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(Massive) Black Hole X-Ray Binaries

(Massive) Black Hole X-Ray Binaries. Roger Blandford KIPAC, Stanford +Jane Dai, Steven Fuerst, Peter Eggleton (Also Hameury, J-P L). RE J1034+396. z=0.042 Seyfert galaxy L bol ~ 10 44.7 erg s -1 FUV-SX XMM-Newton observations 1 hr QPO in ~1 d observing

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(Massive) Black Hole X-Ray Binaries

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

  2. RE J1034+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??? KIAA

  3. Conservative Mass transfer • Transfer m -> M at constant m+M, J • J ~ mMP1/3 • If M>>m and gravitational radiation wins, • dJ/dt~-m2M4/3P-7/3 • If m fills Roche lobe, P~r-1/2 ~m0.8 =>J~m1.3 • J decreases • Orbit expands • Period lengthens cf Hameury et al Stable Mass Transfer KIAA

  4. Relativistic Roche Problem • Riemann -> local tidal tensor. • Evaluate volume within critical equipotential and evaluate • r(L1)=0.3m1/3 P2/3 Ro • r(Roche)=90P-2 g cm-3 • Good for N, ISCO (all a) • Accurate interpolation • Lose mass through L1, L2 Roche Potential L1 L2 KIAA

  5. Pre-Roche evolution • Gravitational radiation dominates • Need PPN corrections to torque • Low mass star fills Roche lobe when P=PR=8m0.8hr [ => m < 0.1 Mo ] • Outside ISCO • P > PISCO ~ M [=>M<3x107Mo] • Time to overflow tR-t=2x105M6-2/3m1.3[(P/PR)8/3-1] yr KIAA

  6. Stellar Evolution • Differs from close binary case • tdynamical << ttransfer << tKelvin • S[m] will be frozen • Solve: dP/dm=-Gm/4pr4 dr/dm=1/4pr2r[S(m),P] => d log <r>/d log m =h h=2 for convective low mass star dS/dm >=0 KIAA

  7. Period vs mass KIAA

  8. Post-Roche Evolution • After mass transfer orbit expands • P ~ m-h/2 ~ m-1 for low mass star t-tR=1400M6-2/3m-1 P8/3 [(P/PR)11/3-1] yr; [~ 5000yr] • Conservative Mass loss dm/dt = (dm/dt)R = -1.3x1020M0.7P-0.3 g s-1 [~ 1021g s-1] ~ -m8.3 eventually till ttransfer > tKelvin • Dynamical complications • Holding pattern? • Interactions, drag KIAA

  9. Mass transfer • Mass flows from L1 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 KIAA

  10. Observed X-ray emission a=0 i=5 i=30 a=0.998 a=0 i=30 i=45 a=0.998 KIAA

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