Jet Break in M87: Fundamental Property in AGN Jets Masa Nakamura - - PowerPoint PPT Presentation

SLIDE 1

Masa Nakamura (ASIAA, Taiwan)

Institute for Theoretical Physics Seminar, Goethe University, Frankfurt, Germany, 12/04/2015

Jet Break in M87: Fundamental Property in AGN Jets

SLIDE 2

SOC: P. Ho (ASIAA, Chair)

• L. Ho (KIAA, Vice-chair, keynote speaker)
• R. Blandford (Stanford, keynote speaker)
• A. Fabian (IoA, Keynote speaker)
• R. Narayan (CfA, Keynote speaker)
• K. Asada (ASIAA, Secretary)
• M. Nakamura (ASIAA, Secretary)

Towards(the(100th(Anniversary(of(the(Discovery(of(Cosmic(Jets

M87 Workshop

May 23-27 2016, ASIAA, Taipei

Image courtesy (left: Francisco Diez, middle: J.-C. Algaba, right: Greenland telescope)

Web.: http://events.asiaa.sinica.edu.tw/workshop/20160523/index.php Contact: m87ws2016@asiaa.sinica.edu.tw Invited Speakers (*TBD):

• K. Asada (ASIAA), J. Biretta (STScI), G. Bower (ASIAA), A. Broderick

(U. Waterloo), E. Churazov (MPA), S. Doeleman (MIT Haystack), *A. Doi (JAXA), J. Hawley (U. Virginia), A. Levinson (Tel Aviv U.), B. McNamara (U. Waterloo), H. Li (LANL), *D. Meier (Caltech), S. Mineshige (Kyoto U.),

• M. Mościbrodzka (Radboud U.), M. Nakamura (ASIAA), E. Perlman

(FIT), W. Potter (U. Oxford), Ł. Stawarz (Jagiellonian U.),

• A. Tchekhovskoy (UCB), *C. Walker (NRAO), J. Walsh (Texas A&M U.)

TOPICS

• SMBHs; mass, spin, and imaging of BH silhouettes
• BH accretion flows; from Bondi radius to the horizon
• BH Jets; from the horizon to galactic scale
• Co-evolution of galaxy and black hole: AGN feedback
• High energy emissions in LLAGNs; their sites and mechanisms

Registration & Abstract Submission ( - 2016/02/15)

SLIDE 3

Outline

• Introduction to M87; puzzle has remained

unsolved on the jet acceleration/collimation

• MHD Jet global structure and dynamics under

the BH gravitational influence and beyond

• MAD in Action; how large is the BH spin?
• Lessons learned from M87; “jet break” in AGNs

may be norm in the BH-galaxy co-evolution?

• Summary

SLIDE 4

Junor+ (1999), Nature

10-2 10-1 1 101 102 103 2 4 6 8

10-3 10-2 10-1 1 101

Distance from the nucleus: z (pc) Distance from the nucleus: z (arcsec) Apparent speed (V/c)

Reid et al. (1989) Junor & Biretta (1995) Biretta et al. (1995) Biretta et al. (1999) Cheung et al. (2007) Kovalev et al. (2007) N2 L HST-1 D E F AB C

• Q. What is a large gap?
• Q. Collimation is real (i.e.

the jet is cylindrical or not)?

We have no clear view of jet acceleration/ collimation even in the most studied AGN jet …

Puzzle Has Remained Unsolved During decades

θ

SLIDE 5

Bp field lines and characteristic surfaces McKinney (2006) Out-going Fast Light Cylinder Out-going Alfvén Out-going Slow In/out-flow Separation Ergosphere Pu, MN, + (2015), ApJ

GRMHD Simulation (a =0.9375) Steady GRMHD (cold) solution (a =0.9375)

Bp field: parabolic solution (Blandford & Znajek 1977) + perturbation (Beskin & Nokhrina 2006) In-going Alfvén In-going Slow Horizon/in-going Fast

GRMHD (1st ever) Steady Inflow/Outflow Solutions for a Parabolic Streamline

Black Hole

corona + accretion flow

inflow energy flux

light surface separation surface light surface static limit

Black Hole

• utflow

SLIDE 6

Open Question 1: How Acceleration/ Collimation in MHD jets is Terminated?

