Tes$ng'theories'of'gravity'with'pulsars'and'binary'systems'
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1 Tes$ng'theories'of'gravity'with'pulsars'and'binary'systems' MichaelKramer Max-Planck-Ins3tutfürRadioastronomie JodrellBankCentreforAstrophysics,UniversityofManchester
2 Gravity ArethephysicallawsderivedhereonEarththesameasinthe restoftheuniverse? Forinstance,doestheastronaut fallinthesamewayeverywhereintheuniverse? Evennearexo3cmaIerinstronggravita3onalfields?
3 100+'years'of'General'Rela$vity'and'Tes$ng'it' Generalrela3vityconceptuallydifferentthandescrip3onofotherforces WeexpectthatGRmusteventuallyfail(incompa3bilitywithquantum theory,singulari3es),butwedon tknowhowandwhere WillEinsteinhavethelastwordon(macroscopic)gravityordoesGRfail farbelowtheplanckenergy? WhatisdarkmaIeranddarkenergy? Dowehavetomodifygravityonlargescales? Howtotestit? Dark MaIer Atoms DarkEnergy (NASA)
4 100+'years'of'General'Rela$vity'and'Tes$ng'it' Generalrela3vityconceptuallydifferentthandescrip3onofotherforces GRhasbeentestedprecisely,e.g.insolarsystem Classicaltests: -Mercuryperihelionadvance -Light-deflec3onatSun -Gravita3onalredshi\ Moderntestsinsolarsystem, -LunarLaserRanging(LLR) -Radarreflec3onatplanets,Cassinispacecra\signal -LAGEOS&GravityProbeB S3ll... (LR/ITP) Weneedtotestgravityinstrong,non-linearcondi3ons:NS+BH Whataretheproper3esofblackholes&gravita3onalwaves? UsingtechniquesandmethodsnotknowntoEinstein...
5 Outline' Introduc3on Pulsars&binaries:tes3ngGRanditsalterna3ves PulsarTimingArrays(PTAs):detec3ngGWs The(far&near)future:SKA+EHT/BHC Conclusions FundamentalPhysicsinRadioAstronomy Max-Planck-Ins3tutfürRadioastronomie
6 Pulsars ' almostblackholes ObjectsofextrememaIer: 10xnucleardensity B~B cr =4.4x10 9 Tesla Electr.fields~10 12 Volt F EM =10 11 F gravita3on High-temperaturesuperfluidsuperconductor bornin(usuallytypeii)supernovaexplosion:
7 Pulsars 'rotate'very'fast' J ad 1.4ms Crabpulsar 33ms Period J s Vela-Pulsar89ms 42,960 Rota3onsperminute 7 1,600 20,000 Speedatequator:45,000,000m/s=162Millionkm/h Centrifugalaccelera3on:20Milliong Pulsarsaremassive,fastrota3ngflywheels Pulsarsareexcellentclocks
8 Most'useful:'Pulsars'with'companions' ~'2500''radio'pulsars' 1.40ms(PSRJ ad) 8.50s(PSRJ ) ~'10%''binary'pulsars' Orbital(period(range( 94min(PSRJ ) 5.3yr(PSRJ ) Companions) MSS,WD,NS,planets Wanted:)PSR2BH) Simpleexperiment: i.e.measure(=3me)howapulsarfallsasatestmassinthegravita3onalpoten3alof acompanion(andinthegalaxy) acleanexperimentwithextremeprecision
9 A'simple'and'clean'experiment:'Pulsar'Timing' Pulsar3mingmeasuresarrival3me(TOA): Fold Fold Model TOA Residual Coherent3mingsolu3onabout1,000,000moreprecisethanDopplermethod
10 High'precision'measurements' 'What's'possible'today ' 'Spin'parameters:' Period: (2)ms(Verbiestetal.2008)Note:2aIosecondsuncertainty Astrometry:' Distance: 157(1)pc (Verbiestetal.2008) Propermo3on: (1)mas/yr (Verbiestetal.2008) Orbital'parameters:' Period: (8)day (Krameretal.inprep.) Projectedsemi-majoraxis: 31,656,123.76(15)km (Freireetal.2012) Eccentricity: 3.5(1.1) 10 7 (Freireetal.2012) Masses:' Massesofneutronstars: (2)/ (2)M (Krameretal.inprep.) MassofWDcompanion: 0.207(2)M (Hotanetal.2006) Massofmillisecondpulsar: 1.667(7)M (Freireetal.2012) Mainsequencestarcompanion: 1.029(3)M (Freireetal.2012) MassofJupiterandmoons: (2)x10-4 M (Championeta.2010) Rela$vis$c'effects:' Periastronadvance: (5)deg/yr (Weisbergetal.2010) Einsteindelay: (8)ms (Weisbergetal.2010) OrbitalGWdamping: 7.152(1)mm/day (Krameretal.inprep) Fundamental'constants:' Changein(dG/dt)/G:( 0.6±1.1) yr 1 (Zhuetal.2015) Gravita$onal'wave'detec$on:' Changeinrela3vedistance:100m/1lightyear (EPTA,NANOGrav,PPTA)
