(Massive) Black Hole X-Ray Binaries Roger Blandford KIPAC, Stanford +Jane Dai, Steven Fuerst, Peter Eggleton (Also Hameury, J-P L)

RE J z=0.042 Seyfert galaxy L bol ~ erg s -1 FUV-SX XMM-Newton observations 1 hr QPO in ~1 d observing Best example to date in AGN of a phenomenon quite common in stellar XRB ~ 16 overall but much higher for section of data ~7% sinusoidal profile Interpreted as diskoseismic mode Could it be an EMRI mass transfer binary? Planetars??? 2 xi 2010KIAA2

Conservative Mass transfer  Transfer m -> M at constant m+M, J  J ~ mMP 1/3  If M>>m and gravitational radiation wins, dJ/dt~-m 2 M 4/3 P -7/3  If m fills Roche lobe, P~  -1/2 ~m 0.8 =>J~m 1.3 J decreases Orbit expands Period lengthens 2 xi 2010KIAA Stable Mass Transfer 3 cf Hameury et al

Relativistic Roche Problem  Riemann -> local tidal tensor.  Evaluate volume within critical equipotential and evaluate r(L1)=0.3m 1/3 P 2/3 R o  (Roche)=90P -2 g cm -3 Good for N, ISCO (all a) Accurate interpolation  Lose mass through L1, L2 2 xi 2010KIAA Roche Potential L1L2 4

Pre-Roche evolution  Gravitational radiation dominates Need PPN corrections to torque  Low mass star fills Roche lobe when P=P R =8m 0.8 hr [ => m < 0.1 M o ]  Outside ISCO P > P ISCO ~ M [=>M<3x10 7 Mo]  Time to overflow t R -t=2x10 5 M 6 -2/3 m 1.3 [(P/P R ) 8/3 -1] yr 2 xi 2010KIAA5

Stellar Evolution  Differs from close binary case  t dynamical << t transfer << t Kelvin  S[m] will be frozen  Solve: dP/dm=-Gm/4  r 4 dr/dm=1/4  r 2  [S(m),P] => d log <  /d log m =   =2 for convective low mass star 2 xi 2010KIAA dS/dm >=0 6

Period vs mass 2 xi 2010KIAA7

Post-Roche Evolution  After mass transfer orbit expands P ~ m -  /2 ~ m -1 for low mass star t-t R =1400M 6 -2/3 m -1 P 8/3 [(P/P R ) 11/3 -1] yr; [~ 5000yr]  Conservative Mass loss dm/dt = (dm/dt) R = -1.3x10 20 M 0.7 P -0.3 g s -1 [~ g s -1 ] ~ -m 8.3 eventually till t transfer > t Kelvin  Dynamical complications Holding pattern? Interactions, drag KIAA2 xi 20108

Mass transfer  Mass flows from L1 onto relativistic disk forming hotspot  Gas spirals in to r ms before plunging into hole  Inclined orbits are more complex as streams may not self-intersect  Disk flow may have complex gaps and resonances  Hot spot Doppler beams emission  Also spiral shocks, eccentricity 2 xi 2010KIAA9

Observed X-ray emission 2 xi 2010KIAA a=0 a=0.998 i=5 i=30i=45 a=0 a=0.998 i=30 10