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1、二倍太阳质量中子星的计算研究赵先锋滁州学院机械与电子工程学院6/30/2021MainContentIntroductionTheRMFtheoryandthemassofaneutronstarApproximatelimitationofthehyperoncouplingconstantsFourofthepossiblemodelsfortheneutronstarPSRJ1614-2230Summary6/30/20212Ⅰ.Introduction1.Thediscoveryofthetwo-timessol
2、armassneutronstarPSRJ1614-2230TheneutronstarPSRJ1614-2230,whichmassis1.97M⊙andmaybetheheaviestbynow,wasobservedin2010.Obviously,itwillbemeaningfultodescribeitsmasstheoretically.6/30/20213BasedonEOS-independentanalyticsolutionsofEinstein’sequations,Demorestetalcal
3、culatedthemassoftheneutronstarandfoundthatthecalculations,whichisinthehadroniclevel,cannotobtainthemassoftheneutronstarPSRJ1614-2230becauseofitstoosmallermass.Butwethinkthatthismaybequestionable.2.Inthehadroniclevel,themassofneutronstar1.97M⊙canbeobtainedifthesui
4、tableEOSandthecouplingconstantsarechosen6/30/202141985,consideringtheoctet,themassofneutronstarcalculatedbyGlendenningisintherangeof1.5~1.8M⊙intheframeworkofrelativisticmeanfield(RMF)theory.Butifonlynucleonsbeingincludedintheneutronstar,themassofneutronstarheobta
5、inedwouldbe2.36M⊙.Itisobviousthatconsideringthehyperonswithinneutronstarwouldreducethemass.6/30/20215Calculationsshowthattheneutron-starmassisverysensitivetothehyperoncouplingconstants. Oneoftheparameterselectionmethodsistochoosethecouplingconstantsofmesonωbythec
6、onstituentquarkmodel[SU(6)symmetry]andtochoosethecouplingsconstantsofmesonσbyfittingtheΛ,ΣandΞwelldepthinnuclearmatter. Becausetheenergydensityofneutronstarmatterisseveraltimeslargerthanthesaturationnucleondensity,thepriorparameterselectionmethodstoagreatextentis
7、extrapolative.Intheinteriorofaneutronstar,thehyperonswouldbeproducedwiththebaryonnumberdensityincrease.Soitisreasonabletothinkthatneutronstarscontaininghyperons.6/30/20216Fromtheresultsaboveitcanbeseenthat,consideringnucleonswithinneutronstars,themassofneutronsta
8、rwhichisgreaterthan1.97M⊙maybeobtainedifthesuitableEOSandthecouplingconstantsarechosen.Inthiswork,weapplytheRMFtheorytodescribethemassoftheneutronstarPSRJ1614-
