School of Physics and Astronomy - 京都大学 · Noemie Globus & Amir Levinson Modeling the...

NoemieGlobus&AmirLevinson

Modelingthecentralengineofrelativisticjets‐applicationtoGRBsoutflows

SchoolofPhysicsandAstronomy

ConferenceonGamma‐RayBurstsNov.11‐Nov.15,2013KyotoUniversity

A.LevinsonandN.Globus,ApJ770,159(2013)N.GlobusandA.Levinson,Phys.Rev.D,88,084046(2013)


RotaGngblackhole

Thedoubleflowstructureofablackholemagnetosphere

GRBs:energydeposiGonbyνν→e‐e+


RotaGngblackhole


stagnaGonup=0

TheposiGonofthestagnaGonsurfacedependsontheenergyinjecGonrate(Levinson&Globus2013)


RotaGngblackhole


GRBs:energydeposiGonbyνν→e‐e+

Zalamea&Beloborodov2011


Alfvénsurfaceoftheinflowinsidetheergoregion

BlandfordZnajekactivated:energyfluxalongmagneticfieldlines

ωH>ΩF>0

RotaGngblackhole+magneGcfield(B~1015G)

CondiGons1)2)


3)Loading?Takahashi+1990


LoadedGRMHDflows

• staGonary+axi‐symmetricMHD• massandenergyinjecGonincluded sourceterms:parGcleqn;energy‐momentumqα

• split‐monopolegeometryinvoked

StreamfuncGon(magneGcflux):Ψ(r,θ)(assumed)

ConstantsofmoGonalongagivenstreamline(qn=qα=0)

‐  angularvelocity:Ω(afreeparameter)‐  parGclefluxperunitBflux:η‐specificenergy(perbaryon):ε‐specificangularmomentum:L‐specificentropy:s

Levinson, 2006; Globus & Levinson, 2013


rst energyflux

neutrinoheaGng

B! (rst ) ! 0

ergosphere

accre+ondisk

rst oudlow

inflow

blackhole

BZac+vated

energyflux

a>0

energyflux

accre+ondisk

energyflux

hea+ng

rst oudlow

inflow

blackhole

B! (rst ) = 0

0<a<1

oudlow

inflow

rst oudlow

inflow

a>0

0< a<1

rst

TYPEIIpoweredbyexternalsource

TYPEIpoweredbyblackhole

energyfluxonhorizon:εr ηε

εH<0⇒εr>0(extracGon)(inflow:η<0)

!


rst energyflux

neutrinoheaGng

B! (rst ) ! 0

ergosphere

accre+ondisk

rst oudlow

inflow

blackhole

BZac+vated

energyflux

a>0

energyflux

accre+ondisk

energyflux

hea+ng

rst oudlow

inflow

blackhole

B! (rst ) = 0

0<a<1

oudlow

inflow

rst oudlow

inflow

a>0

0< a<1



rst plasmaload


LoadedGRMHDflows

• staGonary+axi‐symmetricMHD• massandenergyinjecGonincluded sourceterms:parGcleqn;energy‐momentumqα

• split‐monopolegeometryinvoked

Loading:

1

!g"r

!g! r( ) = !qt

EnergydeposiGon

qn(r) = q

n0!(r ! r

st)

ParGcledeposiGon

qt(r) = q

t0!(r ! r

st)

adiabaGc(εisconserved)

qt (r) = f (r) (εnotcst)

(ηisconservedalongfieldlines)

Levinson, 2006; Globus & Levinson, 2013

εr = ρur ε energyflux

Assump+onssta+onnarityaxisymmetryidealMHD

Splitmonopolegeometry


LoadedMHDflowsinKerrgeometryExample:coldadiabaticcase

TYPEI

eachdiamond=aninflowsolutionthatcrossesalltheMHDcriticalpointsandforwhichrotationalenergyisextractedfromtheBH

Globus & Levinson, 2013

BZresult




2

2

11 aa

c−+

∝η

BZresult


TYPEI

criGcalloading:η > ηc for

BZisshut‐down!

