MAD in Action in M87
Masanori Nakamura (ASIAA)
J. Park (ASIAA), Y. Cui, K. Hada (NAOJ), M. Kino (Kogakuin U./NAOJ), K. Toma (Tohoku U.),
T. Kawashima (NAOJ), J.-Y. Kim (MPIfR), B. W. Sohn, T. Jung, S.-S. Lee (KASI),
and EAVN AGN SWG
AGN Jet Workshop 2020, Jan. 20 - 22, Tohoku U., Sendai

Outline• “VLBI study of AGN Jets” during the last decade• Lesson from M87 to others: Acc. & Colli. zone (ACZ:

Marscher+ 2008) as “Pipeline” (Marscher & Gear 1985)
and Jet Collimation Break (JCB: Asada & MN 2012),

providing a physical extent of ACZ (Park’s talk)• Thrilling results with EHT, but the horizon-scale jetin M87 is still unknown (or has no strong constraints)• Any unique usage of EAVN facilities to understandthe fundamental physics in AGN jets?
01/20/2020, Sendai

Blandford & Payne (1982)➡BP82 (disk-driven) wind may NOT
produce limb-brightened features,
while BZ77 does play a role
(Takahashi, Toma+ 2018; MN+ 2018)➡Revisiting spine-sheath hypothesis• Blandford & Begelman (1999)➡ADIOS as a confining material

ACZ & JCB in a FSRQ: See, Lee (SNU)’s talk

et
lj
0∘
.2
)
j =

,θ
60

z∝ R

=
(Γ
2
0.

a
P

i
l
o
b
ra

t
e
j
c

=

• Blandford & Königl (1979)➡Revisiting “conical” jet model• Blandford & Znajek (1977)

onicaM∙ = 2 × 109 M⊙ (N315)

86GHz

M∙ = 6 × 108 M⊙ (N6251)

RC
S/
C

M∙ = 6.2 × 10 M⊙ (M87)

Γθ

]

9

230GHzM87 + NGC 6251 + NGC 315+ FSRQs + BLOs
1633+382• Nearby
1928+738or
2201+315• Massive MBH
Mrk 501
or
Mrk 421• Large θv
3C 371230GHzGlobal Structure of AGN Jets: ACZ + JCB

1.6

Mrk 501 coresz∝ R

1633+ cores(Algaba, MN+ 2017)(Koyama+ 2016)

M87 cores(Hada+ 2011, 2013;
MN & Asada 2013)
Tseng+ (2016); MN+ (2018); Park+, in prep.

MN+ in prep.

• BH mass:
SANE, Rhigh = 80, a* = − 0.94

SANE, Rhigh = 10, a* = 0

MAD, Rhigh = 10, a* = 0.94

M∙ = (6.5 ± 0.7) × 10 M⊙
9• Mass accretion rate:

· ·
−7
−4
·
m (≡ M/ MEdd) ≃ 5 × 10 − 3 × 10

• Jet power:
42
−1

10

50 μasfrom paper I (EHTC 2019a)• Synthesized emission: the funnel wall and/or

accretion flow with σ < 1: Γ∞ → 1

σ: Poynting flux per unit matter energy flux

• Connection with the extended jet (relativistic

outflow: Γ∞ ≫ 1) is unknown

erg s

43

< Pjet ( ≲ 10−1

erg s )

• BH spin (a=0 can’t do >1042 erg/s ):| a | ≤ 0.94

• Magnetic flux:

ϕ = 3.6 − 56.5 (units of
SANE

MAD

· 2
MRg c)• Electron temperature:

Te ≃ Ti /(10 − 160)

EHT Collaboration

PA43GHz ∼ 288∘ (Walker + 2018)

EAVN Collaboration• PAGRMHD (forward jet):
∘±
∘

235

65 (Apr 5 − 11)

01/20/2020, Sendai

Magnetically Arrested Disk (MAD)•A.
Tchekhovskoy
Poloidal magnetic

field supports the accreting gas
against the BH gravity (Narayan+ 2003; Igmenshchev 2008)
2
Bp

