-
In this work, we investigate the properties of strange quark matter (SQM) and color-flavor-locked (CFL) quark matter under zero temperature or strong magnetic fields within MIT bag model. We find that the thermodynamical properties of CFL quark matter are strongly affected by pairing energy gap Δ and magnetic field. The sound velocity of CFL quark matter and the tidal deformability of CFL quark stars both increase with Δ increasing, while the central baryon density of the maximum star mass in CFL state decreases with Δ. Specifically, the equation of state (EOS) of the CFL quark matter becomes stiffer with the increase of Δ, and the pressure becomes anisotropic when considering the magnetic field in the CFL quark matter. Our results indicate that the mass-radius relations of the CFL quark matter within the MIT bag model can describe the recent observations of pulsars, and that the maximum mass of CFL quark star increases with the increase of Δ. Moreover, the research results indicate that the mass of CFL quark star depends on the magnetic field strength and its orientation distributions within the magnetars, and the polytropic index of CFL quark matter decreases with the increase of star mass.
-
Keywords:
- color-flavor-locked phase /
- quark star /
- magnetar
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图 1 零温情况下基于MIT袋模型的奇异夸克物质与色味锁夸克物质的每核子能量与相应的压强随重子数密度的变化
Figure 1. The energy per baryon and corresponding pressure as functions of baryon densityof SQM and CFL quark matter within MIT bag model.
图 2 奇异夸克物质与色味锁夸克物质的声速平方随重子数密度的变化
Figure 2. The sound velocity square of SQM and CFL quark matter as functions of baryon density.
图 3 奇异夸克物质与CFL夸克物质的多方指数随重子数密度的变化
Figure 3. The polytropic index of SQM and CFL quark matter as a function of $ n_{\mathrm{B}} $.
图 4 夸克星最大质量随能隙常数的变化规律
Figure 4. The maximum mass of quark stars as a function of Δ
图 5 色味锁夸克星引力波潮汐形变随能隙常数的变化规律
Figure 5. Tidal deformability of the CFL quark stars as a function of Δ.
图 6 不同袋常数下色味锁夸克星最大质量对应的中心密度随Δ的变化
Figure 6. The central density of the maximum mass of CFL quark stars as a functions of Δ with different bag constant.
图 7 奇异夸克星与色味锁夸克星在不同Δ的质量半径关系
Figure 7. Mass-radius lines of strange quark stars and CFL quark stars with different Δ.
图 8 强磁场下MCFL夸克物质的每核子能量与压强随重子数密度变化关系
Figure 8. The energy per baryon and pressure as functions of $ n_{\mathrm{B}} $ under strong magnetic fields.
图 9 基于MIT袋模型下的MCFL磁星的质量半径关系
Figure 9. Mass-radius relation of MCFL magnetars within MIT bag model.
图 10 横向磁场与径向磁场下, MCFL态夸克物质的多方指数随重子数密度的变化关系
Figure 10. The polytropic index as a function of baryon number density with transverse magnetic field and longitudinal magnetic field.
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[1] Glendenning N K 2000 Compact Stars (2nd Ed.) (New York: Spinger-Verlag, Inc.
[2] Weber F 1999 Pulsars as Astrophyical Laboratories for Nuclear and Particle Physics (London: IOP Publishing Ltd.
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Google Scholar
[4] Steiner A W, Prakash M, Lattimer J M, Ellis P J 2005 Phys. Rep. 410 325
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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Google Scholar
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