Chinese Physics C > 2025, Vol. 49 > Issue(9): 094005 DOI: 10.1088/1674-1137/add9fd

Constraint on symmetry energy slope using neutron skins of⁴⁸Ca,⁶⁴Ni,¹²⁴Sn, and²⁰⁸Pb and its impact on neutron star radius

1.
Key Laboratory of Radiation Physics and Technology of the Ministry of Education, Institute of Nuclear Science and Technology, Sichuan University, Chengdu 610064, China
2.
Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
3.
School of Physics, Nankai University, Tianjin 300071, China
4.
RIKEN Nishina Center, Wako, Saitama 351-0198, Japan

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Abstract：
We constrain the symmetry energy slope Lat the saturation density using the neutron skin values of ⁴⁸Ca, ⁶⁴Ni, ¹²⁴Sn, and ²⁰⁸Pb determined by various experiments. The resulting Lof 50(6) MeV is consistent with the world-averaged value from different observables and methodologies. The implications of newly constrained Lon the radius determinations of 1.4 solar-mass neutron stars are also discussed based on the established $ R_{1.4}$ - Llinear relationships by the DD-ME2 and TW99 EoS families.
- neutron skin,
- symmetry energy slope,
- neutron star radius

References

[1]	B. Li, L. Chen, and C. Ko, Phys. Rep.464, 113 (2008) doi:10.1016/j.physrep.2008.04.005
[2]	J. M. Lattimer and M. Prakash, Science304, 536 (2004) doi:10.1126/science.1090720
[3]	J. M. Lattimer and M. Prakesh, Phys. Rep.442, 109 (2007) doi:10.1016/j.physrep.2007.02.003
[4]	N. Alam, B. K. Agrawal, M. Fortinet al., Phys. Rev. C94, 052801(R) (2016) doi:10.1103/PhysRevC.94.052801
[5]	J. Hu, S. Bao, Y. Zhanget al., Prog. Theor. Exp. Phys.2020, 043D01 (2020) doi:10.1093/ptep/ptaa016
[6]	B.-A. Li and M. Magno, Phys. Rev. C102, 045807 (2020) doi:10.1103/PhysRevC.102.045807
[7]	B.-A. Li, B.-J. Cai, W.-J. Xieet al., Universe7, 182 (2021) doi:10.3390/universe7060182
[8]	J. Richter and B.-A. Li, Phys. Rev. C108, 055803 (2023) doi:10.1103/PhysRevC.108.055803
[9]	K. Huang, H. Shen, J. Hu, and Y. Zhang, Phys. Rev. C109, 045804 (2024) doi:10.1103/PhysRevC.109.045804
[10]	X. Viñas, P. Bano, Z. Naiket al., Symmetry16, 215 (2024) doi:10.3390/sym16020215
[11]	U. Garg and G. Colò, Prog. Part. Nucl. Phys.101, 55 (2018) doi:10.1016/j.ppnp.2018.03.001
[12]	S. Shlomo, V. M. Kolomietz, and G. Colò, Eur. Phys. J. A30, 23 (2006) doi:10.1140/epja/i2006-10100-3
[13]	Z. Z. Li, Y. F. Niu, and G. Colò, Phys. Rev. Lett.131, 082501 (2023) doi:10.1103/PhysRevLett.131.082501
[14]	H. Sotani, N. Nishimura, and T. Naito, Prog. Theor. Exp. Phys.2022, 041D01 (2022) doi:10.1093/ptep/ptac055
[15]	B. Sun, S. Bhattiprolu, and J. M. Lattimer, Phys. Rev. C109, 055801 (2024) doi:10.1103/PhysRevC.109.055801
[16]	B. A. Brown, Phys. Rev. Lett.85, 5296 (2000) doi:10.1103/PhysRevLett.85.5296
