Active Galactic Nucleus Jets in the Event Horizon Telescope Era

BH HIGH-POWER
ACCRETION & OUTFLOW
jet
Black hole (BH)
Gas

Accretion disk(c)NASAKen OHSUGA (Univ. of Tsukuba)
T. Kawashima (NAOJ),Y. Asahina, A. Utsumi (Univ. Tsukuba),
H. R. Takahashi(Komazawa Univ.), M. Nomura (Kure TC), S. Mineshige (Kyoto Univ.)Role of Radiation and Magnetic
FieldsEnergyMatterRadiation Energy
Outflow is launchedfrom the diskmagnetic
dissipation
and/orturbulence

Grav. Thermalenergy energy
accretion disk

Gas
Black holeMRIturbulenceThree Accretion Modes22

1/2 ページ = 左右 80 ミリ × 天地 70 ミリ
1/2 ページ = 左右 80 ミリ × 天地 70 ミリ

Accretion rate/BH mass
(disk luminosity/Edd. luminosity)

Shakura & Sunyaev 73; Ichimaru 77; Abramowicz+ 88; Narayan & Yi 94;

降
着率
降着率

ブラックホール

スリム円盤

ブラックホール

スリム円盤Black hole

Super-Edd.

Hot/Dense

エディントン限界

エディントン限界

Standard disk

標準円盤Cold/Dense

標準円盤

Optically-thick& geometrically-thickEddington limit

Optically-thick &geometrically-thin

ライアフ

ライアフ

RIAF

Hot/
Rarefied

Optically-thin& geometrically-thickAccretion disks are divided into three modes by depending on theaccretion rate (disk luminosity)

Three Accretion Modes
Spectra (schematic)
radiative flux

Different spectral states
imply the existence ofdifferent accretion modes

(a)
(b)

frequency

Mass accretion rate
(disk luminosity)

Temperature(10Msun)Optical thickness(c)(a)Slim disk(b)Standard disk(c)RIAF/ADAF~108K~106-7K

109K

thickthickthin

BH mass vs Accretion rate
Accretion rate/BH mass

Slim disk (supre-Edd. disk)
NLS1

ULX
XRB
(HS-state)

XRB(LH-state)

Stellar Mass BHStandard disk SyRIAF

BH mass

quasar

LLAGN(M87, SgrA*)
Supermassive BH(c)KawashimaAccretion rate/BH mass

BH mass vs Accretion rate
BZ jetRadiatively-driven
jet
NLS1
ULX

XRB
(HS-state)disk windSy

XRB(LH-state)quasarMagnetically-driven Jet

Stellar Mass BH

LLAGN(M87, SgrA*)

BH mass

Supermassive BH
Modified version of Kawashima-san’s slikde

Radiation-MHD
Simulations

here

Magnet Fields;(1)Angular momentum is transported by the Magneto rotational
instability (MRI), leading to the mass accretion onto BHs.
(2)Jets are accelerated by the Lorentz force.
Radiation Fields;(1)Disk loses the energy by emitting photons (cooling).
(2)Jets are launched via the Radiation force.
General Relativity;(1)BH gravity is described by General Relativity.
(2)Effect of rotating BHs cannot be treated by Newtonian Mechanics

Basic Equations ofGR Radiation-MHD

MHD

mass cons.
Gauss’s law

Gas-Radiationinteraction

Induction eq.
energy momentum
cons. for MHD
energy momentum
cons. for radiation

RADIATION
We use Kerr-shild metricSuper-Edd. disk & Jets
Gas DensityRadiation
Energy density

BH

Super-Edd. disk & Jets
BH

Accretion disk

Magnetic
field line

Lrad (>Lkin) ≥ LEdd
Mdot ~ a few 100LEdd/c2
Takahashi, Ohsuga et al. 2016see also Sadowski et al. 2014, Jiang et al. 2014

Super-Edd. disk& radiatively-driven jets
Mass density
Radiation

Accretion
FlowJets

Strong radiation pressure
supports the thick disk andgenerates the jets.