GM ⇢
2
'
= ⇢c
8⇡
Rg

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'

q

10

2
Ṁ Rg c

33

1/2

ṁ

3/2
2
m9 Mx (G cm )ṁ . 0.01 (RGs, BL Lacs)<latexit sha1_base64="Of92/zcaqTtK51+g3Msfi6t1cNg=">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</latexit>• GRMHD Simulations:ϕ < 10 (SANE), ϕ ∼ 40 − 80 (MAD) (Narayan+ 2012; Sadowski+ 2013)•
MAD in observations:Image
courtesy:A.
Tchekhovskoy
ertical slice through BH accretion system illustrates how theSupportingbalance of forces

31
35
he maximum possible field strength on the BH. The BH, shownΦ
as a =black
circle,is10 − 10 Mx (Zamaninsab+ 2014)jeth vertical magnetic field, whose lines of force are shown with blue lines. The magnetic
ce, FB , pushes outward on the accretion disk gas, which is shown in red. Clearly,
ed the disk, the magnetic field would leave the BH due to the “no-hair theorem”,· 2 (Ghisellini+ 2014)
Pjet ≳ Mc
01/20/2020, Sendai

41
10

0

Efficiency: η (%)

300

· 2
Pjet0.8> Mc
0.2 MAD0.4Can Make
0.6
a

MAD
SANE

200

1

EM energy extraction from a spinning BH (Blandford & Znajek 1977)

PBZ(Φ, a)
η=
×
100
· 2
Mc

ϕ = 60100
ηmax for thin disk (a=0.998)

0

0

0.2

0.4

ϕ = 10
a

0.6

0.8

1
01/20/2020, Sendai

Motivations
Asynchronous activity

from paper V (EHTC 2019e)• Current jet power needs be examined with further inner regions (mm/cm VLBI)
01/20/2020, Sendai

10
1037
8
10

10

10

10

12

14

10

16

10

ν [Hz]

10

18

10

20

10

22

10

24

Motivations

at i = 20◦ and i = 90◦ based on models RH1-RH100 overplotted with theemission appears in the SED as a hump around 230 GHz, and the higher ordern.Evolution of the intensity profile across (left panel) and along (right panel) the jet at λ = 7 mm (ν = 43 GHz). Color lines represent intensity

ous times spaced by 20M ≡ 7 days.

Two-temperature MAD simulations of M87

A&A proofs: manuscript no. main

2887

A&A proofs: manuscript no. main

Fig. 7. From left to right: 43, 86, and 228 GHz. Top row: synth
Second row: same as top row but for the ✏ = 0.0 -jet. Bottom roContour maps of the model images (RH100) at λ = 7 mm (ν = 43 GHz) for viewing angles of i = 20◦ (left panel) and i = 160◦ (rightconvolved with the telescope beam to simulate observations by Hada et al. (2011). The contour levels were chosen to match those fromations (contours decrease by a factor of ◦21/2 from the maximum intensity).
The image size here is 480 × 480GMBH /c2 ≡ 1.8 × 1.8 mas,◦
43about
GHz)twice
for atheviewingangle
of i 4= (images
20 (leftatpanel)and i = 160 (right panel).
issize usedin Fig.
λ = 7 mm).
j

SANE: Moscibrodzka+ (2016)

