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It is predicted in many theories beyond the standard model that the new interaction relevant to spin is existent. The exchange of an axial vector particle will result in attractive dipole-dipole interaction which can be viewed as an effective magnetic potential that looks quite different from those expected from electromagnetism. In this work, we demonstrate that, instead of the laboratory spin source, stringent constraints can be set on these attractive spin-spin interactions from polarized nuclear matters within neutron stars which have extremely strong magnetic fields (up to 1015 G in some cases). By considering such an exotic interaction within the framework of relativistic mean field model, we find that the stability of infinite nuclear matter can be influenced significantly when the ratio of coupling strength to boson mass become larger than
$g_{\rm A}^2/m_{\rm Z'}^2 \sim {\cal O}(10 \, {\rm GeV^{-2}})$ . Furthermore, based on the curvature matrix approach, when$g_{\rm A}^2/m_{\rm Z'}^2 > 130 \, {\rm GeV^{-2}}$ , phase transition inside low-density nuclear matter will no longer take place before the pressure of nuclear matter becomes zero, which forbids core-crust transition at the inner edge separating the liquid core from the solid crust of neutron stars. Thus bare neutron stars without any crusts are predicted. However, observations of pulsar glitches, i.e., the occasional disruptions of the extremely regular pulsations from magnetized, rotating neutron stars, imply the existence of crusts inside these dense objects. This in turn constrains the strength of the exotic interaction. In fact, in the case of dipole-dipole force on a length scale between µm to cm, the highest value of these constraints can be 8 orders of magnitude higher than those from existing laboratory results.-
Keywords:
- neutron star /
- theories beyond standard model /
- new interactions
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图 1 中子星物质状态方程(能量密度、压强)随重子数密度的变化, 其中轴矢量相互作用的有效耦合常数分别等于
$\bar{g}_{\rm A}^2/m_{\rm Z'}^2 = 0, \; 9.9 $ 和30 GeV–2Figure 1. Equation of states inside neutron stars as a function of the baryon density for β-stable nuclear matter where the effective couplings to Z' field are
$\bar{g}_{\rm A}^2/m_{\rm Z'}^2 = 0, \; 9.9$ and 30 GeV–2, respectively.
图 2 中子星壳-芯转变密度(
$n_{\rm t}$ )与核物质零压点($n_{\rm c}$ )随$\bar{g}_{\rm A}^2/m_{\rm Z'}^2$ 的变化曲线Figure 2. Core-crust transition density
$n_{\rm t}$ as well as zero-pressure point density$n_{\rm c}$ of nuclear matter as functions of$\bar{g}_{\rm A}^2/m_{\rm Z'}^2$ .
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[1] ATLAS Collaboration 2012 Phys. Lett. B 716 1
Google Scholar
[2] CMS Collaboration 2012 Phys. Lett. B 716 30
Google Scholar
[3] LIGO Scientific Collaboration and Virgo Collaboration 2016 Phys. Rev. Lett. 116 061102
Google Scholar
[4] LIGO Scientific Collaboration and Virgo Collaboration 2016 Phys. Rev. Lett. 116 241103
Google Scholar
[5] LHCb Collaboration 2016 JHEP 2016 104
Google Scholar
[6] 鲁公儒, 罗鹏晖, 黄金书 2009 物理学报 58 8166
Google Scholar
Lu G R, Luo P H, Huang J S 2009 Acta Phys. Sin. 58 8166
Google Scholar
[7] 鲁公儒, 李新强, 李艳敏, 苏方 2012 物理学报 61 241301
Google Scholar
Lu G R, Li X Q, Li Y M, Su Fang 2012 Acta Phys. Sin. 61 241301
Google Scholar
[8] Feng J L, Fornal B, Galon I, Gardner S, Smolinsky J, Tait T M P, Tanedo P 2016 Phys. Rev. Lett. 117 071803
Google Scholar
[9] Dine M, Fischler W, Srednicki M 1981 Phys. Lett. B 104 199
Google Scholar
[10] Fayet P 1980 Phys. Lett. B 95 285
Google Scholar
[11] Will C M 2014 Living Rev. Relativity 17 4
Google Scholar
[12] Ramsey N F 1979 Physica A 96 285
[13] Ledbetter M P, Romalis M V, Kimball D F J 2013 Phys. Rev. Lett. 110 040402
Google Scholar
[14] Vasilakis G, Brown J M, Kornack T W, Romalis M V 2009 Phys. Rev. Lett. 103 261801
Google Scholar
[15] Hunter L, Gordon J, Peck S, Ang D, Lin J F 2013 Science 339 928
Google Scholar
[16] Wen D H, Li B A, Chen L W 2009 Phys. Rev. Lett. 103 211102
Google Scholar
[17] Xu J, Li B A, Chen L W, Zheng H 2013 J. Phys. G: Nucl. Part. Phys. 40 035107
Google Scholar
[18] Manchester R N, Hobbs G B, Teoh A, Hobbs M 2005 The Astronomical Journal 129 1993
Google Scholar
[19] Xu J, Chen L W, Li B A, Ma H R 2009 Astrophys. J. 697 1549
Google Scholar
[20] Anderson P W, Itoh N 1975 Nature 256 25
Google Scholar
[21] Link B, Epstein R I, Lattimer J M 1999 Phys. Rev. Lett. 83 3362
Google Scholar
[22] Li B A, Chen L W, Ko C M 2008 Phys. Rep. 464 113
Google Scholar
[23] Cai B J, Chen L W 2012 Phys. Rev. C 85 024302
[24] Fattoyev F J, Horowitz C J, Piekarewicz J, Shen G 2010 Phys. Rev. C 82 055803
Google Scholar
[25] Zheng H, Chen L W 2012 Phys. Rev. D 85 043013
Google Scholar
[26] Piegsa F M 2012 Phys. Rev. Lett. 108 181801
Google Scholar
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