Photons mainly escape throughthe region around the rotation
axis, so that the radiationpressure cannot prevent theaccreting motion.

Radiatively Driven Jet
Acceleration via Radiation Flux Force
Force (z-component)

Takahashi & Ohsuga 2014

No acceleration because ofFlux Force ~ Drag Force
Takeuchi, Ohsuga, Mineshige. 2010

1010 01

40302

001

R/r
S

Apparent Luminosity
010c gre[ )0E(goL )g(6151

41

31

21

10203040050

10203040050

102030

r/RS

r/RS

r/RS

(g) Log(E0) [erg cm-3](h) Log[E0/(e+B2/8π)](i) Log(Tgas/Trad)

12131415

1617080 08

123-180

12350

4580

The radiative flux is mildly collimated70
sincethe disk is optically 70andgeometricallythick.
6060

Radiative
Flux

70 07

04060 0650
Thus
observed luminosity50 is veryr.
40 04
40
sensitive
to the observer’s
40 viewing angle.
osphere, at which the optical thickness measured from the upper boundary is unity. The arrow in panel (g) shows

z/RS

R/z

z/RS

Sz/RS

50 05

Fig. 5.— Two-dimensional distribution of
the gas temperature, (c) the plasma-β, (d) tcomponent, (f) the magnetic pitch, (g) the renergies, (i) and the ratio of the gas tempera
and black arrows in panel (a) indicate the velo
photosphere, at which the optical thickness mvector.

lack arrows in panel (a) indicate the velocity vectors whose magnitude exceed the escape velocity. The dashed line
3 the gas temperature to the30radiation temperature. All values
30 0of30 are time-averaged over t =ies, (i) and the ratio
The apparent
luminosity
becomeshighlyonent, (f) the magnetic pitch, (g) the radiation energy,(h) the ratioof the radiationenergy to
the sum of theas temperature, (c)componentof field, (e) the same b02 plasma-β, (d) the magnetic
20 the20 energies via the toroidal
20super-Eddington
fortheface-on. 5.— Two-dimensional distribution of the various quantities for Model A: (a) the density overlaid with the veobservers(22L
in the case
Edd for ≲20°
10 01
1010S
S
r/RS
r/R
r/R
10 ). 203040
501020304050102030 Edd40of Mdot~100L/c2, L50disk~3LEddr/RS

30

20

1003

02

0104000102030

4050

00102030

40

5000102030

4050

Large luminosity of10 ULXsnoitTwo-dimensional
ubirtsid lanoOhsuga,
isnem
id-oMineshige
wT —.5of 2011
.thegiF various (>10. fo5.—
distribution
quantities
ModelcanA: (a)
theexplained
density overlaid with the ve
39-40forerg/s)
be202020)d( , β-amsalp(c)ehtthe)c(plasma-β,,erutare pm
et thesag magnetic
eht
ast temperature,(d)energies via the toroidal component of field, (e) the same br eht )(f)g( the,hctimagnetic
p citengam
eht (g)) f( ,thetnenradiation
opmoc energy, (h)foronent,pitch,
the ratio
the radiation
the offace-oncase.energy to the sum of ther/RS

10

r/RS

r/RS

20

1010R/rS

are(i)
pmandet satheg ehratio
t f30
o oof
itather ehgast dntemperaturea )i( ,seigrentoe the30radiation temperature. All values
ies,
30 are time-averaged over t =olev arrows
eht etacinidpanelni )a( (a)lenaindicate
p ni swothe
rra velocity
kcalb dnvectors
alackwhose magnitude exceed the escape velocity. The dashed line
30

0504

03

02

R/r
S

01

0041

21203040050

10r/RS

2030

40050

100166810121461630r/RS(e) Log(Bp /8π) [erg cm-3](f) Log(|Bϕ|/Bp)

X-ray spectra8(d) Log(Bϕ /8π) [erg cm ]20r/RS

The Astrophysical2Journal, 752:18(12pp), 2012 June
10-32]3-mc gre[ )π8/2ϕB(goL )d(61108101214

16-0.500.5

4050

Kawashima et al.

