Dynamics of scalar fields in the background of rotating black holes II A note on superradia

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arXiv:gr-qc/9802059v1 23 Feb 1998DynamicsofscalarfieldsinthebackgroundofrotatingblackholesII:Anoteonsuperradiance

NilsAndersson(1,2),PabloLaguna(3)andPhilipposPapadopoulos(4)(1)Institutf¨urAstronomieundAstrophysik

Universit¨atT¨ubingen,D-72076T¨ubingen,Germany(2)DepartmentofMathematics,UniversityofSouthampton,Southampton,UK

(3)DepartmentofAstronomy&Astrophysicsand

CenterforGravitationalPhysics&GeometryPennStateUniversity,UniversityPark,PA16802,USA(4)Max-Planck-Institutf¨urGravitationsphysik

Schlaatzweg1,14473Potsdam,Germany(February7,2008)

Weanalyzetheamplificationduetoso-calledsuperradiancefromthescatteringofpulsesoffrotatingblackholesasanumericaltimeevolutionproblem.Weconsiderthe“worstpossiblecase”ofscalarfieldpulsesforwhichsuperradianceeffectsyieldamplifications<1%.Weshowthatthissmalleffectcanbeisolatedbynumericallyevolvingquasi-monochromatic,modulatedpulseswitharecentlydevelopedTeukolskycode.Theresultsshowthatitispossibletostudysuperradianceinthetimedomain,butonlyiftheinitialdataiscarefullytuned.Thisillustratestheintrinsicdifficultiesofdetectingsuperradianceinmoregeneralevolutionscenarios.

I.INTRODUCTIONInthelastfewyears,wehavebeeninvolvedinthedevelopmentofanumericalcodeforthetimeevolutionofperturbationsofrotatingblackholesbasedontheTeukolskyequation[1,2].Thereareseveralmotivationsforthiswork.Oneisthedesiretorevisitproblemsthathavepreviously(mainlyinthe1970s)onlybeenapproachedinthefrequencydomain.Thatis,ourgoalistoexploretheeffectsoftherotationoftheblackholefroma“time-evolution”pointofview.Moreimportantly,ourultimategoalistoprovideaframeworkthatwill,onceweunderstandhowtoconstructastrophysicallyrelevantinitialdata[3],beusedtoextendtheclose-limitapproximationofhead-onblackholecollisionstothecaseofinspiralblackholemergers.Theworkingpremiseinhead-on,close-limitcollisions[4]isthatthemergercanbeviewedasperturbationsofnon-rotatingblackholes.Incontrast,aninspiralclose-limitapproximationrequiresperturbationsaboutarotatingblackhole.OurTeukolskycodeprojecttookusfirsttostudythedynamicsofscalarfieldsintheKerrgeometry[1].Thisworkmainlyconcernedthelate-time,power-lawbehaviourofascalarperturbation.Thesecondinstallmentconcernedgravitationalperturbations[2]anddiscussedthefulldynamicalresponseofablackholetoanexternalperturbation,namelythequasinormalmoderingingandthesubsequentlate-timetails.InRef.[2],wealsodealtbrieflywithsuper-radiance:Theanticipatedamplificationascertainwavelengthsarescatteredbytheblackhole.However,althoughtheresultsweobtainedindicatedthepresenceofsuperradiance[2],wefeelthatourpreviousanalysiswasnotcompletelysatisfactory.Hence,thegoalofthisshortpaperistoreturntotheissueofsuperradianceinasettingthatyieldsunequivocalevidenceforthesuperradiancephenomenon.Thedirectapproachtomeasuresuperradiancefromthetimeevolutionofperturbationsofrotatingblackholesistocomputetheenergyfluxgoing“downthehole”.Forperturbativefieldsthatposseswell-definedstress-energytensors(e.g.scalarandelectromagneticfields),itispossibletoconstructsuchaconservedenergyflux[5].Thecaseofgravitationalperturbationsisnotthatsimple[5,6].Forthisreason,wewillconcentrateouranalysisonthe“simple”caseofscalarperturbations.Thepricetopayisthatsuperradianteffectsinthiscaseare<1%[7],thusrequiringahighlyaccurateevolutioncode.Forscalarperturbations,theTeukolskyequationinBoyer-Lindquistcoordinatesreads󰀇(r2+a2)2

∂t2+4iMamr∂t−∂∂r

󰀆

−1∂θ󰀅sinθ∂Φ∆−1

M2−a2.Referencetotheazimuthalangleϕhasbeenremovedbyassumingthattheperturbationhasaharmonicdependenceeimϕ.

