强磁场与有限温度下色味锁夸克星的唯象模型

初鹏程; 刘玉珩; 刘鹤; 刘宏铭; 杨永杭

doi:10.7498/aps.74.20250451

摘要

基于准粒子模型对强磁场和有限温度下色味锁夸克物质与色味锁磁星的性质进行了讨论. 发现色味锁夸克物质的每核子自由能、有效质量、每核子熵等物理量受磁场、温度、能隙常数的影响较大, 并且强磁场、有限温度环境中色味锁夸克物质的压强会产生各向异性. 进一步研究了不同等熵阶段下的色味锁磁星的性质, 发现色味锁磁星的质量、半径等性质与磁星内部的磁场强度分布、磁场方向分布紧密相关, 磁星内部温度会随着每核子熵的增加而增大. 结论还表明色味锁夸克物质的多方指数会随着色味锁夸克星质量的增大而减少.

关键词:

色味锁态 /
夸克星 /
磁星

Abstract

The properties of the color-flavor-locked (CFL) quark matter under strong magnetic fields at finite temperatures within a quasiparticle model are investigated in this work. Our results indicate that CFL quark matter pressure becomes anisotropic under strong magnetic fields, while its equation of state (EOS) and equivalent quark mass are both strongly affected by temperature, energy gap constant Δ, and strong magnetic field inside the CFL quark matter. The equivalent quark mass of CFL quark matter decreases with temperature and magnetic field strength increasing, which implies an inverse magnetic catalysis phenomenon. The results also indicate that the entropy per baryon of the CFL quark matter increases with temperature rising and decreases with Δ increasing. Furthermore, the properties of CFL magnetars in different isentropic stages are studied. The star mass and radius depend primarily on the strength and orientation of magnetic fieldinside the CFL magnestars. The maximum star mass increases with entropy per baryon increasing, while the star matter temperature rises at high isentropic stage. Moreover, the polytropic index of the CFL quark matter decreases with star mass increasing.

Keywords:

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 ; 刘宏铭, liuhongming13@126.com ;

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 Pengcheng, kyois@126.com ; LIU He, liuhe@qut.edu.cn ; LIU Hongming, liuhongming13@126.com ;

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

参考文献

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施引文献

图 1 不同温度与能隙常数下色味锁态物质的每核子自由能与横纵向压强随着$ n_{\mathrm{B}} $的变化关系

Fig. 1. The free energy per baryon and pressures of CFL quark matter with $ n_{\mathrm{B}} $ at finite temperature and with different $ \varDelta $.

下载: 全尺寸图片幻灯片

图 2 不同温度与能隙常数下u夸克的有效质量随磁感应强度的变化

Fig. 2. The equivalent mass of u quarks as a function of the magnetic field with different temperature and $ \varDelta $.

下载: 全尺寸图片幻灯片

图 3 色味锁态下夸克星物质的每核子熵随着不同温度、磁场、能隙常数的变化

Fig. 3. The entropy per baryon of the quark star matter in MCFL state with various temperature, magnetic field and $ \varDelta $

下载: 全尺寸图片幻灯片

图 4 MCFL下夸克物质的多方指数随磁场、温度、能隙常数的变化规律

Fig. 4. The polytropic index of the MCFL quark star matter as a function of the magnetic field strength, temperature, and $ \varDelta $.

下载: 全尺寸图片幻灯片

图 5 不同等熵阶段中的色味锁磁星的质量-半径情况

Fig. 5. The star mass as functions of the radius of the MCFL quark stars along different isentropic stages.

下载: 全尺寸图片幻灯片

图 6 不同等熵阶段下色味锁夸克星内部温度随$ n_{\mathrm{B}} $与磁场的变化

Fig. 6. The temperature of the MCFL quark star matter as functions of $ n_{\mathrm{B }}$ and magnetic field along different isentropic stages.

