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奇异夸克物质（Strang Quark Matter,SQM）被认为是强相互作用的真正基态，然而近期有研究表明普通夸克物质（u-d Quark Matter,u-d QM）也有可能是强相互作用的基态.通过在夸克质量标度中采用伍德-萨克松（Woods-Saxon）型的衰减因子，基于等效质量模型对u-d QM状态方程的计算结果表明，衰减因子的引入增大了u-d QM稳定存在的参数窗口，使得普通夸克星（u-dQuark Star,u-d QS）的质量在满足2倍太阳质量的前提下，同时满足潮汐形变Λ1.4 ∈[70,580],这一计算结果符合目前的相关天文观测数据，因此脉冲星本质上有可能是u-d QM构成的u-d QS.这一结果为理解脉冲星的本质提供了一种可能，也进一步加深了对强相互作用的理解.Strang Quark Matter (SQM) is considered to be the true ground state of the strong interactions, but recent studies have shown that ordinary quark matter (u-d Quark Matter, u-d QM) may also be the ground state of the strong interactions.
By inserting an attenuation factor of Woods-Saxon type in the quark mass scaling, the resulting calculations of equation of state of u-d QM based on equiv-particle model show that the stability window of model parameters for stable u-d QM can be significantly enlarged with proper model parameters, which can be seen in the following figure. In this figure, the red solid and dashed lines represent the curves of √D versus C with and without attenuation factor, respectively, when the minimum value of the average energy per baryon is set to 930 MeV; the blue solid and dashed lines represent the curves of √D versus C with and without attenuation factor, respectively, when mu = 0. Thereby, the red and blue shaded areas are the absolute stable regions for u-d QM without and with attenuation factor in mass scaling. It is obvious that with the inclusion of attenuation factor and proper model parameters the absolute stable region (blue shaded area) for u-d QM can be much larger than that without the attenuation factor (red shaded area).
The introduction of the attenuation factor makes it possible that the maximum mass of ordinary quark star (u-d quark star, u-d QS) can be larger than 2 times the solar mass, and meanwhile the tidal deformability satisfies Λ1.4 ∈ [70, 580], which are both consistent with the current astronomical observations. Therefore, the pulsars may be essentially the u-d QSs. This result offers a possibility for understanding the nature of pulsars, and it also further deepens the understanding of the strong interactions.-
Keywords:
- Quark matter /
- Quark star /
- Equation of state /
- Tidal deformability
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[1] Peng G X, Li A, Lombardo U 2008 Phys. Rev. C 77065807
[2] Weissenborn S, Sagert I, Pagliara G, Hempel M, Schaffner-Bielich J 2011 Astrophys. J. 740 L14
[3] Clemente F D, Casolino M, Drago A, Lattanzi M, Ratti C 2025 Mon. Not. R. Astron. Soc. 5371056
[4] Li C M, Zheng H R, Zuo S Y, Zhao Y P, Wang F, Huang Y F 2025 Astrophys. J. 980231
[5] Song X Y 2025 Phys. Rev. D 111063018
[6] Zhang C 2020 Phys. Rev. D 101043003
[7] Xu J F, Peng G X, Liu F, Hou D F, Chen L W 2015 Phys. Rev. D 92025025
[8] Xu R X 2003 Astrophys. J. 596 L59
[9] Peng G X, Chiang H C, Zou B S, Ning P Z, Luo S J 2000 Phys. Rev. C 62025801
[10] Klähn T, Fischer T 2015 Astrophys. J. 810134
[11] Xia T, He L Y, Zhuang P F 2013 Phys. Rev. D 88056013
[12] Wen X J, Feng Z Q, Li N, Peng G X 2009 J. Phys. G 36025011
[13] Li B L, Cui Z F, Yu Z H, Yan Y, An S, Zong H S 2019 Phys. Rev. D 99043001
[14] Zhang C, Gao Y, Xia C J, Xu R X 2023 Phys. Rev. D 108063002
[15] Xia C J, Peng G X, Chen S W, Lu Z Y, Xu J F 2014 Phys. Rev. D 89105027
[16] Chen S W, Gao L, Peng G X 2012 Chin. Phys. C 36947