11.5

Kawashima et al. 2012

When
the mass accretion rate80 is higher, our calculations80in80 08NGC1313 X-2
this paper show that SEDs become softer, although our previous
7007
paper70 (Kawashimaet al. 2009)70expected that SEDs become
harder because of Compton upscattering by thermal electrons
6060
06
1in the60jet.
Kawashima et al. (2009)
evaluated the photon indicesby calculating
the Compton y-parametersin the region τeff !501.
50
50 05
The effective optical depth is calculated by integrating the4040
40 04 absorption and the scattering
free–freecoefficients from theouter boundary at r = 500rs to the inner boundary at r = 3rs
0.103
along30 therays with polar angle30θ = constant, for various30θ .
(Here,
we note that the computational
domain for radiation
20
2020 02
hydrodynamic simulation in Kawashima et al. 2009 was smaller
IC342 X-1
1001 in this work.) Since 10than 10thatKawashima et al. (2009) did
not take into account the downscattering by cool outflows,
000 01020 when30
40 accretion
50
1020
30
40
50
05
04
03
02 they
01 overestimated
102030the 40spectral
50
hardeningther/RSr/RS
R/rr/RS
1S
rate is high. When the massaccretion rate is higher,a greater]3-mc gre[ )0E(goL )g(Log(E0) [erg cm-3](h) Log[E0/(e+B2/8π)](i) Log(Tgas/Trad)
number of(g)escaping
photons tends to enter
into the cool outflow
71
6151
41312112131415
16170
12
3-10123
4
5
surrounding
the jet and they are80 subsequently downscattered,
80 0880
because the funnel becomes narrower and jet becomes thicker
0.1
70 0770
for Thomson
scatterings. This 70is the reason why the SEDs
become softer when the mass accretion rate is higher, in60 0660
this work.
Nevertheless, the conclusionin Kawashima et 60al.
(2009)
the spectral state changes
from the slim disk one
550 0that5050
NGC5204 X-1
to the Comptonizing outflows is valid in highly supercritical
vector.
40 04 flows because the SED40of the photons escaping from40
accretion
photosphere, at which
the optical
thickness measured from the upper boundary is unity. The arrow in panel (g) shows the radiative flux
suchsupercriticalflows
is whose
determinedby exceed
the Comptonand black arrows inpanelhighly(a) indicate
the velocity
vectors
magnitude
the escape velocity. The dashed line in panel (b) is the3 the gas temperature to the30radiation temperature. All values
30 0of30 are time-averaged over
1 t = 6−7 s. The whiteenergies, (i) and theratio
downscatterings in the outflow.
component, (f) the magnetic pitch, (g) the radiation energy, (h) the ratio of the radiation energy to the sum of the gas and magnetic
z/RS

R/z

z/RS

Sz/RS

X-ray spectra, calculated by the
post-processing radiation transfer,nicely fit the observations (ULXs).

Mdot=103LEdd/c2
viewing angle=10°

hard X-ray is observed sincehigh-energy photons escapethrough the funnelz/RSz/RS

R/z

z/RS

S

hard X-ray is
reduced byCompton down4.3. Comparison with Observationsof ULXs
scattering

200LEdd/c2
10°200LEdd/c2
50°

Fig. 5.— Two-dimensional distribution of the vari
the gas temperature, (c) the plasma-β, (d) the magn
component, (f) the magnetic pitch, (g) the radiationenergies, (i) and the ratio of the gas temperature to t
and black arrows in panel (a) indicate the velocity vec
photosphere, at which the optical thickness measuredvector.

the gas temperature, (c)of field, (e) the same but of the poloidal
02 plasma-β, (d) the magnetic
20 the20 energies via the toroidal component
20Fig. 5.— Two-dimensional distribution of the various quantities for Model A: (a) the density overlaid with the velocity vectors, (b)
10 01