µ γ = 1 + σ

σ : Poynitng-to-matter energy flux ratio

• Capability of cold RMHD jet acceleration

can be measured by the total (matter + Poynting)-to-matter energy flux ratio:

γ∞ µ (σ∞ 0)

µ ∼ 101−3

(Beskin 2010; Nokhrina+ 2015)

would be norm?

µ 10 σ∞ 0

• ,

(45)

• B
• B
• ∣

∣

• ∣

∣

• ∣

∣

• Pu, MN+ (2015), ApJ; qualitatively consistent with McKinney (2006)

θj ∝ z(1−a)/a Γ ∝ z(a−1)/a

along a streamline that threads the EH at mid-latitude (similar to McKinney 2006) separation point

Γ ¯ Br/ ¯ Bφ ' 1

quasi F-F; e.g., Lyutikov+ (2005) Clausen-Brown+ (2011) c.f., Jorstad+ (2005) Pushkarev+ (2009) Clausen-Brown+ (2013)

Γθ ∼ 0.1

SLIDE 7

Transition found in MOJAVE AGNs

Figure 6. Histograms of projected linear distance for jet features

Homan+ (2015) Lister+ (2013) (see also Kellermann 2004; similar tendency can been seen)

• A transition from positive to negative acceleration seems to locate at ~ 10 pc

(Lister+ 2013; Homan+ 2015) ⇒ ~ 100 pc or longer in de-projection

• Non-ballistic flows are strongest at < 10 pc; jets are expanding less rapidly than

z ∝ r, so that jets is still being collimated (Homan+ 2014; also Pushkarev & Kovalev 2012 w/ Tb analysis)

SLIDE 8

2007 2008 2009 milliarcsecond milliarcsecond 200 400 600 800 200

Asada, MN+ (2014), ApJL

SL Motions Upstream of HST-1

EVN Observations@1.6GHz

SLIDE 9

Asada, MN+ (2014), ApJL Bondi radius

Kovalev et al. 2007: VLBA at 15 GHz Reid et al. 1989: Gloabal VLBI at 1.6 GHz Cheung et al. 2007: VLBA at 1.6 GHz Biretta et al. 1999: HST Biretta et al. 1995: VLA at 15 GHz Meyer et al. 2013: HST Ly et al. 2007; VLBA 43 GHz (area) Walker et al. 2008: VLBA 43 GHz Acciari et al. 2009: VLBA 43 GHz Kovalev et al. 2007: VLBA at 15 GHz Reid et al. 1989: Gloabal VLBI at 1.6 GHz Cheung et al. 2007: VLBA at 1.6 GHz Biretta et al. 1999: HST Biretta et al. 1995: VLA at 15 GHz Meyer et al. 2013: HST Ly et al. 2007; VLBA 43 GHz (area) Walker et al. 2008: VLBA 43 GHz Acciari et al. 2009: VLBA 43 GHz This work: EVN at 1.6 GHz

A Missing Link Has Been Filled

SLIDE 10

Asada & MN (2012), ApJL; MN & Asada (2013), ApJ; Asada, MN+ (2014), ApJL

Jet Structure and Dynamics in M87

Sub/Superluminal Pairs

(Trailing MHD shocks? MN+ 2010, MN & Meier 2014)

“Jet break” “ D e c e l e r a t i

• n

”

z ∝ r0.99

1 101 102 103 104 105 106

ISCO for Schwarzshild BH

10-3 10-2 10-1 1 101 102 103 104 Deprojected distance from the nucleus: z (pc) Radius: r (rs)

MERLIN 1.8 GHz (Asada & Nakamura 2012) EVN 1.6 GHz (Asada & Nakamura 2012) VLBA 15 GHz (Asada & Nakamura 2012) VLBA 43 GHz (Asada & Nakamura 2012) VLBA Core 43 GHz (Nakamura & Asada 2013) VLBA Core 86 GHz (Nakamura & Asada 2013) EHT Core 230 GHz @2009 (Doeleman et al. 2012) VLBA Core 5, 8, 15, 24, 43, & 86 GHz (Hada et al. 2013) EHT Core 230 GHz @2012 (Akiyama et al. 2015)

