Massive Black Hole XRay Binaries Roger Blandford KIPAC

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

RE J 1034+396 • z=0. 042 Seyfert galaxy • Lbol ~ 1044. 7 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 • <Q> ~ 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 2010 KIAA 2

Conservative Mass transfer § Transfer m -> M at constant m+M, J § J ~ m. MP 1/3 § If M>>m and gravitational radiation wins, • d. J/dt~-m 2 M 4/3 P-7/3 § If m fills Roche lobe, P~r-1/2 ~m 0. 8 =>J~m 1. 3 • J decreases • Orbit expands Stable • Period lengthens 2 xi 2010 KIAA cf Hameury et al Mass Transfer 3

Relativistic Roche Problem § Riemann -> local tidal tensor. § Evaluate volume within critical equipotential and evaluate • • r(L 1)=0. 3 m 1/3 P 2/3 Ro r(Roche)=90 P-2 g cm-3 Good for N, ISCO (all a) Accurate interpolation Roche Potential L 1 § Lose mass through L 1, L 2 2 xi 2010 KIAA 4 L 2

Pre-Roche evolution § Gravitational radiation dominates • Need PPN corrections to torque § Low mass star fills Roche lobe when P=PR=8 m 0. 8 hr [ => m < 0. 1 Mo ] § Outside ISCO • P > PISCO ~ M [=>M<3 x 107 Mo] § Time to overflow t. R-t=2 x 105 M 6 -2/3 m 1. 3[(P/PR)8/3 -1] yr 2 xi 2010 KIAA 5

Stellar Evolution § § Differs from close binary case tdynamical << ttransfer << t. Kelvin S[m] will be frozen Solve: d. P/dm=-Gm/4 pr 4 dr/dm=1/4 pr 2 r[S(m), P] => d log <r>/d log m =h h=2 for convective low mass star 2 xi 2010 KIAA d. S/dm >=0 6

Period vs mass 2 xi 2010 KIAA 7

Post-Roche Evolution § After mass transfer orbit expands • P ~ m-h/2 ~ m-1 for low mass star t-t. R=1400 M 6 -2/3 m-1 P 8/3 [(P/PR)11/3 -1] yr; [~ 5000 yr] § Conservative Mass loss dm/dt = (dm/dt)R = -1. 3 x 1020 M 0. 7 P-0. 3 g s-1 [~ 1021 g s-1] ~ -m 8. 3 eventually till ttransfer > t. Kelvin § Dynamical complications • Holding pattern? • Interactions, drag 2 xi 2010 KIAA 8

Mass transfer § Mass flows from L 1 onto relativistic disk forming hotspot § Gas spirals in to rms 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 2010 KIAA 9

Observed X-ray emission a=0 i=5 a=0. 998 i=30 a=0. 998 i=45 2 xi 2010 KIAA 10