Sound velocity in dense stellar matter with strangeness and compact stars
The phase state of dense matter in the intermediate density range ( 1-10 times the nuclear saturation density) is both intriguing and unclear and can have important observable effects in the present gravitational wave era of neutron stars. As matter density increases in compact stars, the sound velo...
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Published in | Chinese physics C Vol. 45; no. 5; p. 55104 |
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Main Authors | , , , |
Format | Journal Article |
Language | English |
Published |
01.05.2021
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Abstract | The phase state of dense matter in the intermediate density range (
1-10 times the nuclear saturation density) is both intriguing and unclear and can have important observable effects in the present gravitational wave era of neutron stars. As matter density increases in compact stars, the sound velocity is expected to approach the conformal limit (
) at high densities and should also fulfill the causality limit (
). However, its detailed behavior remains a prominent topic of debate. It was suggested that the sound velocity of dense matter could be an important indicator of a deconfinement phase transition, where a particular shape might be expected for its density dependence. In this work, we explore the general properties of the sound velocity and the adiabatic index of dense matter in hybrid stars as well as in neutron stars and quark stars. Various conditions are employed for the hadron-quark phase transition with varying interface tension. We find that the expected behavior of the sound velocity can also be achieved by the nonperturbative properties of the quark phase, in addition to a deconfinement phase transition. Moreover, it leads to a more compact star with a similar mass. We then propose a new class of quark star equation of states, which can be tested by future high-precision radius measurements of pulsar-like objects. |
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AbstractList | The phase state of dense matter in the intermediate density range (
1-10 times the nuclear saturation density) is both intriguing and unclear and can have important observable effects in the present gravitational wave era of neutron stars. As matter density increases in compact stars, the sound velocity is expected to approach the conformal limit (
) at high densities and should also fulfill the causality limit (
). However, its detailed behavior remains a prominent topic of debate. It was suggested that the sound velocity of dense matter could be an important indicator of a deconfinement phase transition, where a particular shape might be expected for its density dependence. In this work, we explore the general properties of the sound velocity and the adiabatic index of dense matter in hybrid stars as well as in neutron stars and quark stars. Various conditions are employed for the hadron-quark phase transition with varying interface tension. We find that the expected behavior of the sound velocity can also be achieved by the nonperturbative properties of the quark phase, in addition to a deconfinement phase transition. Moreover, it leads to a more compact star with a similar mass. We then propose a new class of quark star equation of states, which can be tested by future high-precision radius measurements of pulsar-like objects. |
Author | Li, Ang Xia, Chengjun Zhu, Zhenyu Zhou, Xia |
Author_xml | – sequence: 1 givenname: Chengjun surname: Xia fullname: Xia, Chengjun – sequence: 2 givenname: Zhenyu surname: Zhu fullname: Zhu, Zhenyu – sequence: 3 givenname: Xia surname: Zhou fullname: Zhou, Xia – sequence: 4 givenname: Ang surname: Li fullname: Li, Ang |
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CitedBy_id | crossref_primary_10_1103_PhysRevD_105_023018 crossref_primary_10_1051_epjconf_202226004001 crossref_primary_10_1103_PhysRevD_107_043005 crossref_primary_10_3847_1538_4365_ad0ece crossref_primary_10_1142_S0218301322500379 crossref_primary_10_1093_mnras_stac2015 crossref_primary_10_1088_1361_6471_ac1713 crossref_primary_10_1103_PhysRevD_107_063019 crossref_primary_10_1103_PhysRevC_104_055803 crossref_primary_10_1103_PhysRevD_104_034011 crossref_primary_10_3390_foundations1020017 crossref_primary_10_1103_PhysRevLett_128_161101 crossref_primary_10_1103_PhysRevD_108_063032 crossref_primary_10_1103_PhysRevC_103_045804 crossref_primary_10_1103_PhysRevD_105_123004 crossref_primary_10_1103_PhysRevD_109_123005 crossref_primary_10_3847_2041_8213_ac194d crossref_primary_10_1088_1361_6471_ac4ea1 crossref_primary_10_1088_1674_1137_ac5513 crossref_primary_10_1103_PhysRevD_106_014014 crossref_primary_10_1016_j_physletb_2022_137121 crossref_primary_10_1016_j_nuclphysa_2023_122608 crossref_primary_10_1002_andp_202200297 crossref_primary_10_1088_1361_6382_ac7f78 crossref_primary_10_1103_PhysRevD_109_043054 crossref_primary_10_1088_1361_6471_ac6f14 crossref_primary_10_1103_PhysRevC_109_065803 crossref_primary_10_3847_2041_8213_ac5ea6 |
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