HST-1

1 101 102 103 104 105 106 107 10-3 10-2 10-1 1 101

Bondi radius

Distance from the nucleus: z (rs) Four-velocity: ΓV/c

VLA 15 GHz (Biretta et al. 1995) HST (Biretta et al. 1999) HST (Meyer et al. 2013) VLBA 1.7 GHz (Cheung et al. 2007) VLBA 1.7GHz + EVN 5 GHz (Giroletti et al. 2012) EVN 1.6 GHz (Asada et al. 2014) VLBI 1.6 GHz (Reid et al. 1989) VLBA 15 GHz (Kellermann et al. 2004) VLBA 15 GHz (Kovalev et al. 2007) (area) VLBA 43 GHz (Ly et al. 2007)

HST-1

“ A c c e l e r a t i

• n

”

z ∝ r1.75

SLIDE 11

Outline

• Introduction to M87; puzzle has remained

unsolved on the jet acceleration/collimation

• MHD Jet global structure and dynamics under

the BH gravitational influence and beyond

• MAD in Action; how large is the BH spin?
• Lessons learned from M87; “jet break” in AGNs

may be norm in the BH-galaxy co-evolution?

• Summary

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Open Question 2: How Are GRMHD Jets Confined?

HARM 2D (Gammie+ 2003; Noble+ 2006): 2562 grids a = 0.9375

βp ≡ pgas/pmag pgas pmag

• Quasi-steady jet is formed, while corona/wind are highly turbulent (~ 2,000 MG/c3)
• Global jet structure is unchanged even after the MRI in the corona is saturated
• Gas pressure-dominated corona may not confine the jet, suggesting the jet and

corona/wind may be a force-free on the small scale (< 100 rs)

BZ77 BP82

PRELIMINARY

SLIDE 13

• A power-law dependence of the azimuthal current
• n the equatorial plane (McKinney & Narayan 2007):
• GRMHD simulated jet agrees well with the force-free field

solution for a thin disc with an r-5/4 (i.e., BP82)

Outer Boundary of GRMHD Jets

• Strong BH B-field squeeze the accretion flow vertically

down to h/r ~ 0.05 near the EH from ~ (0.3 - 1) at large distances (Tchekhovskoy 2015) a=0.9375 BZ77 BP82 dIφ dr ∝ 1 r2−ν

2 4 2 4

Tchekhovskoy+ (2011)

⊗Toroidal current: Iφ

⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗ ⊗

ν = 1 ν = 3/4

(Parabolic, Blandford & Znajek 1977) (Blandford & Payne 1982) (split-monopole)

ν = 0 dIφ dr ∝ 1 r2−ν

SLIDE 14

a = 0.7 a = 0.9 a = 0.99 b2/ρc2 βplasma a = 0.5 b2/ρc2 ' 1 pgas/pmag . 0.1 t = 104 GM/c3 t = 104 GM/c3 t = 104 GM/c3 t = 104 GM/c3

PRELIMINARY PRELIMINARY

SLIDE 15

Comparison w/ Observations in M87

MN, Noble+ in prep.

10-1 1 101 102 103 104 1 101 102 103 Distance from the black hole: z (rg) Radius: r (rg)

VLBA 15 GHz (Asada & Nakamura 2012) VLBA 43 GHz (Asada & Nakamura 2012) VSOP 5 GHz (Asada, Nakamura, & Pu in prep.) VLBA Core 43 GHz (Nakamura & Asada 2013) VLBA Core 86 GHz (Nakamura & Asada 2013) VLBA Core 5, 8, 15, 24, 43, & 86 GHz (Hada et al. 2013) EHT Core 230 GHz @2009 (Doeleman et al. 2012) EHT Core 230 GHz @2012 (Akiyama et al. 2015) Approximate F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Payne 1982) Analytical F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Znajek 1977) Ergosphere (a=0.7)

10-1 1 101 102 103 104 1 101 102 103 Distance from the black hole: z (rg) Radius: r (rg)

VLBA 15 GHz (Asada & Nakamura 2012) VLBA 43 GHz (Asada & Nakamura 2012) VSOP 5 GHz (Asada, Nakamura, & Pu in prep.) VLBA Core 43 GHz (Nakamura & Asada 2013) VLBA Core 86 GHz (Nakamura & Asada 2013) VLBA Core 5, 8, 15, 24, 43, & 86 GHz (Hada et al. 2013) EHT Core 230 GHz @2009 (Doeleman et al. 2012) EHT Core 230 GHz @2012 (Akiyama et al. 2015) Approximate F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Payne 1982) Analytical F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Znajek 1977) GRMHD simulations (a=0.7-0.99) for outermost streamlines Ergosphere (a=0.7)