[17]	M. von Schmid, T. Aumann, S. Bagchiet al., Eur. Phys. J. A59, 83 (2023) doi:10.1140/epja/s10050-023-00967-z
[18]	J. T. Zhang, P. Ma, Y. Huanget al., Phys. Rev. C108, 014614 (2023) doi:10.1103/PhysRevC.108.014614
[19]	K. Yue, J. T. Zhang, X. L. Tuet al., Phys. Rev. C100, 054609 (2019) doi:10.1103/PhysRevC.100.054609
[20]	Y. Huang, S. Y. Xia, Y. F. Liet al., Phys. Lett. B856, 138902 (2024) doi:10.1016/j.physletb.2024.138902
[21]	Y. Huang, L. Xayavong, X. L. Tuet al., Phys. Lett. B847, 138293 (2023) doi:10.1016/j.physletb.2023.138293
[22]	A. Trzcińska, J. Jastrzebski, P. Lubińskiet al., Phys. Rev. Lett.87, 082501 (2001) doi:10.1103/PhysRevLett.87.082501
[23]	D. Adhikari, H. Albataineh, D. Androicet al., Phys. Rev. Lett.126, 172502 (2021) doi:10.1103/PhysRevLett.126.172502
[24]	G. A. Korolev, A. V. Dobrovolsky, A. G. Inglessiet al., Phys. Lett. B780, 200 (2018) doi:10.1016/j.physletb.2018.03.013
[25]	M. Tanaka, M. Takechi, A. Hommaet al., Phys. Rev. Lett.124, 102501 (2020) doi:10.1103/PhysRevLett.124.102501
[26]	S. Terashima, H. Sakaguchi, H. Takedaet al., Phys. Rev. C77, 024317 (2008) doi:10.1103/PhysRevC.77.024317
[27]	J. T. Zhang, X. L. Tu, P. Sarrigurenet al., Phys. Rev. C104, 034303 (2021) doi:10.1103/PhysRevC.104.034303
[28]	G. D. Alkhazov, M. N. Andronenko, A. V. Dobrovolskyet al., Phys. Rev. Lett.78, 2313 (1997) doi:10.1103/PhysRevLett.78.2313
[29]	I. Tanihata, H. Hamagaki, O. Hashimotoet al., Phys. Rev. Lett.55, 2676 (1985) doi:10.1103/PhysRevLett.55.2676
[30]	A. Krasznahorkay, M. Fujiwara, P. van Aarleet al., Phys. Rev. Lett.82, 3216 (1999) doi:10.1103/PhysRevLett.82.3216
[31]	H. Sagawa, S. Yoshida, X.-R. Zhouet al., Phys. Rev. C76, 024301 (2007) doi:10.1103/PhysRevC.76.024301
[32]	J. Jastrzebski, A. Trzcińska, P. Lubińskiet al., Int. J. Mod. Phys. E13, 343 (2004) doi:10.1142/S0218301304002168
[33]	D. Adhikari, H. Albataineh, D. Androicet al., Phys. Rev. Lett.129, 042501 (2022) doi:10.1103/PhysRevLett.129.042501
[34]	P.-G. Reinhard, X. Roca-Maza, and W. Nazarewicz, Phys. Rev. Lett.129, 232501 (2022) doi:10.1103/PhysRevLett.129.232501
[35]	C. Mondal and F. Gulminelli, Phys. Rev. C107, 015801 (2023) doi:10.1103/PhysRevC.107.015801
[36]	T. Miyatsu, M.-K. Cheoun, K. Kimet al., Phys. Lett. B843, 138013 (2023) doi:10.1016/j.physletb.2023.138013
[37]	T.-G. Yue, Z. Zhang, and L.-W. Chen, arXiv: 2406.03844v1
[38]	Z. Zhang and L.-W. Chen, Phys. Rev. C108, 024317 (2023) doi:10.1103/PhysRevC.108.024317
[39]	F. Sammarruca, Symmetry16, 34 (2024) doi:10.3390/sym16010034
[40]	J. M. Lattimer, Particles6, 30 (2023) doi:10.3390/particles6010003
[41]	B. T. Reed, F. J. Fattoyev, C. J. Horowitzet al., Phys. Rev. Lett.126, 172503 (2021) doi:10.1103/PhysRevLett.126.172503
[42]	Z. Zhang and L.-W. Chen, Phys. Lett. B726, 234 (2013) doi:10.1016/j.physletb.2013.08.002
