1 / 10

(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

chloe
Download Presentation

(Massive) Black Hole X-Ray Binaries

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related