spindependance





θη 2sin∝c

TYPEI

angulardependance


rst energyflux

neutrinoheaGng

B! (rst ) ! 0

ergosphere

accre+ondisk

rst oudlow

inflow

blackhole

BZac+vated

energyflux

a>0

energyflux

accre+ondisk

energyflux

hea+ng

rst oudlow

inflow

blackhole

B! (rst ) = 0

0<a<1

oudlow

inflow

rst oudlow

inflow

a>0

0< a<1

rst




DoubletransonicflowinSchwarzschildgeometryLevinson & Globus, 2013

a=L=0

TYPEII

outersonicline

Innersonicline

• poweredbyneutrinosource

• fracGonofinjectedenergythatemergesatinfinity>0.5

• highspecificentropy

soluGonswitharealisGcenergyinjecGonprofile::neutrinoannihilaGonratesfromZalamea&Beloborodov2011

cHctc2c )p3m4(r)q(r3 −±=−

Sonicpoints

!Q0

!qt (r) =!Q0r!b


rst energyflux

neutrinoheaGng

B! (rst ) ! 0

ergosphere

accre+ondisk

rst oudlow

inflow

blackhole

BZac+vated

energyflux

a>0

energyflux

accre+ondisk

energyflux

hea+ng

rst oudlow

inflow

blackhole

B! (rst ) = 0

0<a<1

η < ηc εH < 0

oudlow

inflow

rst oudlow

inflow

a>0

0< a<1

rst

η > ηc εH > 0



Loading


rst energyflux

neutrinoheaGng

B! (rst ) ! 0

ergosphere

accre+ondisk

rst oudlow

inflow

blackhole

BZac+vated

energyflux

a>0

energyflux

accre+ondisk

energyflux

hea+ng

rst oudlow

inflow

blackhole

B! (rst ) = 0

0<a<1

η < ηc εH < 0

oudlow

inflow

rst oudlow

inflow

a>0

0< a<1

rst

η > ηc εH > 0

TYPEIIdrivenbyneutrinoannihilaGon


!E!! < PBZ

! !macc< 0.1

MH

3M"

#

$%

&

'(

)2/9

*B

1027

G cm2

#

$%

&

'(

8/9

F(a) M".s)1

if

Otherwise:

GRBcase:

νν→e‐e+

Toconclude...

(bothBZandpressuredrivenjetscurrentlyunderinvesGgaGon)


BACK‐UP

EnergysourceforGRBsrelativisticwinds

...Fromtheaccretiondisk?

•NeutrinodominatedaccreGonflowsarecandidatestobethecentralengineofGRBoudlows.⇒  DerivaGon of disk structure and neutrino annihilaGon rates: Popham et al. 1999, Zalamea &

Beloborodov2011(calculaGonsintheKerrspaceGme)

•Levinson,2006:Loaded(i.e.nonadiabaGc)relaGvisGcMHDwindintheSchwarzschildspaceGme.


…Fromtheblackholepolarregion?

•PlasmainjecGoninthemagnetosphere:νν→e+e‐inGRBs(thebaryoniccomponentfromthediskcanbeneglected)•TheenergysourceistherotaGonalenergyoftheblackhole⇒  PioneeringworkofBlandford&Znajek1977⇒  Manysemi‐analyGcstudiesandnumericalsimulaGonssupportthisscenario(Takahashietal.1990,

Komissarov2004,Barkov&Komissarov2008..)•TheenergysourceisneutrinoannihilaGon(neutrinosareemimedfromtheaccreGondisk)⇒  SoluGons for the double‐flow structure in the Schwarzschild geometry : pressure‐driven winds

(Jaroszynski,1996;Levinson&Globus2013)

(thistalk)


LoadedMHDflowsinKerrgeometryExample:hotcase

TYPEII



w=specificenthalpy h=w/ρ≈4p/ρ>>1

School of Physics and Astronomy - 京都大学 · Noemie Globus & Amir Levinson Modeling the...

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