[43]	L.-W. Chen, C. M. Ko, B.-A. Liet al., Phys. Rev. C82, 024321 (2010) doi:10.1103/PhysRevC.82.024321
[44]	X. Roca-Maza, M. Centelles, X. Viñaset al., Phys. Rev. Lett.106, 252501 (2011) doi:10.1103/PhysRevLett.106.252501
[45]	J. Friedrich and P.-G. Reinhard, Phys. Rev. C33, 335 (1986) doi:10.1103/PhysRevC.33.335
[46]	M. Beiner, H. Flocard, N. Van Giaiet al., Nucl. Phys. A238, 29 (1975) doi:10.1016/0375-9474(75)90338-3
[47]	J. Dobaczewski, H. Flocard, and J. Treiner, Nucl. Phys. A422, 103 (1984) doi:10.1016/0375-9474(84)90433-0
[48]	J. Gómez, C. Prieto, and J. Navarro, Nucl. Phys. A549, 125 (1992) doi:10.1016/0375-9474(92)90070-Z
[49]	F. Tondeur, M. Brack, M. Farineet al., Nucl. Phys. A420, 297 (1984) doi:10.1016/0375-9474(84)90444-5
[50]	M. Rayet, M. Arnould, G. Pauluset al., Astron. Astrophysics.116, 183 (1982)
[51]	N. Van Giai and H. Sagawa, Phys. Lett. B106, 379 (1981) doi:10.1016/0370-2693(81)90646-8
[52]	J. Bartel, P. Quentin, M. Bracket al., Nucl. Phys. A386, 79 (1982) doi:10.1016/0375-9474(82)90403-1
[53]	E. Chabanat, P. Bonche, P. Haenselet al., Nucl. Phys. A635, 231 (1998) doi:10.1016/S0375-9474(98)00180-8
[54]	H. Krivine, J. Treiner, and O. Bohigas, Nucl. Phys. A336, 155 (1980) doi:10.1016/0375-9474(80)90618-1
[55]	G. A. Lalazissis, T. Nikšić, D. Vretenaret al., Phys. Rev. C71, 024312 (2005) doi:10.1103/PhysRevC.71.024312
[56]	S. Typel and H. H. Wolter, Nucl. Phys. A656, 331 (1999) doi:10.1016/S0375-9474(99)00310-3
[57]	W. Long, H. Sagawa, J. Menget al., Europhys. Lett.82, 12001 (2008) doi:10.1209/0295-5075/82/12001
[58]	W. Long, J. Meng, N. Van Giaiet al., Phys. Rev. C69, 034319 (2004) doi:10.1103/PhysRevC.69.034319
[59]	W.-H. Long, N. Van Giai, and J. Meng, Phys. Lett. B640, 150 (2006) doi:10.1016/j.physletb.2006.07.064
[60]	G. A. Lalazissis, J. König, and P. Ring, Phys. Rev. C55, 540 (1997) doi:10.1103/PhysRevC.55.540
[61]	M. Bender, K. Rutz, P.-G. Reinhardet al., Phys. Rev. C60, 034304 (1999) doi:10.1103/PhysRevC.60.034304
[62]	M. Rufa, P.-G. Reinhard, J. A. Maruhnet al, Phys. Rev. C38, 390 (1988) doi:10.1103/PhysRevC.38.390
[63]	P. Reinhard, M. Rufa, J. Maruhnet al., Z. Phys. A323, 13 (1986)

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Y. Huang, K. X. Huang, Z. X. Yang, X. L. Tu, J. N. Hu, J. T. Zhang and J. F. Han. Constraint of symmetry energy slope using neutron skins of ⁴⁸Ca, ⁶⁴Ni, ¹²⁴Sn, and ²⁰⁸Pb and its impact on neutron star radius[J]. Chinese Physics C. doi: 10.1088/1674-1137/add9fd

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Constraint on symmetry energy slope using neutron skins of48Ca,64Ni,124Sn, and208Pb and its impact on neutron star radius

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Constraint on symmetry energy slope using neutron skins of⁴⁸Ca,⁶⁴Ni,¹²⁴Sn, and²⁰⁸Pb and its impact on neutron star radius