11 Outline' Introduc3on Pulsars&binaries:tes3ngGRanditsalterna3ves PulsarTimingArrays(PTAs):detec3ngGWs The(far&near)future:SKA+EHT/BHC Conclusions FundamentalPhysicsinRadioAstronomy Max-Planck-Ins3tutfürRadioastronomie
12 The'first'binary'pulsar' 'the'first'dns:'hulsettaylor'pulsar'' ms Hulse & Taylor (1975) ms
13 Comparison'HulseTTaylor'vs'Double'Pulsar' PSRB PSRJ A/B Morecompact Sun andmuchcloser PSRB PSRJ0737T3039A/B
14 The'Double'Pulsar'(Burgayetal.2003,Lyneetal.2004) Old22-mspulsarina147-minorbitwithyoung2.77-spulsar Orbitalveloci3esof1Mill.km/h Eclipsingbinaryincompact,slightlyeccentric(e=0.088)andedge-onorbit Ideallaboratoryforgravita3onalandfundamentalphysics Inpar3cular,exploita3onfortestsofgeneralrela3vity (Krameretal.2006,Bretonetal.2008,Krameretal.inprep.,Wexetal.inprep.) Animation by McGill McGill( Collaborators: C.Bassa,R.Brenton,M.Burgay, I.Cognard,N.,G.Desvignes, R.Ferdman,P.Freire,L.Guillemot, G.Hobbs,G.Janssen,P.Lazarus,D. Lorimer,A.Lyne,R.Manchester,M. McLaughlin,B.Perera,A.Possen3, J.Reynolds,J.Sarkissian,I.Stairs, B.Stappers,G.Thereau,N.Wex andmore
15 Double'Pulsar:'a'unique'rela$vis$c'doubleTline'system' Wecanmeasuretwoorbitsmassra3o Note:theory-independentto1PNorder (Damour&Deruelle1986,Damour2005) Hugeorbitalprecessionof ±0.0001deg/yr R x B x A = m A m B = ± (4xlargerthanHulse-Taylor) 2/3 P dω / dt = 3T b $ Sun # & " 2π % 5/3 ( m A + m B ) 2/3 1 e 2 m A +m B =( ± )M " Combined(GR): ComparetoMercury: m A =(1.3381±0.0007)M " = deg/yr &m B =(1.2489±0.0007)M " Newestmeasurement:dω/dt= (2)deg/yr-errorabout1/10x2PN
16 Double'Pulsar:'five'tests'in'one'system' Hugeorbitalprecessionof (2)deg/yr Clockvaria3onduetogravita3onalredshi\:385.6±2.6μs Latestmeasurement:383.9±0.5μs(improvement:x5 butnotx30) Obs.Val. Exp.(GR) =1.000 ± Asotherclocks,pulsarsrunslowerindeepgravita3onalpoten3als -Changingdistancetocompanion(andfeltgrav.poten3al)duringellip3calorbit
17 Double'Pulsar:'five'tests'in'one'system' Hugeorbitalprecessionof (2)deg/yr Clockvaria3onduetogravita3onalredshi\:383.9±0.5μs Shapirodelayinedge-onorbit:s=sin(i)= ( , ) s=sin(i)= ± i=88.7(+0.5,-0.8)deg Obs.Val(s) = ± new:89.29±0.05deg Exp.(GR) Obs.Val(r) Exp.(GR) =0.98 ± ,000km -Atsuperiorconjunc3on,pulsesfrompulsarApassBin<10,000kmdistance -Space-3menearcompanioniscurvedAddi3onalpathlength Delayinarrival3me dependingongeometryandcompanionmass
18 Hugeorbitalprecessionof (2)deg/yr Clockvaria3onduetogravita3onalredshi\:383.9±0.5μs Shapirodelayinedge-onorbit:s=sin(i)= ± Rela3vis3cspinprecession:Ω B =4.8(7)degyr -1 ShrinkageoforbitduetoGWemission:ΔP b =107.79±0.11ns/day Double'Pulsar:'five'tests'in'one'system' -Pulsarsapproacheachotherby 7.152±0.001mm/day Obs.Val Exp.(GR) = ± Mergerin85Millionyears Anima3onbyNASA/Rezzolla/AEI Precisionwillimprovewith3me:supersedingsolarsystemtestssoon
19 How'do'pulsars'compare'to'LIGO?' GW150914:' 90%(credible(regions(for(the(waveform( and(the(gw(frequency( ^ GW150914(v 0.4c) GW151226(v 0.4c) combined DoublePulsar(v 0.002c) GR'viola$ons'are'limited'to'less'than'4%' (foreffectsthatcannotbereabsorbedina redefini3onofparameters) [LSC/Virgo2016] (v 2 /c 2 correc3ons) Quadrupoleformula [LSC/Virgo2016,Krameretal.inprep.]