Downloaded from https://academic.oup.com/mnras/article-abstract/486

P = (4 − 30) × 1042 erg s− 1uxes in units of Jansky for each model (Col. 7). The position angle of the jetboth models. The size of each panel is 200 × 200 GMBH /c2 in the plane of thengular size of about 0.8 × 0.8 mas.
tness assymetry is due to Doppler boosting. In both cases
A robust comparison of Fig. 4 to observations of the sourcen in Fig. 4, the emission from the counter-jet is strongly at 7 mm is presented in Hada et al. (2011). In Fig. 6, we convolve
essed.
our theoretical intensity maps (Fig. 4) with the telescope beamrge 3.2. Emission at λ = 7 mm and 3.5 mm= 0.3 and 0.14 mas, see Hada et al. 2011) andsize (FWHM
hejetedge-brightening of the jet images is illustrated in Fig. 5 contour them beamin the same fashion as Fig. 3b in Hada et al. (2011).
panel),
which shows the radiation intensity profile acrosslo- Figure
4 shows
the appearanceof our2
There RH100
is overall good qualitative agreement, but also some ret axis at a distanceof 25GMfromthe fiducial
SMBH. model
BH /c away◦◦
ons at λ = 7 mm for i = 20 (left panel) and i = maining
160 (rightdiﬀerences. Our jet model is somewhat more compact
e 5 (left panel) shows how the intensity profile evolves inon).
the thedirection
panel).
The images
show thedistributions
sky along the jet axis to account for the extended
Lines with
diﬀerent
colors indicate
the intensity
intensity profile
at in onFig. 7. From left to right: 43, 86, and 228 GHz. Top row: synthetic images at a single
43snapshot −of1thebrightness jet features observed at 7 mm. Also ourthatThearetimenormalized
to unity.
computedthe GRMHD
usantimes.
span between
theThey
blackareandmagentaon low-surface
43GHz
imaging
with
SANE:
Davelaar+(2019)
jthe first and modelFig.when
10. conFirst panel from the left: 43 GHz radio map of M 87 (Janssen
et al.same2019).
panel:
map
ofsamethe asthermal-jet, butSecond row:
as topSecond
row but forthe ✏ =synchrotron
0.0 -jet. Bottomrow:second row
ac- modeltosnapshot
model does
thentime-averaged
over jeta durationof not display the characteristic two rims
corresponds
about 28 based. Theandratioof theintensity of thethe telescope beam, even though the underlying
yms
at is about
convolvedthe-with a 2D Gaussian beam. Third panel: same as the second panel but now for a -jet model with ✏ = 0.0. Fourth panel: Same as theabouttwo
35 d.
mm, theplasmaaroundthe maximumof theandAtis 7roughly
constant
in time.
Figure5 volved withoretical model
betteragree-but now with ✏ = 0.015. The white ellipse indicates the beam used to convolve the images. All models produce a jet that is too narrowredpanel)intensity
also showsthe evolution
intensitythickprofile(thealongdistribution
is of
optically
synchrotron
pho- is clearly edge-brightened. An even
third
panel
mentofbetween
probably bet. The tosphere,
profile along
twoisintensity
τabsthe= jet1 showssurface,locatedenhanceat a distanceabout our model and observations could
comparedto the VLBI map. The extent of the jet increases when electron acceleration is present, and✏ = 0.015.
Fig.is8.maximum
Logarithmicfor
optical-depth
maps at 228 GHz of a single s
achieved (1) by using GRMHD models with a higher spatial res2
thatapparently
move
upstreamofthejet(“knots”
locateding 10− 25 GMBH /c
from
the
BH).
The
imagesdisplayextended◦ apparent
olutionthat resolves
jetmeasured
boundary(2019)better;(2) by opening
increasing
the The leftmost panel shows an
13.andLog-scale
imagesof find
86 GHzofthe twomodelsoverlaid
withthethe55
angle.
86GHz
imagingwith
MAD:
Chael+∼re 4565GM/c2 ).
We
that
these
intensity
BH
with
and
complexstructures
thatsnapshots
are two
evidently
edge-brightened.
sizetheof GMVA
the computational
we areonlys”
haveMoreover,subluminal
apparent
speedsof v/c =asymmetry
0.13
and data
0.4,
eall
reconstruction
using
the
algorithm
on 2014
fromreported indomain
Kim et sinceal. (2018).
The
topsimulating
row shows the high-resolution GRTRANS
there
is CLEAN
thebrightness
betweenthe
two
Article number, page 10 of 15
theinnermost
parts
of
the
jet
at
43
GHz;
and
(3)
by
includinghsed
jetacceleration.
withapower-law.
Theresultsaresimilartotheones
presented
loop
increasesthemagnetic
flux at the horizon at later times.
esindicateof thetwosimulations
at
86
GHz
(zoomed-out
versions
of
the
86
GHz
images
in
Fig.
10).
The
bottom
row
shows
the
simulation
imagesconvolved
rims on both sides of the jet. The jet is corotating with the BH• NoneP ∼ 10erg sof models (SANE/MAD, (non-)Thermal eDF) canreproduce the morphology; Limb-brightened (L-B) feature• Punsly (2019) argue both SANE and MAD jets (M16, C19)
42
−
1
the
beam reported in Kim et al. (2018). The snapshot images were normalized to the total flux of2014 simage.
simulations
erg
bytheDexter
et al.Both(2012),
whoproduce
also injected accelerated electrons These stronger magnetic fields will a↵ect the overall source moris 6Gaussian
page
ofand
15 the disk. (The angular momentum vector of the BH, and Pj = (6.6 − 13.0) × 10
opening
at 86 GHz
counterjet
emission,
simulation
imagesis somewhat
less than magneticthan
theangle
disk jets
is pointing
in andthe noticeable
N-W directionin theimages.)although
The the limb brightening in the blurredarenarrowerjet phology,
at 43/86GHz(Hada+
2013,
based
on theamountof available
energy. realThe -jetresulting in wider
opening angles
which2016)lead to lesshe 86 GHz CLEAN reconstruction.

