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色味锁夸克物质与夸克星

初鹏程 刘鹤 杜先斌

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色味锁夸克物质与夸克星

初鹏程, 刘鹤, 杜先斌

Quark matter and quark star in color-flavor-locked phase

Chu Peng-Cheng, Liu He, Du Xian-Bin
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  • 讨论了零温、强磁场下基于准粒子模型的奇异夸克物质、色味锁夸克物质的热力学性质. 结果表明色味锁夸克物质比奇异夸克物质更稳定, 压强会随着色味锁态能隙常数的增大而增加. 并且发现强磁场下磁星的最大质量会随着色味锁夸克物质的能隙常数的增加而增加, 磁星的潮汐形变率会随着能隙常数的增加而增加, 磁星最大质量的中心密度会随着能隙常数的增加而降低. 结果还说明考虑色味锁态得到的磁星质量半径关系可以满足最近实验观测 PSR J0740 + 6620, PSR J0030 + 0451, 和 HESS J1731-347所给出的质量半径约束.
    In this work, we investigate the thermodynamical properties of strange quark matter (SQM) and color-flavor-locked (CFL) quark matter under strong magnetic fields by using a quasiparticle model. We calculate the energy density and the corresponding anisotropic pressure of both SQM and CFL quark matter. Our results indicate that CFL quark matter exhibits greater stability than the SQM, and the pressure of CFL quark matter increases with the energy gap constant $\varDelta $ increasing. We also observe that the oscillation effects coming from the lowest Landau level can be reduced by increasing the energy gap constant $ \varDelta $, which cannot be observed in SQM under a similar strong magnetic field. The equivalent quark mass for u, d, and s quark and the chemical potential for each flavor of quarks decrease with the energy gap constant $ \varDelta $ increasing, which matches the conclusion that CFL quark matter is more stable than SQM. From the calculations of the magnetars with SQM and CFL quark matter, we find that the maximum mass of magnetars increases with the energy gap constant $\varDelta $ increasing for both the longitudinal and the transverse orientation distribution of magnetic field. Additionally, the tidal deformability of the magnetars increases with the $\varDelta $ increasing. On the other hand, the central baryon density of the maximum mass of the magnetars decreases with the $\varDelta $ increasing. The results also indicate that the mass-radius lines of the CFL quark star can also satisfy the new estimates of the mass-radius region from PSR J0740 + 6620, PSR J0030 + 0451, and HESS J1731-347.
      通信作者: 初鹏程, kyois@126.com ; 刘鹤, liuhe@qut.edu.cn
    • 基金项目: 国家自然科学基金(批准号: 11975132, 12205158, 11505100)和山东省自然科学基金(批准号: ZR2022JQ04, ZR2021QA037, ZR2019YQ01)资助的课题.
      Corresponding author: Chu Peng-Cheng, kyois@126.com ; Liu He, liuhe@qut.edu.cn
    • Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 11975132, 12205158, 11505100) and the Natural Science Foundation of Shandong Province, China(Grant Nos. ZR2022JQ04, ZR2021QA037, ZR2019YQ01).
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  • 图 1  $ \varDelta = 50 $ MeV时色味锁夸克物质的能量密度随重子数密度与磁场的变化

    Fig. 1.  Energy density of CFL quark matter as functions of baryon density and magnetic field with $ \varDelta = 50 $ MeV.

    图 2  $ \varDelta = 100 $ MeV时色味锁夸克物质的能量密度随重子数密度与磁场的变化

    Fig. 2.  Energy density of CFL quark matter as functions of baryon density and magnetic field with $ \varDelta = 100 $ MeV.

    图 3  $ \varDelta = 50 $ MeV时色味锁夸克物质的压强随重子数密度与磁场的变化

    Fig. 3.  Pressure of CFL quark matter as functions of baryon density and magnetic field with $ \varDelta = 50 $ MeV.

    图 4  $ \varDelta = 100 $ MeV时色味锁夸克物质的压强随重子数密度与磁场的变化

    Fig. 4.  Pressure of CFL quark matter as functions of baryon density and magnetic field with $ \varDelta = 100 $ MeV.

    图 5  $ \varDelta = 50 $ MeV和$ \varDelta = 100 $ MeV时色味锁夸克物质的压强不对称度随磁场的变化

    Fig. 5.  Pressure anisotropy of CFL quark matter as functions of magnetic field with $ \varDelta = 50, 100 $ MeV.

    图 6  $ \varDelta = 50 $ MeV和$ \varDelta = 100 $ MeV时u, d, s三味夸克的有效质量随磁场的变化规律

    Fig. 6.  Equivalent quark mass for u, d, and s quarks as functions of magnetic fields B with $ \varDelta = 50 $ MeV and $ \varDelta = 100 $ MeV.