1010S
r/Robservatories
r/RS
Recent 10X-ray(Suzaku,XMM-Newton,
and 10 20 r/RS30 400.1 50
203040501020304050
000Chandra)provideus 40
with50precise
spectraofULXs
below
0 0000504030201
1020301020304050
1020304050R/r10 keV.
InFigure
wecompare
theSEDs
obtainedin
thiswork
r/R7,r/RS
r/RS
SS
101010and the XMM-Newton
pngiFdataof three ULXs: NGC 1313 X-2,irav Fig.
eht fo5.—
noitTwo-dimensional
ubirtsid lanoisnem
id-owT —.5of .thedistribution
various quantities for Model A: (a) the density overlaid with the velocity vectors, (b)0.3 but of the poloidal
1
10X-1,
areprovided
by of field, (e) the same
20ngtheam gaseht temperature,)d( , β-amIC
salp342e20
htthe)c(plasma-β,,erandutareNGCpm
et thes5204
ag magnetic
ehtX-1,20which(c)(d)
energies
viakindly
the toroidal
component
nocomponent,itaidar eht )(f)g( the,hcJ.timagnetic
ptengameht (g))Thef( ,thetnSEDs
enradiation
opmoofc ourpitch,energy,(h) are
the ratioof the radiation
C.ciGladstone.
resultsnormalized
by the energy to the sum of the gas and magnetic
t oenergies,t erutare(i)pmand
et satheg ehratio
t f30
o oof
itather ehgast dntemperaturea )i( ,seigrentoe the30radiation temperature. All values
30 are time-averaged over t = 6−7 s. The white
X-ray
Figure3, while
the SEDs
ULXs
FigureComparisonSEDs
ceandv ytiblack
colev arrows
eht etacin
idpanelni )a(luminosity
lenaindicate
p ni swothe
rshownra velocity
kcalbindnvectorsa(a)whosemagnitude
exceedofthe
escape velocity.
The7.dashedline in ofpanel(b)obtainedis the from our radiation hydrodynamic
simulations
withshowsthosetheof ULXs.
Topflux
panel: the SED for the simulation model
dephotosphere,
rusaem ssenkatcihwhicht arelacitpo eopticalht hcihw
tby
a ,ertheehp
sX-rayotohp luminosity
thethickness
measuredfrom the upperboundaryis unity. The arrowin panel (g)radiativenormalized
shown
in Gladstone0(data; Gladstone 2009)

r/RS

10

1020zzz

30z

20

30

4050

Effect of BH spin
Disk luminosity and jet power might
depend on the BH spin. We perform
simulations of the super-Eddington
flows around BHs with a=0.9, 0, -0.9.

Non-Rotating BH; a=0*a: spin parameter
Rotating BH; a=0.9

Rotating BH; a=-0.9(c)NASAEffect of BH spin
Radiativelydriven jetSuper-Edd.
diskBH

BH (a*=0)

Mdot(BH) ~ 410LEdd/c2
Lrad ~ 8LEdd → ηrad ~ 2.0%
Lkin ~ 5.6LEdd → ηkin ~ 1.4%

Preliminary
Utsumi et al. in prep.

Disk rotation⬅ISCO(a=0.9)

ISCO
(a=0)
⬇

Preliminary
Utsumi et al. in prep.

ISCO(a=-0.9)⬇

Rotation velocity
goes down within
the ISCO radius.

Disk rotates with
Keplerian velocity
at the region ofr > ISCO raidus

Counter rotation within the ergospherePreliminaryLorentz factor

Utsumi et al. in prep.

Jet region

Jet region

2.0z/rg

Jet region

Jet velocity (Lorentz factor)
is larger for rotating BH thanfor non-rotating BH.
50

1.50Rotating BH(a=0.9)0r/rg

30

Rotating BH(a=-0.9)

non-Rotating
BH
0r/rg

300r/rg30

1.0Preliminary

BH spin & Jets

Utsumi et al. in prep.