[17] Xu J F, Cui L, Lu Z Y, Xia C J, Peng G X 2023 Nucl. Sci. Tech. 34171
[18] Demorest P, Pennucci T, Ransom S M, Roberts M S E, Hessels J W T 2010 Nature 4671081
[19] Antoniadis J, Freire P C C, Wex N, Tauris T M, Lynch R S, Kerkwijk M H V, Kramer M, Bassa C, Dhillon V S, Driebe T, Hessels J W T, Kaspi V M, Kondratiev V I, Langer N, Marsh T R, Mclaughlin M A, Pennucci T T, Ransom S M, Stairs I H, Leeuwen J V, Verbiest P W, Whelan D G 2013 Science 3401233232
[20] Cromartie H T, Fonseca E, Ransom S M, Demorest P B, Arzoumanian Z, Blumer H, Brook P R, DeCesar M E, Dolch T, Ellis J A, Ferdman R D, Ferrara E C, Garver-Daniels N, Gentile P A, Jones M L, Lam M T, Lorimer D R, Lynch R S, McLaughlin M A, Ng C, Nice D J, Pennucci T T, Spiewak R, Stairs I H, Stovall K, Swiggum J K, Zhu W W 2020 Nat. Astron. 472
[21] Fonseca E, Cromartie H T, Pennucci T T, Ray P S, Kirichenko A Y, Ransom S M, Demorest P B, Stairs I H, Arzoumanian Z, Guillemot L, Parthasarathy A, Kerr M, Cognard I, Baker P T, Blumer H, Brook P R, DeCesar M, Dolch T, Dong F A, Ferrara E C, Fiore W, Garver-Daniels N, Good D C, Jennings R, Jones M L, Kaspi V M, Lam M T, Lorimer D R, Luo J, McEwen A, McKee J W, McLaughlin M A, McMann N, Meyers B W, Naidu A, Ng C, Nice D J, Pol N, Radovan H A, ShapiroAlbert B, Tan C M, Tendulkar S P, Swiggum J K, Wahl H M, Zhu W W 2021 Astrophys. J. Lett. 915 L12
[22] LIGO Scientific and Virgo Collaboration, Abbott R, et al 2020 Astrophys. J. Lett. 896 L44
[23] LIGO Scientific and Virgo Collaboration, Abbott B P, et al 2016 Phys. Rev. Lett. 116061102
[24] LIGO Scientific and Virgo Collaboration, Abbott B P, et al 2017 Astrophys. J. 848 L12
[25] LIGO Scientific and Virgo Collaboration, Abbott B P, et al 2018 Phys. Rev. Lett. 121161101
[26] Witten E 1984 Phys. Rev. D 30272
[27] Farhi E, Jaffe R L 1984 Phys. Rev. D 302379
[28] Holdom B, Ren J, Zhang C 2018 Phys. Rev. Lett. 120222001
[29] Wang J T, Peng G X 2023 Int. J. Mod. Phys. E 322350033
[30] Fowler G, Raha S, Weiner R 1981 Z. Phys. C 9271
[31] Peng G X, Chiang H C, Yang J J, Li L, Liu B 1999 Phys. Rev. C 61015201
[32] Wen X J, Zhong X H, Peng G X, Shen P N, Ning P Z 2005 Phys. Rev. C 72015204
[33] Chen H M, Xia C J, Peng G X 2022 Chin. Phys. C 46055102
[34] Damour T, Nagar A 2009 Phys. Rev. D 80084035
[35] Fonseca E, Pennucci T T, Ellis J A, Stairs I H, Nice D J, Ransom S M, Demorest P B, Arzoumanian Z, Crowter K, Dolch T, Ferdman R D, Gonzalez M E, Jones G, Jones M L, Lam M T, Levin L, McLaughlin M A, Stovall K, Swiggum J K, Zhu W 2016 Astrophys. J. 832167
[36] Chu P C, Chen L W 2014 Astrophys. J 780135
[37] Xu J F, Xia C J, Lu Z Y, Peng G X, Zhao Y P 2022 Nucl. Sci. Tech. 33143
[38] Xu J F, Cui L, Xia C J, Lu Z Y 2024 Nucl. Phys. Rev. 41325
[39] Cui S S, Peng G X, Lu Z Y, Peng C, Xu J F 2015 Nucl. Sci. Tech. 2640503
[40] Yang L, Wen X J 2017 Phys. Rev. D 96056023
[41] Chu P C, Li X H, Ma H Y, Wang B, Dong Y M, Zhang X M 2018 Phys. Lett. B 2502447
[42] Felipe R G, Martinez A P, Rojas H P, Orsaria M 2008 Phys. Rev. C 77015807
[43] Chu P C, Liu H, Du X B 2024 Acta Phys. Sin. 73052101
[44] Pal S, Chaudhuri G 2024 Phys. Rev. D 110123021
[45] Zheng X P, Yang S H, Li J R 2003 Astrophys. J. Lett. 585 L135
[46] Gourgoulhon E, Haensel P, Livine R, Paluch E, Bonazzola S, Marck J A 1999 Astron. Astrophys. 349851
[47] Yuan W L, Li A 2024 Astrophys. J. 9963
[48] Bai Y, Chen T K 2025 arXiv: 2502.20241
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