    图 7  $ \varDelta = 50 $ MeV和$ \varDelta = 100 $ MeV时u, d, s三味夸克的化学势随磁场的变化规律

    Fig. 7.  Chemical potential of u, d, and s quarks as functions of magnetic fields B with $ \varDelta = 50 $ MeV and $ \varDelta = 100 $ MeV

    图 8  磁场与零磁场下色味锁相夸克星质量半径关系

    Fig. 8.  Mass-radius relation of QSs with CFL quark phase under magnetic fields.

    图 9  奇异夸克星与色味锁相磁星最大质量随磁场的变化关系

    Fig. 9.  Maximum star mass of magnetars as a function of magnetic field $ B_0 $ with SQM and CFL quark phase by considering transverse magnetic field orientation and longitudinal orientation.

    表 1  不同磁场方向分布情况下($ B_0 = 4\times \text{10}^{18} $G)磁星最大质量中心密度、1.4倍太阳质量潮汐形变率随Δ的变化

    Table 1.  The central density and tidal deformability of the magnetars considering “radial orientation” and “transverse orientation” at $ B_0 = 4\times \text{10}^{18} $G with g-2 within quasiparticle model with different Δ.

    $ B_{{/ /}} $ $ B_{{/ /}} $ $ B_{\perp} $ $ B_{\perp} $
    Δ/MeV 50 100 50 100
    $ n_{\mathrm{c}} $/$ \text{fm}^{-3} $ 0.95 0.82 0.91 0.8
    $ \varLambda_{1.4} $/MeV 741 1256 805 1351
    下载: 导出CSV
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    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.

    [3]

    Lattimer J M, Prakash M 2004 Science 304 536Google Scholar

    [4]

    Steiner A W, Prakash M, Lattimer J M, Ellis P J 2005 Phys. Rep. 410 325Google Scholar

    [5]

    Demorest P 2010 Nature 467 1081Google Scholar

    [6]

    Antoniadis J 2013 Science 340 6131Google Scholar

    [7]

    Shahbaz T, Casares J 2018 Astrophys. J. 859 54Google Scholar

    [8]

    Cromartie H T, Fonseca E, Ransom S M et al. 2020 Nat. Astron. Lett. 4 72

    [9]

    Fonseca E, Cromartie H T, Pennucci T T, et al. 2021 Astrophys. J. Lett. 915 L12Google Scholar

    [10]

    Miller M C, Lamb F K, Dittmann A J, et al. 2021 Astrophys. J. Lett. 918 L28Google Scholar

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    Ivanenko D, Kurdgelaidze D F 1969 Lett. Nuovo Cimento 2 13Google Scholar

    [13]

    Itoh N 1970 Prog. Theor. Phys. 44 291Google Scholar

    [14]

    Bodmer A R 1971 Phys. Rev. D 4 1601Google Scholar

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    Witten E 1984 Phys. Rev. D 30 272Google Scholar

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    Stephanov M A, Rajagopal K, Shuryak E V 1998 Phys. Rev. Lett. 81 4816Google Scholar

    [23]

    Terazawa H 1979 INS-Report (Tokyo: Univ. of Tokyo) p336

    [24]

    Alford M, Reddy S 2003 Phys. Rev. D 67 074024Google Scholar

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    Alford M, Jotwani P, Kouvaris C, Kundu J, Rajagopal K 2005 Phys. Rev. D 71 114011Google Scholar

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    Alford M G, Rajagopal K, Reddy S, Wilczek F 2001 Phys. Rev. D 64 074017Google Scholar

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    Shovkovy I A 2005 Found. Phys. 35 1309Google Scholar

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    Rajagopal K, Wilczek F 2001 Phys. Rev. L 86 3492Google Scholar

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    Alford M G, Rajagopal K, Schaefer T, Schmitt A 2008 Rev. Mod. Phys. 80 1455Google Scholar

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    Mihara T A 1990 Nature 346 250Google Scholar

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    Chanmugam G 1992 Annu. Rev. Astron. Astrophys. 30 143Google Scholar

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    Ferrer E J, Incera V, Keith J P, Portillo I, Springsteen P L 2010 Phys. Rev. C 82 065802Google Scholar

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    Yan F Z, Gao Z F, Yang W S, Dong A J 2021 Astron. Nachr. 342 249Google Scholar

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    Wang H, Gao Z F, Jia H Y, Wang N, Li X 2020 Universe 6 63Google Scholar

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    Li B P, Gao Z F 2023 Astron. Nachr. 344 e20220111

    [58]

    Deng Z L, Li X D, Gao Z F, Shao Y 2021 Astrophys. J. 909 174Google Scholar

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    G ao, Z F, Omar N, Shi X C, Wang N 2019 Astron. Nachr. 340 1030Google Scholar

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    Dong J M 2021 Mon. Not. R. Astron. Soc. 500 1505

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    Schertler K, Greiner C, Thoma M H, Schertler K, Greiner C, Thoma M H 1997 Nucl. Phys. A 616 659Google Scholar

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  • 文章访问数:  1089
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  • 被引次数: 0
出版历程
  • 收稿日期:  2023-10-15
  • 修回日期:  2023-11-21
  • 上网日期:  2023-12-08
  • 刊出日期:  2024-03-05

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