Lifting the Veil on Quark Matter in Compact Stars with Core g-mode Oscillations

Compact stars containing quark matter may masquerade as neutron stars in the range of measured mass and radius, making it difficult to draw firm conclusions on the phase of matter inside the star. The sensitivity of core g -mode oscillations to the presence of a mixed phase may alleviate this diffic...

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Bibliographic Details
Published inThe Astrophysical journal Vol. 904; no. 2; pp. 187 - 196
Main Authors Wei, Wei, Salinas, Marc, Klähn, Thomas, Jaikumar, Prashanth, Barry, Megan
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.12.2020
IOP Publishing
Subjects
Astrophysics
Binary stars
Coalescing
Damping
Gravitational waves
Matter & antimatter
Neutron stars
Oscillations
Quarks
Sensitivity analysis
Stellar oscillations
Viscosity
Waveforms
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ISSN0004-637X
1538-4357
DOI10.3847/1538-4357/abbe02

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Summary:Compact stars containing quark matter may masquerade as neutron stars in the range of measured mass and radius, making it difficult to draw firm conclusions on the phase of matter inside the star. The sensitivity of core g -mode oscillations to the presence of a mixed phase may alleviate this difficulty. In hybrid stars that admit quark matter in a mixed phase, the g -mode frequency rises sharply due to a marked decrease in the equilibrium sound speed. Resonant excitation of g -modes can leave an imprint in the waveform of coalescing binary compact stars. We present analytic and numeric results to assess the sensitivity displayed by g -mode oscillations to quark matter in a homogeneous or mixed phase and also compute relevant damping times in quark matter due to viscosity.
Bibliography:AAS25974
High-Energy Phenomena and Fundamental Physics
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ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abbe02