色味锁夸克物质与夸克星

初鹏程; 刘鹤; 杜先斌

doi:10.7498/aps.73.20231649

摘要

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.

关键词:

夸克物质 /
夸克星 /
磁星

Abstract

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.

Keywords:

quark matter /
quark star /
magnetar

作者及机构信息

青岛理工大学理学院, 青岛　266033

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.

Authors and contacts

School of Science, Qingdao University of Technology, Qingdao 266033, China

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).

文章全文 : translate this paragraph

参考文献

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施引文献

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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.

下载: 全尺寸图片幻灯片

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

map

[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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[30]	Bonanno L, Sedrakian A 2012 A&A 539 A16 Google Scholar
[31]	Chu P C, Wang B, Jia Y Y, Dong Y M, Wang S M, Li X H, Zhang L, Zhang X M, Ma H Y 2016 Phys. Rev. D 94 123014 Google Scholar
[32]	Chu P C, Li X H, Wang B, Dong Y M, Jia Y Y, Wang S M, Ma H Y 2017 Eur. Phys. J. C 77 512 Google Scholar
[33]	Chu P C, Zhou Y, Chen C, Li X H, Ma H Y 2020 J. Phys. G: Nucl. Part. Phys. 47 085201 Google Scholar
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[37]	Rajagopal K, Wilczek F 2001 Phys. Rev. L 86 3492 Google Scholar
[38]	Alford M G, Rajagopal K, Schaefer T, Schmitt A 2008 Rev. Mod. Phys. 80 1455 Google Scholar
[39]	Lugones G, Horvath J E 2003 Astron. Astrophys. 403 173 Google Scholar
[40]	Horvath J E, Lugones G 2004 Astron. Astrophys. 422 L1 Google Scholar
[41]	Woltjer L 1964 Astrophys. J. 140 1309 Google Scholar
[42]	Mihara T A 1990 Nature 346 250 Google Scholar
[43]	Chanmugam G 1992 Annu. Rev. Astron. Astrophys. 30 143 Google Scholar
[44]	Lai D, Shapiro S L 1991 Astrophys. J. 383 745 Google Scholar
[45]	Ferrer E J, Incera V, Keith J P, Portillo I, Springsteen P L 2010 Phys. Rev. C 82 065802 Google Scholar
[46]	Bandyopadhyay D, Chakrabarty S, Pal S 1997 Phys Rev. Lett. 79 2176 Google Scholar
[47]	Bandyopadhyay D, Pal S, Chakrabarty S 1998 J. Phys. G: Nucl. Part. Phys. 24 1647 Google Scholar
[48]	Menezes D P, Pinto M, Benghi, Avancini S, Providência C 2009 Phys. Rev. C 79 035807 Google Scholar
[49]	Menezes D P, Pinto M, Benghi, Avancini S, Providência C 2009 Phys. Rev. C 80 065805 Google Scholar
[50]	Ryu C Y, Kim K S, Cheoun Myung-Ki 2010 Phys. Rev. C 82 025804 Google Scholar
[51]	Ryu C Y, Cheoun Myung-Ki, Kajino T, Maruyama T, Mathews Grant J 2012 Astropart. Phys. 38 25 Google Scholar
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[53]	Gao Z F, Wang N, Shan H, L i, X D, Wang W 2017 Astrophys. J. 849 19 Google Scholar
[54]	Deng Z L, Gao Z F, Li X D, Shao Y 2020 Astrophys. J. 892 4 Google Scholar
[55]	Yan F Z, Gao Z F, Yang W S, Dong A J 2021 Astron. Nachr. 342 249 Google Scholar
[56]	Wang H, Gao Z F, Jia H Y, Wang N, Li X 2020 Universe 6 63 Google Scholar
[57]	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. 909 174 Google Scholar
[59]	G ao, Z F, Omar N, Shi X C, Wang N 2019 Astron. Nachr. 340 1030 Google Scholar
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[61]	Dong J M 2021 Mon. Not. R. Astron. Soc. 500 1505
[62]	Fu G Z, Xing C C, Wang N 2020 Eur. Phys. J. C 80 582 Google Scholar
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[64]	Pisarski R D 1989 Nucl. Phys. A 498 423
[65]	Wen X J 2009 J. Phys. G: Nucl. Part. Phys. 36 025011 Google Scholar
[66]	Zhang Z, Chu P C, Li X H, Liu H, Zhang X M 2021 Phys. Rev. D 103 103021 Google Scholar
[67]	Chu P C, Chen L W 2014 Astrophys. J. 780 135 Google Scholar
[68]	Chu P C 2018 Phys. Lett. B 778 447 Google Scholar
[69]	Chu P C, Chen L W 2017 Phys. Rev. D 96 103001 Google Scholar
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[75]	Menezes D P, Providencia C, Melrose D B 2006 J. Phys. G 32 1081 Google Scholar
[76]	Chao J Y, Chu P C, Huang M 2013 Phys. Rev. D 88 054009 Google Scholar
[77]	Chu P C, Wang X, Chen L W, Huang M 2015 Phys. Rev. D 91 023003 Google Scholar
[78]	Chu P C, Wang B, Ma H Y, Dong Y M, Chang S L, Zheng C H, Liu J T, Zhang X M 2016 Phys. Rev. D 93 094032 Google Scholar
[79]	Chu P C, Chen L W 2017 Phys. Rev. D 96 083019 Google Scholar
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