A38, page 5 of 15

T’s resolution. The brightest spot in the 230 GHz image moves
the rotation of the magnetic field lines, particularly in the H10models yield a jet power of the order of 1043 ergs s 1 , which is in obscuration of the shadow by the forward jet.
agreement with observations of the jet core power by Reynolds
though the bright ∼ 40 µas photon ring remains the most prominent
SendaiFig. 7. Fromleft
to right:
43, 86,thanand 228GHz. Top row: synthetic images at a single snapshot of 01/20/2020,
the thermal-jet at an inclinationof i = 16etal.
(1996),
andisapproximately
two
times
lower
the
feature.
Second row: same as top row but for the ✏ = 0.0 -jet.
same
as theandfirst androw but
for the ✏ = 0.015 -jet.
4.4.Bottom
Corerow:size,
shift,
jet second
openingangle

M87
VLBI core obs.
GRMHD sim.

<latexit sha1_base64="/ThWlbwn7VTvD+vfDrMZjBOldBQ=">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</latexit>=q

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01/20/2020, Sendai

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Resolving a jet in the direction transverse to its axis isimportant for understanding the opening angle, collimation
efﬁciency, and possible velocity gradient across the jet. To
perform this, one needs a high-quality image at a sufﬁcientangular resolution across the jet. The new 86 GHz image
presented here allows us to analyze the detailed transverse
structure of the jet-launch region near the black hole.

Quasi-symmetricdistorsion• SSA thick VLBI cores→ |B| (z < 50 rg)

Hada+ (2012, 2016); Kino+ (2014, 2015)
43 230 GHz' (12) ⇥ 10<latexit sha1_base64="j5U/djhzCXGgF9YMs5m4tgI9JBo=">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</latexit>

3.3. Transverse Jet Structure~1000 rg

We don’t know where/how
SL knots are formed…

located with respect to the core, while case (2) is also possible
if we additionally consider the relativistic “arm-length ratio”
that reﬂects apparent motions differing by a factor of ∼2
between the jet and the counter jet.
In the case of (1), when compared using the total ﬂux densities,
the BR is 25.2 at 86 GHz or 5.7 at 43 GHz. In the case of (2), theBR is 22.0 at 86 GHz or 4.4 at 43 GHz. Alternatively, if we use
the peak ﬂux densities, the BR is 25.3/4.7 at 86/43 GHz for case(1), or 21.4/5.6 at 86/43 GHz for case (2).
It is not clear yet whether the resulting difference in BR
between 86 and 43 GHz is real or not. We consider that themeasurements at 43 GHz would be more secure due to the higher
S/N for the counter jet. Conservatively, here we conclude thatthe BR is between ∼5 and ∼25 within the central 1 mas region.

HSA 86GHz (Hada+ 2016)

Figure 8. Close-up view of the innermost region of the M87 jet observed with
VLBA+GBT at 86 GHz. The image is restored with a 0.11 mas circular
Gaussian beam, which is equivalent to that of the minor axis of the synthesized
beam. The image is rotated on the sky by 23n in order to align the jet central
axis to the horizontal direction. For reference, on the origin of the coordinates
we place a green-colored circle with a diameter of 40 μas, which is equivalent
to the size of the 230 GHz core reported by Doeleman et al. (2012). The arrows
indicate where the jet shape is locally shrinking.

