Black Hole Shadow with Accretion Flow and Jets

Transcription

1 Black Hole Shadow with Accretion Flow and Jets Hung-Yi Pu (ASIAA) M87 workshop 2016/05/24 Collaborators: Kinwah Wu (UCL), Ziri Younsi (ITP & ULC), Yosuke Mizuno (ITP), Kazunori Akiyama (MIT & NAOJ), Kazuki Kuramochi (NAOJ) Masanori Nakamura (ASIAA), Keiichi Asada (ASIAA), Kouichi Hirotani (ASIAA),

2 black hole shadow general properties and GRRT with accretion (example: Sgr A*) flow dynamics with jet (example: M87) the non-thermal electrons populations Summary

3 ergosphere event horizon image produced by Odyssey_Edu: (Pu and Yun 2016)

4 4 GM/c 2 10 GM/c 2 ~40μas ~40μas for for M87 M87; ~50μas for Sgr A* ( M, 16.7 Mpc)

5 Black Hole Shadow center of BH shadow shifts when BH spin varies

6 GR Radiative Transfer as an Tool *Photon p

7 GR Radiative Transfer as an Tool *Photon *GR + HD/ MHD p u I = I / 3 = invariant *energy shift E comoving E obs = p u 0 p u 1 *radiative transfer di = I + d = = j / 2 (invariant) (invariant)

8 1 E comoving E obs = p u 0 p u 1 I = I / 3 = invariant observer-source approach E emit (u i ),f emit (u i ), θ emit (u i ) fluid s co-moving frame u i (x i ) u p Constructing Dynamical Jet Evolution di = I + d Younsi et al ( dt d, dr d E emit (u i ),f emit (u i ), θ emit (u i ) observer s image frame Observer s image frame, d p t = p E = L z E d obs,f obs d, d d, dp r Fuerst & Wu 2004 d d = 1 0, di = 1 j0, d 3, dp d )

9 M N kernal_fun<<<m,n>>>(par1, par2, ) M*N parallel threads are being launched Odyssey: a GPU based parallel code for GRRT (Pu, Yun, Younsi, and Yoon, 2016)

10 Compute Unified Device Architecture

11 Modeling Accretion

12 Keplerian rotation disk Fukue 1989 rotating shell Broderick et al. 2006,2011,2016 free-fall (zero angular momentum at infinity) what model best describes. Sgr A*? (~10-8 MEdd) Falcke et al. 2000

13 sub-keplerian Accretion flow Keplerian balance between gravity, rotation and pressure balance between gravity and disk rotation ion electron innermost stable circular orbit advection cooling radiative cooling radiative inefficient heat stored inside disk, and disk puff up radiative efficient thin disk relative accretion rate

14 B 2 / =1 a =0.9 = u u t k = 1 r 3/2 1 / k = 1.1, 1.0, 0.9, 0.8 GRMHD simulation for a RIAF ISCO (HARM 2D code)

15 Frequency dependency optically thin higher frequency (transparent) optically thick (opaque)

16 n e,th / r 1.1 T e / r 0.84 Yuan et al. 2003

17 n e,th / r 1.1 exp( z 2 /x 2 ) n e,nth / r exp( z 2 /x 2 ) T e / r 0.84 as in e.g., Broderick et al. 2006, 2011, Yuan et al. 2003

18 Dynamical dependency *everything is the same except the flow dynamics free-fall rotation Keplerian rotating e.g., Broderick et al. 2006

19 *a=0, viewing angle =68 o (Broderick et al.2011) 230GHz Kep sub-kep free-fall ν L ν (erg/s) GHz ν (GHz)

20 *position angle =150 o (Broderick et al.2016)

21

22 Modeling Jet

23 T µ = T µ EM T µ = T µ EM + T µ fluid H.-Y. Pu et al energy flux E r T r t ne EM u r light surface outflow corona + accretion flow inflow separation surface (stagnation surface) Koide et al static limit Black Hole light surface

24 thermal synchrotron ne,th(x,y,z) Te(x,y,z) non-thermal synchrotron ne,nth(x,y,z) min max

25 thermal synchrotron ne,th(x,y,z) Te(x,y,z) GRMHD simulation ni(x,y,z) Ti(x,y,z) assumption B(x,y,z) non-thermal synchrotron ne,nth(x,y,z) assumption min max

26 GRMHD simulation thermal synchrotron ne,th(x,y,z) Te(x,y,z) assumption ni(x,y,z) Ti(x,y,z) T i T e =3 T i T e = A b2 1+b 2 + B 1 1+b 2 b = P gas /P mag A = 100 B =1 (Moscibrodzka et al. 2016) log kte/mc 2 log kte/mc 2 log ne

27 GRMHD simulation thermal synchrotron ne,th(x,y,z) Te(x,y,z) assumption ni(x,y,z) Ti(x,y,z) 230GHz BH mass=4.3 x 10 6 Msun mdot~10-9 medd image: H.-Y. Pu log ne

28 GRMHD simulation thermal synchrotron ne,th(x,y,z) Te(x,y,z) ni(x,y,z) Ti(x,y,z) two temperature GRMHD simulation or GRRMHD simulation

29 GRMHD simulation ni(x,y,z) Ti(x,y,z) Dexter et al B(x,y,z) non-thermal synchrotron ne,nth(x,y,z) assumption min max

30 GRMHD simulation ni(x,y,z) Ti(x,y,z) Dexter B(x,y,z) non-thermal synchrotron ne,nth(x,y,z) assumption u nth = B2 8 min max non-thermal internal energy is a good fraction of field energy

31 Challenge thermal syn + non-thermal syn unknown non-thermal electron properties (spatial and energy distribution) can we consider the variation of the nonthermal electron? Moscibrodzka Moscibrodzka Broderick Chan Dexter

32 zoom in the separation surface energy flux light surface outflow corona + accretion flow inflow separation surface (stagnation surface) ck Hole origin of nonthermal electrons? Black Hole static limit light surface

33 n e,nth (,s)= 0 n e,th g( ) s energy flux light surface outflow A B C inflow corona + accretion flow separation surface (stagnation surface) static limit Black Hole light surface

34 Model Setting B A C semi-analytical force-free jet model by Broderick and Leob 2009

35 B initial condition at sep. surface min =1 = 0 max

36 Spatial variation of non-thermal electrons max B computed results = 0 due to synchrotron cooling M BH = M min =1 max = 100

37 image spectrum??

38 possible characteristic of separation surface? *toy model and very preliminary result

39 black hole shadow strongly depends on the environment with accretion (example: Sgr A*) flow dynamics could be an important parameter when interpretation EHT observations for Sgr A* with jet (example: M87) investigating the sptial variation of non-thermal electrons