20 Combining'all'tests:'a'"massTmass'diagram"' Quasi-sta3onarystrongfieldtests Precession(of(periastron((17(deg/yr)( 7-2=5testsofGRplus1emergingone Shapiro(delay((130(μs)( Radia3vetests(gravita3onalwavedamping) Orbital(period(decay((A39(μs/yr)(
21 Higher'order'light'propaga$on:'Effect'of'moving'lens' 1.5PNShapiroEffect: A A A B B B
22 Higher'order'light'propaga$on:'Effect'of'light'bending' A A A A B B
23 Equa$onTofTState'Dependence'of'Periastron'Advance''' DoublePulsar: [ Kramer et al. (in prep.)] Lense-Thirring [Damour&Schäfer(1988)] Moment-of-iner3a
24 Future'Constrains'on'the'EOS'with'the'Double'Pulsar' MOCKdatasimula3onsoffuturepulsarsignals (KehlMScthesis,2015). ExampleforfutureEOSrestric3on(AP3) MeerKAT SKA1 FullSKA LTeffect preliminary(( Lense-Thirringprecession willbequalita3vely measureablewithska1 preliminary(( LaÇmer&Schutz2005 RestricttheEOSbymeasuring Lense-Thirringprecession withfuturetelescopes(ska)
25 Outline' Introduc3on Pulsars&binaries:tes3ngGRanditsalterna3ves PulsarTimingArrays(PTAs):detec3ngGWs The(far&near)future:SKA+EHT/BHC Conclusions FundamentalPhysicsinRadioAstronomy Max-Planck-Ins3tutfürRadioastronomie
26 Constraining'alterna$ve'theories' 'some'examples...' Scalar-tensorgravity Jordan-Fierz-Brans-Dicke Quadra3cscalar-tensorgravity (seeworkbydamour&esposito-farese) PSRJ ,PSRJ (Freireetal.2012,Antoniadisetal.'13) PSR-WDs,PSRJ ,PSRJ (Freireetal.2012,Antoniadisetal.'13) MassiveBrans-Dicke Vector-tensorgravity Einstein-Æther Hořavagravity PSRJ (Alsingetal.2012) Variousbinarypulsars (Yagietal.2014) TeVeS&TeVeS-liketheories Bekenstein'sTeVeS TeVeS-like DoublePulsar (Krameretal.inprep,Wexetal.,inprep) PSRJ (Freireetal.2012) FundamentalPhysicsinRadioAstronomy Max-Planck-Ins3tutfürRadioastronomie
27 Bekenstein s TeVeS and the Double Pulsar It'doesn't'pass.' Scalar-vector-tensor theory with aquadratic kinetic term and disformal coupling Scalar coupling strength [ Kramer et al., in prep.; Wex, Esposito-Farèse et al., in prep. ]
28 Dipolar'Gravita$onal'Radia$on'in'Binary'Systems?' UnlikeGR,mostalterna3vetheoriesofgravity includingtensor-scalartheories predictdipoleradia3onthatdominatestheenergylossoftheorbitaldynamics: Hence,visibleinorbitaldecay: + P quadrupole b / P dipole b / = 0 in GR v c 5 v c 3 ( A B ) 2 B{ ~ 0 in Double Pulsar since A
29 Dipolar'Gravita$onal'Radia$on'in'Binary'Systems?' UnlikeGR,mostalterna3vetheoriesofgravity includingtensor-scalartheories predict otherradia3onmul3polesthatdominatetheenergylossoftheorbitaldynamcis(1.5pn): A B Fordifferentbodies,measurableasorbitaldecayfromdipolarradia3on: P dipole b = 4 2 P b Gm A m B c 3 (m A + m B ) 1+e 2 /2 (1 e 2 ) 5/2 ( A B ) 2 PSR-BHsystemwouldbebestasBHwouldhavezeroscalarcharge ButPSR WDsystemalsoeffec3velab inpar3cularifpsrismassive
