The physics of strong magnetic fields of magnetars.docx
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The physics of strong magnetic fields of magnetars.docx
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Thephysicsofstrongmagneticfieldsofmagnetars
Thephysicsofstrongmagneticfieldsofmagnetars
DepartmentofAstronomy,NanjingUniversity,Nanjing,210093,China.
Abstract:
Aphasetransitionfromparamagnetismtoferromagnetisminneutronstarinteriorisexplored.Sincethereis3P2neutronsuperfluidinneutronstarinterior,itcanbetreatedasasystemofmagneticdipoles.Underthepresenceofbackgroundmagneticfield,themagneticdipolestendtoaligninthesamedirection.Belowacriticaltemperature,thereisaphasetransitionfromparamagnetismtoferromagnetism.Andthisgivesaconvenientexplanationofthestrongmagneticfieldofmagnetars.Inourpointofview,thereisanupperlimitforthemagneticfieldstrengthofmagnetars.Themaximumfieldstrengthofmagnetarsisabout(3.0-4.0)1015gauss.Thiscanbetesteddirectlybyfurtherinvestigations.
Keywords:
magneticfields—stars:
neutron—pulsar:
general
I.Introduction
Itisgenerallyacceptedthatthereareverystrongmagneticfields,B>1012gauss,formostradiopulsars(e.g.ShapiroandTeukolski1983).Thereprobablyaremagnetarswithmagneticfieldstrengthexceedingthequantumcriticalthreshold,Hcr=4.4141013gauss(Duncan&Thompson1992;Paczynski1992;Usov1992;Thompson&Duncan1995,1996).AnomalousX-rayPulsars(AXPs)andSoftGammaRepeaters(SGRs)areidentifiedasclassesofmagnetarcandidates(e.g.Kouvelliotouetal.1998,1999;Hurleyetal.1999;Mereghetti&Stella1995;Wilsonetal.1999;Kaspietal.1999).Themagneticfieldsofthemagnetars,whichcanbededucedfromtheirlongspinperiods(P~5-12s)andspindownrate(
)basedonthestandardmagneticdipolarradiation,aresostrongastoreachtwoordersofmagnitudethequantumcriticalthresholdHcr.Moreover,thesameestimateofthemagneticfieldisderivedfromtheobservationofanabsorptionlineintheX-rayspectrumofSGR1806-20(Ibrahimetal.2002).
Apuzzleiswhatistheoriginofstrongmagneticfieldofmagnetars.Apossibleexplanationisthatthestrongmagneticfieldofneutronstarsoriginatesfromthecollapseofthecoreofasupernovawiththeconservationofmagneticflux(e.g.Ostriker&Gunn,1969)(thefossilfieldhypothesis);thereforemagneticfieldof
oftheprogenitorsisrequired.Braithwaite&Spruit(2004)analysedthestructureofthemagneticfieldsinAstarsandwhitedwarfs,anddemonstratedtheformationofstablefieldconfigurationsaccordingtothefossilfieldhypothesis.Ferrario&Wickramasinghe(2006)studiedthefielddistributionofthewhitedwarfprogenitors,andtheysuggestedthatmagnetarsaredescendedfromthehighmagneticfieldmassiveprogenitors.However,thedetailedcalculationaboutthemagneticfieldofmagnetarshavenotbeencarriedoutdirectly.Moreover,theprogenitorsofmagnetarshavenotbeenidentifiedinobservations.
AnotherpopularmechanismispresentedbyDuncanandThompson(Duncan&Thompson1992;Thompson&Duncan1993).Theypointoutthatthereareviolentconvectionintheprocessofpro-neutronstarsformation,andanefficientα-Ωdynamocanamplifythemagneticfieldtothefieldstrengthofmagnetarsinseveralsecondsiftheinitialspinperiodofthemagnetarislessthan3msandtheproto-neutronstarsrotatedifferentially.Nevertheless,aspointedoutbyBraithwaite&Spruit(2004),thedynamohypothesismaybedifficulttoproduceenoughhighfieldandexplainthecorrelationwithrotation.Recently,Vink&Kuiper(2006)studiedtheremnantenergeticofmagnetars.Theydetectedthatthesupernovaexplosionenergyofthemagnetarsissimilartothatofnormalradiopulsars.However,ifthefieldsofthemagnetarsoriginatefromthedynamohypothesis,millisecondinitialspinperiodshouldbeexpected,theexplosionshouldbeasenergeticasthehypernovasincetherotationalenergyofthemillisecondproto-neutronislargeenoughnottobeneglectedinpoweringsupernova.
Thefossilfieldhypothesisandthedynamohypothesisarerelativelymaturemodelsastotheoriginofthehighmagneticfield.Bothofthemhavebeenemployedtointerpretsomeobservationssuccessfully,whereassomenewobservationalresultsmaychallengetothem.Altogether,theoriginofthehighmagneticfieldsofmagnetarsisanactiveandabsorbingissuewhichneedfurtherwork.Severalmodelshavealreadybeenproposedbasedontheferromagnetismofthenetronstarmatter,e.g.Iwazaki(2005)arguedthatthehugemagneticfieldofmagnetarsissomecolorferromagnetismofquarkmatter.
Inthispaperweproposeanewideafortheoriginofthemagnetars.Thestrongmagneticfieldsofthemagnetarsmayoriginatefromtheinducedmagneticmomentofthe3P2neutronCooperpairsintheanisotropicneutronsuperfluid.