Innermost Structure of the M87 Jet

33

2

Mx (G cm )• Enclosed current !I(Φ)
e.g. Mestel (1969); Okamoto (1978);Beskin (1997); Narayan+ (2007)c
I( ) = RB ⇡2<latexit sha1_base64="G4fjqV7pBsANit1cfp9kI0Bu2NM=">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</latexit>' (1.5<latexit sha1_base64="6E3L85MF/WsY8y0pd8D9L8+LQT8=">AAAG2XicjdS9b9NAFADw1wCmlI+msCCxnIiC2oHo3IJaMZXSVrRSpaT5aKW4RLZ7CVb8he0YFcsDG+rCwMDABBIDYmaFgYWBlaF/AmIsEgsDz2cjBKeWuyjxu+f3Oz9fpDN82wojSg/GSidOnlJOj5+ZOHvu/IXJ8tTFTuiNApO1Tc/2gm1DD5ltuawdWZHNtv2A6Y5hsy1jeCe7vxWzILQ8txXt+WzH0Qeu1bdMPcJUrzyjhZbDHpBptXaTXCdzM0SLMBESld5L1PmUaCTRAofcTnvlCq1RPogYqEVQgWLUvanSZ9BgFzwwYQQOMHAhwtgGHUL8dEEFCj7mdiDBXICRxe8zSGEC7QirGFbomB3i7wBn3SLr4jxbM+TaxKfY+A1QEqjSL/QNPaSf6Fv6lf48cq2Er5H1sodXI7fM703uX27++K9y8BrB/T/q2J4j6MMC79XC3n2eyd7CzH386Plh89ZmNblGX9Fv2P9LekA/4hu48XfzdYNtvjimHwN7SaGK6xh8H3Yx+t1dplysesj3yOF5FysSzOfV2W4nxdxBSXgmlZADQQ4k5VCQQ0kZCDKQlLEgY0m5IsgVSbksyGVJuSTIJUm5Lsh1SdkRZEdStgTZkpR1QdYl5Zog1yTlhiA3JGVDkA1JuSrIVUnZF2RfUjYF2cwlnuXqvye3GHRma+pcbbZxo7K4UJzq43AFrsI0ntzzsAh38b9q49Ofwjt4Dx+UrvJYeaLs56WlscJcgr+G8uwXwStq7w==</latexit>⌦F2⇡3) ⇥ 1017 A• Electromagnetic(a = 0.9)(Poynting) luminousity
2

LEM = I z ' (4<latexit sha1_base64="3U7+vVxjC+e+zEfSIScJcJ2nDeo=">AAAG9nicjdRPaxNBFADw16hrrX+a6kXwMhgi9dAwm0YsglBqE0wxkDR/WmiasLudrEv2n7ubaLvsF/ALeBAEhSKiB7+DFw+eBA9Fv4B4rODFg283K2IH60xI9s3b95t9O4FRXdPwA0oPpjInTp6STk+fmTl77vyF2ezcxY7vjDyNtTXHdLxNVfGZadisHRiByTZdjymWarINdXgnvr8xZp5vOHYr2HXZtqXotjEwNCXAVD9budcPu55FyrWI3CbVXliMyB7p+obFHpD50oJ84zrpBjjziUx7YWkxIl2SCObpGPq9cEGOon42Rws0GYQP5DTIQTrqzlzmA3RhBxzQYAQWMLAhwNgEBXz8bIEMFFzMbUOIOQ8jI7nPIIIZtCOsYlihYHaIvzrOttKsjfN4TT/RGj7FxK+HkkCefqKv6CF9T1/Tr/TnP9cKkzXiXnbxqk4sc/uzjy83f/xXWXgN4P4fdWzPAQxgKenVwN7dJBO/hTbx470nh81b6/nwGn1Bv2H/z+kBfYdvYI+/a/sNtv70mH5U7CWCPK6jJvuwg9Hv7mJlY9XDZI+sJG9jRYj5SXW822E6t1CSJBMJSJ2TuqAccnIoKD1OeoJyzMmxoCxzsiwoVzm5KihXOLkiKNc4uSYoO5zsCMoWJ1uCss7JuqCscrIqKGucrAnKBicbgrLCyYqgHHByICibnGxOJJ7l8tGTmw86xYK8WCg2SrnlpfRUn4YrcBXm8eS+CctwF/+rNj79DXyEz/BFeiQ9k/all5PSzFRqLsFfQ3r7C/amdfs=</latexit>—σ=1—βp = 1 — ur = 0 (Stagnation) MN+ (2018)15) ⇥ 10