下载: 全尺寸图片幻灯片

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
[3]	Lattimer J M, Prakash M 2004 Science 304 536 Google Scholar
[4]	Steiner A W, Prakash M, Lattimer J M, Ellis P J 2005 Phys. Rep. 410 325
[5]	Demorest P 2010 Nature 467 1081 Google Scholar
[6]	Antoniadis J 2013 Science 340 6131
[7]	Shahbaz T, Casares J 2018 Astrophys. J. 859 54 Google Scholar
[8]	Thankful H, Cromartie 2020 Nature Astron. Lett. 4 72
[9]	Fonseca E, Cromartie H T, Pennucci T T, et al. 2021 Astrophys. J. Lett. 915 L12 Google Scholar
[10]	Miller M C, Lamb F K, Dittmann A J, et al. 2021 Astrophys. J. Lett. 918 L28 Google Scholar
[11]	Abbott R 2020 Astrophys. J. Lett. 896 L44 Google Scholar
[12]	Ivanenko D, Kurdgelaidze D F 1969 Lett. Nuovo Cimento 2 13 Google Scholar
[13]	Itoh N 1970 Prog. Theor. Phys. 44 291 Google Scholar
[14]	Bodmer A R 1971 Phys. Rev. D 4 1601 Google Scholar
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[16]	Farhi E, Jaffe R L 1984 Phys. Rev. D 30 2379 Google Scholar
[17]	Alcock C, Farh E, Olinto A 1986 Astrophys. J. 310 261 Google Scholar
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[43]	Deng Z L, Gao Z F, Li X D, Shao Y 2020 Astrophys. J. 892 4 Google Scholar
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[45]	Wang H, Gao Z F, Jia H Y, Wang N, Li X 2020 Universe 6 63 Google Scholar
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[47]	Deng Z L, Li X D, Gao Z F, Shao Y 2021 Astrophys. J. 909 174 Google Scholar
[48]	G ao, Z F, Omar N, Shi X C, Wang N 2019 Astron. Nachr. 340 1030 Google Scholar
[49]	Lander S K 2023 Astrophys.J. 947 L16 Google Scholar
[50]	Woltjer L 1964 Astrophys. J. 140 1309 Google Scholar
[51]	Mihara T A 1990 Nature 346 250 Google Scholar
[52]	Chanmugam G 1992 Annu. Rev. Astron. Astrophys. 30 143 Google Scholar
[53]	Lai D, Shapiro S L 1991 Astrophys. J. 383 745 Google Scholar
[54]	Ferrer E J, Incera V, Keith J P, Portillo I, Springsteen P L 2010 Phys. Rev. C 82 065802
[55]	Bandyopadhyay D, Chakrabarty S, Pal S 1997 Phys Rev. Lett. 79 2176 Google Scholar
[56]	Bandyopadhyay D, Pal S, Chakrabarty S 1998 J. Phys. G: Nucl. Part. Phys. 24 1647 Google Scholar
[57]	Menezes D P, Pinto M, Benghi, Avancini S, Providência C 2009 Phys. Rev. C 79 035807 Google Scholar
[58]	Menezes D P, Pinto M, Benghi, Avancini S, Providência C 2009 Phys. Rev. C 80 065805 Google Scholar
[59]	Ryu C Y, Kim K S, Cheoun Myung-Ki 2010 Phys. Rev. C 82 025804 Google Scholar
[60]	Ryu C Y, Cheoun Myung-Ki, Kajino T, Maruyama T, Mathews Grant J 2012 Astropart. Phys. 38 25 Google Scholar
[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
[63]	Aidala C, Akiba Y, Alfred M, et al. 2018 Phys. Rev. L 120 022001 Google Scholar
[64]	Zhang C, Mann R B 2021 Phys. Rev. D 103 063018 Google Scholar