II.Anisotropic3P2neutronsuperfluid
Therearetworelevantregimesofneutronsuperfluidintheneutronstarinterior:
oneistheisotropic1S0neutronsuperfluidwiththecriticaltemperatureT(1S0)11010Kinadensityrange11010<(g/cm3)<1.61014.Theotheristheanisotropic3P2neutronsuperfluidwithawidedensityrange1.31014<(g/cm3)<7.21014.Thecriticaltemperature
is
.
(1)
Wenotethattheenergygap(3P2)isalmostaconstantaboutthemaximumwithanerrorlessthan3%inaratherwidedensityregion3.31014<(g/cm3)<5.21014(seeFig.2ofElgagøyetal.1996,butweneglecttheFstateofneutronCooperpairhere).
A3P2neutronCooperpairhasaspinwithquantumnumber,=1.Themagneticmomentofthe3P2neutronCooperpairistwicethatoftheabnormalmagneticmomentofaneutron,2ninmagnitude,anditsprojectionontheexternalmagneticfield(z-direction)isz×(2n),z=1,0,-1,where
.
Itisinterestingtonotethatthebehaviorofthe3P2neutronsuperfluidisverysimilartothatoftheliquid3Heatverylowtemperature(Leggett1975):
1)Theprojectiondistributionforthemagneticmomentofthe3P2neutronCooperpairsintheabsenceofexternalmagneticfieldisstochastic,or“EqualSpinPair”(ESP)phasesimilartotheA-phaseoftheliquid3Heatverylowtemperature(Leggett1975).The3P2neutronsuperfluidisbasicallyisotropicwithoutnetmagneticmomentintheabsenceoftheexternalmagneticfield.WenameitastheA-phaseofthe3P2neutronsuperfluidsimilartotheAphaseoftheliquid3Heatverylowtemperature(Leggett1975).
2)However,theprojectiondistributionforthemagneticmomentofthe3P2neutronCooperpairsinthepresenceofexternalmagneticfieldisnotstochastic.Thenumberof3P2neutronCooperpairwithparamagneticmomentismorethantheoneswithdiamagneticmoment.Therefore,the3P2neutronsuperfluidhasanetinducedparamagneticmomentanditsbehaviorisanisotropicinthepresenceofexternalmagneticfield.WenameitastheB-phaseofthe3P2neutronsuperfluidsimilartotheBphaseoftheliquid3Heatverylowtemperature(Leggett1975).
Thefullstoryofanisotropic3P2neutronsuperfluidismorecomplicatedwhenmagneticinteractionisintroduced.Weconsiderthisproblemfromtheeffectivefieldtheorypointofview(Feng&Jin2005).Itispossiblethattheinducedmagneticfieldofthe3P2superfluidwillboosttheneutronstarmagneticfieldtothatofmagnetars,wheneverthestellarinternaltemperatureisbelowthephasetransitiontemperature.WewilldiscussthisinsectionV.
III.Inducedparamagneticmomentofthe3P2neutronsuperfluidintheB-phase
Theinducedparamagneticmomentofthe3P2neutronsuperfluidintheB-phasemaybesimplyestimatedasfollows:
thesystemofthe3P2neutronCooperpairswithspinquantumnumber,
maybetreatedasaBose-Einsteinsystem.ItobeystheBose-Einsteinstatistics.
Amagneticdipoletendstoaligninthedirectionoftheexternalmagneticfield.The3P2neutronCooperpairhasenergyZ2nB(Z=1,0,-1)intheappliedmagneticfieldduetotheabnormalmagneticmomentoftheneutrons.Herenistheabsolutevalueofthemagneticmomentofaneutron,weusethisconventionfromnowon.Bisthebackgroundmagneticfield.Whileintheeffectivefieldframe,Bisthetotalmagneticfield.DetaileddiscussionwillbepresentedinsectionV.Wedenotethenumberdensityof3P2neutronCooperpairswithspinprojectionz=1,0,-1byn1,n0andn-1respectively.Theirrelativeratiosare
(2)
.(3)
Thedifferenceofthenumberdensityof3P2neutronCooperpairswithparamagneticanddiamagneticmomentis
(4)
.(5)
TheBrillouinfunction,f(nB/kT),isintroducedtotakeintoaccounttheeffectofthermalmotionWenotethatfItisanincreasingfunction,inparticular,
and
.f(nB/kT)increasewithdecreasingtemperature.AndthisisthemathematicalformulafortheB-phaseofthe3P2superfluid.
Arelevantquestionishowmanyneutronshavebeencombinedintothe3P2Cooperpairs?
Thetotalnumberofneutronsisgivenby
(Herekisawavevector,
pisthemomentum).Theneutronscombinedintothe3P2CooperpairsarejustinathinlayerintheFermisurfacewiththickness
.Thenwehave
(k< .(6) Here,wewouldliketoemphasizethattheenergygap,,isthebindingenergyoftheCooperpairratherthanavariationoftheFermienergyduetoadisturbanceorduetothevariationofparticlenumberdensity(Inthelattercase,itiseasytomisunderstandtoget or ).Therefore,wethinktheeq.(6)isaproperestimation. Forthenon–relativisticneutrongas( ),thefractionoftheneutronsthatcombinedintothe3P2Cooperpairsis (7) . TheFermienergyoftheneutronsystemmaybecalculatedbytheformula .(8) Theenergygapoftheanisotropicneutronsuperfluidis(3P2)~0.05MeV(Elgagøyetal.
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