mi> </mml:mrow> <mml:mi>max</mml:mi> </mml:msubsup> </mml:math> is a maximum mass of a pure neutron star allowed by a given equation of state. We evaluate $$n-n'$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:mrow> <mml:mi>n</mml:mi> <mml:mo>-</mml:mo> <mml:msup> <mml:mi>n</mml:mi> <mml:mo>′</mml:mo> </mml:msup> </mml:mrow> </mml:math> transition rate in neutron stars, and show that various astrophysical limits on pulsar properties exclude the transition times in a wide range $$10^{5},text {year}< tau _varepsilon < 10^{15},text {year}$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:mrow> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>5</mml:mn> </mml:msup> <mml:mspace /> <mml:mtext>year</mml:mtext> <mml:mo><</mml:mo> <mml:msub> <mml:mi>τ</mml:mi> <mml:mi>ε</mml:mi> </mml:msub> <mml:mo><</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>15</mml:mn> </mml:msup> <mml:mspace /> <mml:mtext>year</mml:mtext> </mml:mrow> </mml:math> . For short transition times, $$tau _varepsilon < 10^5$$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML> <mml:mrow> <mml:msub> <mml:mi>τ</mml:mi> <mml:mi>ε</mml:mi> </mml:msub> <mml:mo><</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>5</mml:mn> </mml:msup> </mml:mrow> </mml:math> 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." @default.
• W3216956546 created "2021-12-06" @default.
• W3216956546 creator A5031574021 @default.
• W3216956546 creator A5042228727 @default.
• W3216956546 creator A5075929864 @default.
• W3216956546 creator A5081082643 @default.
• W3216956546 date "2021-11-01" @default.
• W3216956546 modified "2023-10-02" @default.
• W3216956546 title "Neutron-mirror neutron mixing and neutron stars" @default.
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