10-1 1 101 102 103 104 1 101 102 103 Distance from the black hole: z (rg) Radius: r (rg)

VLBA 15 GHz (Asada & Nakamura 2012) VLBA 43 GHz (Asada & Nakamura 2012) VSOP 5 GHz (Asada, Nakamura, & Pu in prep.) VLBA Core 43 GHz (Nakamura & Asada 2013) VLBA Core 86 GHz (Nakamura & Asada 2013) VLBA Core 5, 8, 15, 24, 43, & 86 GHz (Hada et al. 2013) EHT Core 230 GHz @2009 (Doeleman et al. 2012) EHT Core 230 GHz @2012 (Akiyama et al. 2015) GMVA 86 GHz (Asada et al. in prep.) Approximate F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Payne 1982) Analytical F-F solutions (a=0.7-0.99) for outermost streamlines (Blandford & Znajek 1977) GRMHD simulations (a=0.7-0.99) for outermost streamlines Ergosphere (a=0.7)

PRELIMINARY

SLIDE 16

Trails of Components?

A B C I F E D G (HST-1)

Cheung+ (2007)

c1:4.3c c2:0.47c

MN+ (2001); MN & Meier (2004) Growing Current-driven instability

U p p e r l e f t : k n

• t

I a p p e a r s t

• f

a d e a n d m

• v

e b a c k w a r d a l

• n

g t h e j e t a t . 2 3 ± . 1 2 c . L

• w

e r l e f t : k n

• t

A i s s h

• w

n w i t h a s t r e t c h t

• e

m p h a s M i d d l e p a n e l : t h e k n

• t

A / B c

• m

p l e x s h

• w

s r e m a r k a b l e v a r i a b i l i t y , w i t h b

• t

h s u b

• r

e l a t i v i s t i c a n d s u p e r l u m i n a l a p p a r e n t m

• t

i

• n

s . a p p e a r s i n t h e l a s t e p

• c

h . R i g h t p a n e l : k n

• t

C s h

• w

s s p e e d s

• n

t h e

• r

d e r

• f

. 4 – . 9 c . B

• t

t

• m

p a n e l : a d e p i c t i

• n
• f

v e t h e

• n

l i n e j

• u

r n a l . )

pixels yr

− 1

in both previous studies.

5

As suggested by the

• n Figure 1, D-Middle is one of the fastest

a speed of 4.27 ± 0.30c along the jet, D-West shows evidence of deceleration by the final epoch in 2008, while transverse speeds of −0.59 are consistent 0.98c

Note: Knots are NOT stationary except HST-1

P r

• j

e c t e d V

• fi

e l d s ( M e y e r + 2 1 3 ) P r

• j

e c t e d B

• fi

e l d s ( O w e n + 1 9 8 9 )

B⊥ B⊥ B

SLIDE 17

Length scale (Rg)

FS FF RF RS Conical expansion

Length scale (pc)

A C HST-1 Trailing knots Flow streamline

5106 107 500 1000 1500

B DE DW

MN, Garofalo, & Meier (2010), ApJ

Trails of MHD Shocks?

SLIDE 18

Quad RMHD Shock Model

t =2.0

2 4 6 8 2 4 6 8 /0

RF RS CD FS FF

(a)

20 40 60 B (mG) (b) 10-2 10-1 1 101 p (c) 10-1 1 101 102

• (d)

1.5 1.6 1.7 1.8 1.9 20 40 60 80 z (pc) tan-1(B/Bz) (e)

• 10-8

5 10

• (c)

1.5 1.6 1.7 1.8 1.9

• 0.2

0.2 z (pc) V/c (d)

MN, Garofalo, & Meier (2010), ApJ; MN & Meier (2014), ApJ Biretta et al. (1999)

θv~ 14°: Vε ~ 0.99 c ⇒ FF VEast ~ 0.79 c ⇒ RF

DSA (Fermi I acceleration via relativistic shock): 1.Proper compression

• 2.Low magnetization
• 3.Low magnetic obliquity

σ 0.5

θ 13 n(E) ∝ E−δ, δ = 2.2 − 2.3

rcmp = 3.3 − 3.5

A super-fast magnetosonic flow drives forward/reverse-fast/slow shocks

“Counter-rotation”

SLIDE 19

Outline

• Introduction to M87; puzzle has remained

unsolved on the jet acceleration/collimation

• MHD Jet global structure and dynamics under

the BH gravitational influence and beyond

• MAD in Action; how large is the BH spin?
• Lessons learned from M87; “jet break” in AGNs

may be norm in the BH-galaxy co-evolution?

