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),
black hole shadow general properties and GRRT with accretion (example: Sgr A*) flow dynamics with jet (example: M87) the non-thermal electrons populations Summary
ergosphere event horizon image produced by Odyssey_Edu: https://odysseyedu.wordpress.com (Pu and Yun 2016)
4 GM/c 2 10 GM/c 2 ~40μas ~40μas for for M87 M87; ~50μas for Sgr A* (6.6 10 9 M, 16.7 Mpc)
Black Hole Shadow center of BH shadow shifts when BH spin varies
GR Radiative Transfer as an Tool *Photon p
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)
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. 2012 ( 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 )
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)
Compute Unified Device Architecture
Modeling Accretion
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
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
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)
Frequency dependency optically thin higher frequency (transparent) optically thick (opaque)
n e,th / r 1.1 T e / r 0.84 Yuan et al. 2003
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
Dynamical dependency *everything is the same except the flow dynamics free-fall rotation Keplerian rotating e.g., Broderick et al. 2006
*a=0, viewing angle =68 o (Broderick et al.2011) 230GHz 10 37 10 36 Kep sub-kep free-fall ν L ν (erg/s) 10 35 10 34 10 33 86.5 GHz 10 32 10 1 10 2 10 3 10 4 ν (GHz)
*position angle =150 o (Broderick et al.2016)
Modeling Jet
T µ = T µ EM T µ = T µ EM + T µ fluid H.-Y. Pu et al. 2015 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. 2002 static limit Black Hole light surface
thermal synchrotron ne,th(x,y,z) Te(x,y,z) non-thermal synchrotron ne,nth(x,y,z) min max
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
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
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
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
GRMHD simulation ni(x,y,z) Ti(x,y,z) Dexter et al. 2012 B(x,y,z) non-thermal synchrotron ne,nth(x,y,z) assumption min max
GRMHD simulation ni(x,y,z) Ti(x,y,z) Dexter+ 2012 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
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 + 2016 Moscibrodzka + 2014 Broderick+ 2009 Chan + 2015 Dexter + 2012
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
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
Model Setting B A C semi-analytical force-free jet model by Broderick and Leob 2009
B initial condition at sep. surface min =1 = 0 max
Spatial variation of non-thermal electrons max B computed results = 0 due to synchrotron cooling M BH =6 10 9 M min =1 max = 100
image spectrum??
possible characteristic of separation surface? *toy model and very preliminary result
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