1II.SUPERRADIANCEINTHEFREQUENCYDOMAINInthestandardapproachtosolvetheTeukolskyequation,oneproceedsviaseparationofvariables.Forourpresentpurposes,itissufficienttonotethatthisessentiallycorrespondstoassumingthati)thetime-dependenceoftheperturbationisaccountedforviaFouriertransformation,andii)thereexistsasuitablesetofangularfunctionthatcanbeusedtoseparatethecoordinatesrandθ.Inthecaseofscalarperturbations,theangularfunctionsturnouttobestandardspheroidalwave-functions[8].Knowingthis,weassumearepresentation(foreachgivenintegerm)

Φ=󰀄dωe−iωt∞󰀁l=0Rlm(r,ω)Slm(θ,ω),(2)whereitshouldbenotedthattheangularfunctionsdependexplicitlyonthefrequencyω;thatis,theyareintrinsicallytime-dependentfunctions.Afteraseparationofvariablesoftheformgivenby(2),theproblemreducestoasingleordinarydifferentialequationforRlm(r,ω).Thisequationcanbewrittenas

d2Rlm(r2+a2)2−dG

2Mr+

.(6)

Alternatively,onecandeducethatenergycanbeextractedfromtheblackholeimmediatelyfromtheboundarycondition(4).Ifωalocalobserver,willinfactcorrespondtowavescomingoutoftheholeaccordingtoanobserveratinfinity.Thatis,forsuperradiantfrequencies,onewouldexpecttofindenergyflowingoutfromthehorizon,cf.[10].SuperradianceisthewaveanalogueofthestandardPenroseprocess,anditsexistenceimpliesthatitwouldinprinciplebepossibletominearotatingblackholeforsomeofitsrotationalenergy.Thismayseemexciting,butitisveryunlikelythatthiseffectwillplayarelevantroleinanyreasonableastrophysicalscenario.Nonetheless,itisaninterestingeffectthatdeservesaclosetheoreticalinvestigation.InFig.1,weshowasampleofresultsforthereflectioncoefficientinthecasewhenl=m=2.Theseresultswereobtainedbyastraightforwardintegrationof(3)andsubsequentextractionofR.Themaximumamplificationinthiscaseiscloseto0.2%.SimilarresultswereobtainedbyTeukolskyandPressmorethan25yearsago[5,7].Theyalsoconsideredelectromagneticwavesandgravitationalperturbationsandfoundthatthemaximumamplificationis0.3%forscalarwaves,4.4%forelectromagneticwavesandaslargeas138%forgravitationalwaves.GiventheresultsinFig.1,itisworthpointingoutthattheyagreewiththestandardconclusionsregardingtheapparent“size”ofarotatingblackholeasseenbydifferentobservers.Itiswell-known(seeforexample[11])thattheblackholewillappearlargertoaparticlemovingarounditinaretrogradeorbitthantoaparticleinaprogradeorbit.Thisisillustratedbythefactthattheunstablecircularphotonorbit(atr=3Minthenon-rotatingcase)islocatedatr=4Mforaretrogradephoton,whileitliesatr=Mforaprogradephoton.TheresultsinFig.1illustratethesameeffect:Inourcase,wehaveprogrademotionwhenω/mispositiveandretrogrademotionwhenω/misnegative.ThedatainFig.1correspondtom=2,andtheenhancedreflectionforpositivefrequenciesasa→Mhastheeffectthattheblackhole“lookssmaller”tosuchwaves.Conversely,theslightlydecreasedreflectionfornegativefrequenciesleadstotheblackholeappearing“larger”asa→M.