Rad. Conversion
Lrad vs Lkin
Efficiency
Lrad/(Mdot c2)

Jet Conversion
Efficiency
Lkin/(Mdot c2)

a=0.9

Lrad < Lkin

6%

11%

a=0

Lrad > Lkin

2%

1.4%

a=-0.9Lrad < Lkin

3%5%

BH spin drives powerful jet ?
See Utsumi-kun’s POSTER for details.

BH spin & Jets

Preliminary
Utsumi et al. in prep.

Outward Poynting Flux
Rotating BH(a=0.9)non-Rotating Rotating BH
BH(a=-0.9)

Outward Poynting flux, which is driven by
BZ effect, is enhanced for rotating BH.

Wind Outflows from Super-Edd. Disks

Jet

Super-Eddington disk+ Jet

Takeuchi, Ohsuga, Mineshige 2013

accretion

ClumpyOutflow

Time-dependent, Clumpy outflow
with wide angle

RT instability

Clumpy outflows (3D)
Kobayashi+18

OowlftuTorn sheet like structure.
The size is ~100Rs.
Outflow velocity is ~0.1c.
Rotation velocity is 30% of Vkep.

Black Hole~1000RsSheet like structure
Outflow velocity ~ 0.1-0.2c
Size (azimuthal direction) ~ 100Rs
Rotation velocity ~ 30% of Vkep

Absorption lines
Outflow velocity of~0.1-0.2c agrees with theobservations ofblueshifted absorption
lines.
Pinto+16,see also Kosec+18

Sheet like structure
Outflow velocity ~ 0.1-0.2cSize (azimuthal direction) ~ 100Rs
Rotation velocity ~ 30% of Vkep
Time variation
Timescale of the luminosity
variation (100Rs/0.3Vkep) is

Our result is consistent withthe observations of ULXs
(Middleton+11) and V404 Cyg(Motta+17) in the case ofMBH~10-100Msun.

Clumpy outflows
Some ULXs exhibit the time
variations of X-ray luminosity,
implying the launching of clumpy
outflows.

Middleton+11

Launching of clumpy winds isalso reported by observationsof NLS1s or V404 Cyg.

Jin+17 see also Motta+17

Simulations of near-Edd. disk
Igarashi et al. in prep.
See Igarashi-san’s POSTER

hereJiang et al. 2019
Sadowsiki et al. 2016

Simulations of line-winds
Nomura et al. 2016(see also Proga et al. 00, 04)

BH(108Msun)
Line winds

Standard disk

Funnel-shaped disk winds(~0.1c) are ejected at theregion of 100Rg.

Spectra (line)
Simulated absorption line
by MONACO code(c)Mizumoto

consistentLine-winds would be origin
of UFOs, which is detectedin some of Sy galaxies.

Observed line feature

Tombesi et al. 2011

Outflow rate/Eddington rate

Spectra (Continuum)
Nomura et al. submitted

·MBH

0.8

Accretion rate isreduced by about half.

0.4

Spectra

000.5

1.0

Accretion rate/Eddington rate

High-energy parts arereduced by the reductionof the accretion rate.

·Mout·MsupSummarysuper-Eddington Flows• Radiatively-driven jets are launched from the super-Eddington
disks.

• Jet power (and disk luminosity) is enhanced by the BH spin.
Probably this is due to the BZ effect.

• Disk winds from the super-Edd. disks fragment into many gas
clouds via the RT instability.

near-Eddington Flows• Line-winds ejected from the disks would be origin of UFOs.
• Simulations of Jets from the near-Eddington disk are left as futureworks.

Important Keyword “3”We need three steps in order to reveal BH.
Collaboration between observations and theory is important.
Theory/Model
Hydrodynamics
Simulations

Radiation
Transfer Calc.

Observations

Accretion rate

We should understandBH spin

BH massBHs in 3D-space (Mass,Accretion rate, Spin).