43

erg s

(z ∼ 160 Ω, a = 0.9)
01/20/2020, Sendai

1

Axisymmetric 2D GRMHD Survey<latexit sha1_base64="m+wdeLJpXqT90m5SUfCAhHbeahY=">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</latexit>

100<latexit sha1_base64="9VKKmTeXDAj9oImLd1Ta9sLYLTM=">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</latexit><latexit sha1_base64="sqhvxvJJTsOtbio13fZ+O3IgvDw=">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</latexit>

a = 0.9

⇡ 70
⇡ 100

φ

<latexit sha1_base64="ia8m6WsCEVpd+TgrDzHYNvB1DDA=">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</latexit>

⇡ 10
⇡ 30

50
0

0

1
4

2000

<latexit sha1_base64="7Ex46p2zOMFGBnslSdJnFByn3oo=">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</latexit>

4000

6000

8000

4
10

a = 0.9

.1

.
M
φ

-1
10

10

2
-2

-3
10

0

0

2000

4000

6000

8000

4
10

t/tgin prep.
MN+
4

01/20/2020, Sendai

Lateral Expansion & Accelerationa = 0.9

SANE

SANE

SANE
MAD

MAD

MAD

--σ=1
— FFE solution(z ~ R1.6)

MN+ in prep.

σ> 1• Bulk acceleration takes place in the funnel where !
• Large !ϕ causes a lateral expansion (effective magnetic nozzle); limb-brightened → MAD?

ϕ = 30 − 70 can be matched with the parabolic shape of !σ ∼ 1 → VLBI obs.?

• !

01/20/2020, Sendai

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210 pc✓kTB
0.9 keV◆ 1✓M•
6.2 ⇥ 109 M

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0.3 cm 3✓◆ 3/2 ✓
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Di Mateo+ (2003); Rafferty+ (2006); Russell+ (2015)· 2
Pjet(= 5 × 10 erg/s)/ Mc ∼ 1

ṀEdd

43

· 2
Pjet ≳ Mc

10-3

A

(2
+
k
Par

X-ray obs.

<latexit sha1_base64="Z//vej3AntBx+FCIjLpOKOY8i2g=">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</latexit>=

136.4 M yr 1◆⇣✏ ⌘ 1 ✓M•
acc
0.1
6.2 ⇥ 109 M

X-ray / Pol. obs.

ne / R 1 (R & 5000 Rs ) : s ' 0.5<latexit sha1_base64="mnhsTKKutq8kKfs/4IWDBpzTlSA=">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</latexit>

10-4

Russell+ (2015) - X-ray
Park+ (2019) - VLBA Pol. (≦ 5 GHz)

To be explored w/ HSA Pol. (≦ 22 GHz, PI: Park)Ṁ (r) = Ṁout

10-5

✓

R
Rout

◆s

Ṁ . 9.2 ⇥ 10 4 M yr 1 (R ' 20 Rs )<latexit sha1_base64="Lp67wpoqGkzWKUDmdgR+MQau4bs=">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</latexit>

Kuo+ (2014) - SMA Pol.

, 0s1e.g., Yuan & Narayan (2014) ARAA

10-6
1

101

102

103
R/Rs

104

Ṁ |R=10 Rs ' 5.3 ⇥ 10 4 M yr 1

105ṁ ' 3.9 ⇥ 10 6<latexit sha1_base64="WrbFlD+KgG9Thi7KoiEeZdQ48Jc=">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</latexit>Ṁ c2 ' 3.0 ⇥ 1043 erg s 1

01/20/2020, Sendai

M87

33

≃ (1 − 2) × 10

VLBI core obs.