[65]	Yuan L W, Li A, Miao Z Q, Zuo B J, Bai Z 1984 Phys. Rev. D 105 123004
[66]	Schertler K, Greiner C, Thoma M H, Schertler K, Greiner C, Thoma M H 1997 Nucl. Phys. A 616 659 Google Scholar
[67]	Pisarski R D 1989 Nucl. Phys. A498 423
[68]	Wen X J 2009 J. Phys. G: Nucl. Part. Phys. 36 025011 Google Scholar
[69]	Zhang Z, Chu P C, Li X H, Liu H, Zhang X M 2021 Phys. Rev. D 103 103021 Google Scholar
[70]	Chu P C, Chen L W 2014 Astrophys. J. 780 135
[71]	Chu P C 2018 Phys. Lett. B 778 447 Google Scholar
[72]	Chu P C, Chen L W 2017 Phys. Rev. D 96 103001 Google Scholar
[73]	Chodos A, Jaffe R L, Ohnson K, Thorn C B, Weisskopf V F 1974 Phys. Rev. D 9 3471 Google Scholar
[74]	Alford M, Braby M, Paris M, Reddy S 2005 Astrophys. J. 629 969 Google Scholar
[75]	Rehberg P, Klevansky S P, Hüfner J 1996 Phys. Rev. C 53 410
[76]	Hanauske M, Satarov L M, Mishustin I N, Stocker H, Greiner W 2001 Phys. Rev. D 64 043005 Google Scholar
[77]	Rüster S B, Rischke D H 2004 Phys. Rev. D 69 045011 Google Scholar
[78]	Menezes D P, Providencia C, Melrose D B 2006 J. Phys. G 32 1081 Google Scholar
[79]	Chao J Y, Chu P C, Huang M 2013 Phys. Rev. D 88 054009 Google Scholar
[80]	Chu P C, Wang X, Chen L W, Huang M 2015 Phys. Rev. D 91 023003 Google Scholar
[81]	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
[82]	Chu P C, Chen L W 2017 Phys. Rev. D 96 083019 Google Scholar
[83]	Roberts C D, Williams A G 1994 Prog. Part. Nucl. Phys. 33 477 Google Scholar
[84]	Zong H S, Chang L, Hou F Y, Sun W M, Liu Y X 2005 Phys. Rev. C 71 015205 Google Scholar
[85]	Peng G X, Chiang H C, Yang J J, Li L, Liu B 1999 Phys. Rev. C 61 015201 Google Scholar
[86]	Peng G X, Chiang H C, Zou B S, Ning P Z, Luo S J 2000 Phys. Rev. C 62 025801
[87]	Peng G X, Li A, Lombardo U 2008 Phys. Rev. C 77 065807 Google Scholar
[88]	Li A, Peng G X, Lu J F 2011 Res. Astron. Astrophys. 11 482 Google Scholar
[89]	Schertler K, Greiner C, Sahu P K, Thoma M H 1998 Nucl. Phys. A 637 451 Google Scholar
[90]	Alford M, Kouvaris C, Rajagopal K 2005 Phys. Rev. D 71 054009 Google Scholar
[91]	Giannakis I, Hou D F, Ren H C, Rischke D H 2004 Phys. Rev. L 93 232301 Google Scholar
[92]	董爱军, 高志福, 杨晓峰等 2023 72 030502 Google Scholar Dong A J, Gao Z F, Yang X F, et al. 2023 Acta Phys. Sin. 72 030502 Google Scholar
[93]	Ferrer E J, Vivian de la Incera 2005 Phys. Rev. Lett. 95 152002 Google Scholar
[94]	Ferrer E J, Vivian de la Incera, Cristina M 2006 Nucl.Phys. B 747 88 Google Scholar
[95]	Feng B, Ferrer E J, Vivian de la Incera 2011 Nucl.Phys. B 853 213 Google Scholar
[96]	Paulucci L, Ferrer E J, Vivian de la Incera, Horvath J E 2011 Phys. Rev. D 83 043009 Google Scholar
[97]	Isayev A A, Yang J 2011 Phys. Rev. C 84 065802
[98]	Isayev A A, Yang J 2012 Phys. Lett. B 707 163 Google Scholar
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