• Summary

SLIDE 20

BAF / ADAF

˙ M/ ˙ MB

r/rs

˙ MB 0.12M/yr (e.g., Di Matteo+ 2003)

RIAF theory/simulation suggests a substantial decrease

• f the BH mass accretion; how is the M87 jet powered

(Pj ~ 1043-44 erg/s)?

RIAF in M87

GADAF CDAF/ADIOS

(Kuo, Asada+ 2014, RM obs., SMA@230GHz)

˙ M• 9.2 × 104M/yr

2D MHD sim. (Yuan+ 2012) 3D MHD sim. (Pang+ 2011)

1 101 102 103 104 105 10-6 10-5 10-4 10-3 10-2 10-1 1

Pj/ ˙ M•c2 > 1

?

Pj(= 5 × 1043 erg/s)/ ˙ M•c2 ∼ 1

R u s s e l l + ( 2 1 5 ) (e.g., Ghisellini+ 2014)

SLIDE 21

MAD in Action in M87?

0.2 0.4 0.6 0.8 1 1040 1041 1042 1043 1044 1045 1046 0.2 0.4 0.6 0.8 1 1040 1041 1042 1043 1044 1045 1046

Black hole spin : a∗ ≡ a/M Black hole spin : a∗ ≡ a/M η = Pj ˙ M•c2 × 100% Jet power : Pj [erg/s]

e.g., Tchekhovskoy (2015)

• Magnetically Arrested Disk (MAD)

(Bisnovatyi-Kogan & Ruzmaikin 1974, 1976; Narayan 2003; Tchekhovskoy+ 2011; Tchekhovskoy & McKinney 2012; Zamaninasab+ 2014) φ• = Φ• ( ˙ M•r2

gc)1/2 50 (spin average)

MN+ in prep.

˙ M• 6.3 104 R 10rs 0.5 M/yr (e.g., Kuo, Asada+ 2014; Russell+ 2015) for a MAD state (FG ≈ FB)

0.2 0.4 0.6 0.8 1 50 100 150 200 Maximum radiative efficiency ~ 30% for a thin disk with a/M=0.998 (Thorne 1974)

a/M & 0.6

SLIDE 22

Outline

• Introduction to M87; puzzle has remained

unsolved on the jet acceleration/collimation

• MHD Jet global structure and dynamics under

the BH gravitational influence and beyond

• MAD in Action; how large is the BH spin?
• Lessons learned from M87; “jet break” in AGNs

may be norm in the BH-galaxy co-evolution?

• Summary

SLIDE 23

Case 2: FRI RG

SMBH sphere of inf. geometrical transition parabolic, z ~ r2.02 conical, z ~ r

. 9 4

Jet Radius [rs] [pc] Deprojected Distance from Core [rs] [pc]

VLBA 15 GHz VLBA 5 GHz (This work) EVN(a) 1.6 GHz (This work) EVN(b) 1.6 GHz (This work) EVN(c) 1.6 GHz Best fit Single power-law fit VLA 1.4 GHz VLBA 15 GHz core VLBA 5 GHz core EVN 1.6 GHz core 102 103 104 105 106 107 108 103 104 105 106 107 108 109 10-2 10-1 100 101 102 103 10-1 100 101 102 103 104

Tseng, Asada, MN+, submitted to ApJL NGC 6251(0.5 pc/mas = 8700 rs), log M● = 8.78, θv=19°

SLIDE 24

Summary

• M87: The best observable for examining the AGN jet with

the highest angular resolution (1 mas ~ 125 rs)

• 1.Sub-mm VLBI will reveal the origin of the jet in M87

as well as the jet inner structure for blazers (non-BK79?)

• 2.VSOP obs. reveals the jet spine (BZ77), while the jet

sheath may be the outermost streamline (BP82) from BH

• 3.Jet acceleration/collimation takes place in the parabolic

stream up to ~ 105 rs (inside the sphere of BH influence)

4.GRMHD jet sim./MAD scenario may give the BH spin as

a > 0.7

• 5.We propose that the “Jet Break” (from parabolic; BP82

to conical; BK79) may be norm in AGNs