Hada+ (2012, 2016);
Kino+ (2014, 2015)

GRMHD sim.
& VLBI obs.
<latexit sha1_base64="/ThWlbwn7VTvD+vfDrMZjBOldBQ=">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</latexit>=q

2
Ṁ Rg c≃ 3 × 1031

≃ 30 − 70
Pol. / X-ray obs.
Russell+ (2015); Park+ (2019)01/20/2020, Sendai

Quasi-simultaneous Monitoring of VLBI Core•

Past efforts w/ KVN 22-129GHz (2012-2016; Kim, Lee+ 2018)• Spectral steeping, but limited (u, v) coverage and/or structure blending?
• True spectrum of the jet base can be flat up to 129 GHz•

Partially SSA-thick at 230GHz? (Kino 2015+)•

Assuming the poloidal flux conservation in the funnel, Φ! EH can be extracted from VLBI core at+ 2011; r ≲ 50 rg)
mm-cm bands !( ≥ 43 GHz) where the SSA-thick core exists (Hada!

Flux density (Jy)Measurement within a 0.5 × 0.5mas2 box around the peak2

EAVN@22GHz, Apr. 17, 2017
EAVN@43GHz, Apr. 18, 2017
KVN@86GHz, Apr. 19, 2017
KVN@129GHz, Apr. 19, 20171

5×10-1
101

2×101

5×101
102
Frequency (GHz)

Data from paper IV (EHTC 2019d)

Measuring core size & flux at ≤! 86 GHz(GMVA+ALMA / EAVN)• Monitoring VLBI core flux at 22-129 GHz(KVN+EAVN hybrid mode)➡ Estimations of Φ
! EH & LEM during EHT2020

•

2×102

GMVA+ALMA 2020 (PI: J. Kim)
submitted to EAVN2020A (PI: Y. Cui)

Jet axial distance (projected): z (μas)
1

Jet radius: R (rg)

102

101

ϕ ∼ 60 (cgs) ←102

Observations(Area) Force-free parabolic jet solution
a = 0.5 (upper edge) - 0.99 (lower edge)MADϕ ∼ 4 (cgs) ←

101

SANE
from GMVA+ALMA Cy 7 proposal (PI: Kim, J.)

Figure 2: GRMHD+GRRT images and simulated GMVA(+ALMA)
the• legend
for references).
Topinand: jet formation
with highφ~100, a=0.9
Adequate
jet expansion
thebottom
lateral directionin MAD
φ~70, a=0.9
left • toΓ
right: imagesfromthesimulations,
synthetic
GMVA+AL1!
increases
due
to
the
magnetic
nozzleeffectφ~30, a=0.9
without ALMA.
φ~10, a=0.9
GMVA + ALMA
• Unexpected counter jet emission is suppressedthestructure
of
the
onset
of
the
jet,
(iii)
establish
firm
ev
1
2
1
10
10
• Quasi-symmetric limb-brightens feature may appears
launching in M 87 based on polarization measurement.
MN+ in prep.
Jet axial distance (de-projected): z (rg)in the approaching jet side (! ≲ 100 μas)
3 Immediate Objectives :• Proving presence/absenceofaring-likefeatureat
3mm• Let’s see imaging the jet w/ EHT@230GHz/ GMVA@86GHz in 2020
recent state-of-the-art numerical simulations predict bright synchr
phology at the base of jet (Fig. 2). In the standard jet formatio
01/20/2020, Sendai
angular momentum by surrounding magnetic field (B-field) leads toSummary• MWL data (< 230 GHz) is useful to nail down the horizon-scale·parameters (Φ! EH, LEM, M) in M87• EHT2020: Simultaneous obs. with EAVN/KVN (22/43/86/129GHz)

and GMVA+ALMA towards VLBI cores• Presumably, MAD in action in M87:

!ϕ ≃ 30 − 70
33
− 6 1/2
9
3/2·• !ΦEH ≃ 10 (ϕ/60) (m/4 × 10 )(M/6.5 × 10 M⊙) Mx
43−
1• !LEM ≃ (4 − 15) × 10 erg s (a = 0.9)•

• Limb-brightened feature is one of key observables

01/20/2020, Sendai

Jan 31, 2020: Deadline for registrations / abstract submission
http://eaagn2020.csp.escience.cn/dct/page/1