30 Next'best'thing:''a'PSRTWD'system' PSRJ :firstmassiveNSinrela3vis3corbit(Lynchetal.2013) CombiningVLT,Effelsberg,Arecibo&GBTdata,newrecordmassmeasured: Optical spectroscopy PSR J M=2.01±0.04M (Antoniadisetal.,2013) " 28 PSR J Optical spectroscopy R = ± 0.13 Figure 1.1: Finding chart for PSR J from the SDSS navigate online tool H P Pb e = = (5) ms (2) h 10 6 = = (5) ms (2) h 10 6 H Effelsberg H P Pb e H R = ± 0.13 H H [ Boyles et al. 2013, Lynch et al ] ± M [ Boyles et al. 2013, Lynch et al ]
31 Tes$ng'a'new'gravity'regime' PSRJ :firstmassiveNSinrela3vis3corbit(Lynchetal.2013) CombiningVLT,Effelsberg,Arecibo&GBTdata,newrecordmassmeasured: M=2.01±0.04M " (Antoniadisetal.,2013) ImportantforprobingdifferentgravfieldsbutalsoforEoSofsuper-densemaIer Combinewith moment-of-iner3a fromdoublepulsar. Aretheyborn massive? Seeearlier...
32 Next'best'thing:''a'PSRTWD'system' PSRJ :firstmassiveNSinrela3vis3corbit(Lynchetal.2013) CombiningVLT,Effelsberg,Arecibo&GBTdata,newrecordmassmeasured: M=2.01±0.04M " (Antoniadisetal.,2013) P b =( 250 ± 9) fs s 1 =7.9 ± 0.3 µs yr 1 No)indica8on)of)dipolar)radia8on) p =1 =) P b = µs/yr GR =) P b = 8.2 µs/yr
33 Limits'on'TensorTscalar'theories' ' LimitsbeIerthansolarsystemlimitsformostoftheparameterspace, e.g.inframeworkbydamour&esposito-farese: LLR Cassini LIGO/VIRGO NS-NS LLR matter 0 ϕ ALLOWED THEORIES LIGO/VIRGO NS-BH B SEP B LISA NS-BH PSR-BH J J J Note: InGR,α 0 andβ 0 =0 Jordan-Fierz-Brans-Dicke: onaxisofβ 0 =0 DoublePulsarclosesthe gap le\bypsr-wdsystems s and strong-field scalar-tensor gravity Heraeus Seminar 10 FigurebyEsposito-Farese GR (α 0 =β 0 =0) 0 matter ϕ ϕ Gilles Esposito-Farese, IAP, C
34 Constraining'tensorTscalar'gravity Kramer(2016) matter perihelion shift α 0 ϕ LLR VLBI Cassini LLR (weakfield) General Relativity m (strongfield) GR (α 0 =β 0 =0)
35 The'new'"most'rela$vis$c'binary"...' NewdiscoveryfromHTRU-SLow-lat(Cameron,Ngetal.inprep.) Anew4.4-hbinaryatabout6kpcdistance: P 0 =21.5ms P b =0.184d x=2.24lt-s e=0.61() dω/dt=10.38deg/yr max.acc>600m/s 2 M tot =2.74M ",M c >1.39M " Expected: γ=3.58ms dp b /dt=5.3x10-12 s/s Ω precess =3.1deg/yr Merger<80Myr record Inclination angle (deg) Pulsar Mass (Msol) Effelsberg
36 The'new'"most'rela$vis$c'binary"...' Largestorbitalprecession/orbit&largestGWluminosity Discovery Now
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