getting to eddington and beyond in agn and binaries!
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Getting to Eddington and beyond in AGN and binaries!. Chris Done University of Durham. Accreting black holes. L / L Edd determined by mass accretion rate onto the black hole LMXRB – roche lobe overflow of low mass companion HMXRB – wind accretion from high mass companion - PowerPoint PPT PresentationTRANSCRIPT
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Getting to Eddington and beyond in AGN and binaries!
Chris DoneUniversity of Durham
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• L/LEdd determined by mass accretion rate onto the black hole
• LMXRB – roche lobe overflow of low mass companion
• HMXRB – wind accretion from high mass companion
• HMXRB – roche lobe overflow from high mass companion
• AGN
Accreting black holes
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• L/LEdd determined by mass accretion rate onto the black hole
• LMXRB – roche lobe overflow of low mass companion
• HMXRB – wind accretion from high mass companion
• HMXRB – roche lobe overflow from high mass companion
• AGN
Accreting black holes
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• L/LEdd determined by mass accretion rate onto the black hole
• LMXRB – roche lobe overflow of low mass companion
• HMXRB – wind accretion from high mass companion
• HMXRB – roche lobe overflow from high mass companion
• AGN
Accreting black holes
![Page 5: Getting to Eddington and beyond in AGN and binaries!](https://reader035.vdocuments.us/reader035/viewer/2022062520/56815a73550346895dc7d9a3/html5/thumbnails/5.jpg)
• L/LEdd determined by mass accretion rate onto the black hole
• LMXRB – roche lobe overflow of low mass companion
• HMXRB – wind accretion from high mass companion
• HMXRB – roche lobe overflow from high mass companion
• AGN
Accreting black holes
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LMXRB – Transient!• H ionisation instability in disc – eg Lasota 2001• If T(Rout)<H ionisation then disc globally unstable• T(Rout) depends on mass, mass accretion rate and binary size – all
correlated by roche lobe overflow condition!
DGK072 years
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• Radius of star depends on type (ie mass)
• Star has to fill roche lobe for mass accretion
• Mass accretion rate from companion depends on type
• Outer edge of disc can’t be larger than ½ size of binary orbit.
• Find all have T(Rout)<H ionisation instability for all low mass companion stars
• See review by Lasota (2001)
Roche lobe overflow
Menou et al 1999
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• Peak luminosity depends on how much mass can accumulate in quiescence and how fast it accretes onto black hole
• Lpeak R(out)3/R(out ) R(out)2 King & Ritter 1998
• Main sequence secondary is small so R(out) small so Lpeak<LEdd
Roche lobe overflow
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• GRS1915+105 is huge! 33 day period. L/LEDD~1 for 20 years
• GS2023 – went to 2LEdd, then blew its disc apart…
• GX339 and XTEJ1550 are the next biggest but L<LEDD
J. Orosz
LMXRB BH in our galaxy
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• Rare systems – most end as NS in population synthesis models
• High mass loss rate from stellar wind, but only capture small fraction so L<<LEdd
Winds fed HMXRB – BH
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• Main sequence high mass star. Mass accretion rate from companion is high
• Keeps outer disc temperature in Cyg X-1 above H ionisation so persistent
• HUGE mass transfer as supergiant evolves – SS 433 in our galaxy
• Most ULX in other galaxies
Roche lobe overflow HMXRB-BH
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• Main sequence high mass star. Mass accretion rate from companion is high
• Keeps outer disc temperature in Cyg X-1 above H ionisation so persistent
• HUGE mass transfer as supergiant evolves – SS 433 in our galaxy
• Most ULX in other galaxies
Roche lobe overflow HMXRB-BH
Rappaport et al 2005
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Intermediate mass BH?
• Ultra - Luminous X-ray sources in spiral arms of nearby starforming galaxies – ULX
• L~1039-40 ergs s-1 so M~10-100 M
for L <LEdd
• Hard for stellar evolution to make BH > 50 M
Gao
et a
l 200
3
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• Hard spectra plus soft excess looks like scaled up BHB in LHS?
• IMBH?
• But break above 7keV – NOT like LHS!!!
ULX state ?
Gladstone Roberts & Done 2008
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ULX state ?
Gladstone Roberts & Done 2008
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ULX state ?
Gladstone Roberts & Done 2008
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ULX state ?
Gladstone Roberts & Done 2008
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• L/LEdd determined by mass supply
• But ~0.5% of mass in star formation ends up in the black hole to make the M- relation
AGN
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BH-Galaxy AND environment•Big black holes live in host galaxies with big bulges!
•Need 0.5% of bulge mass (ie starformation) to end up down the BH
Bla
ck h
ole
mas
s
Stellar system mass
103
109
1061012
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Black hole mass
• SMBH grow by gas accretion and BH-BH mergers
• Mergers dominate only highest BH mass (> 109 M) . Spin of 0.7-0.8
• Accretion (thin disk) dominates for lower mass (<108 M)
• Accretion (hot flow) never really dominates
Fanidakis et al 2010
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Black hole mass accretion rate
• Not many with L/LEdd>1 in local universe - and they are predominantly low mass BH
• What do they look like?
Fanidakis et al 2010
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Disc spectra from 106 M L/LEdd ~1
• Much more soft X-ray flux than expected from either disc or power law
• Enormous soft X-ray excess !!
Jin et al 2011
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Disc spectra from 106 M L/LEdd ~1
• Standard SS disc temperature – assumes energy thermalises
• BHB discs - Colour temperature correction as scattering > absorption opacity. Tobs=1.8 Teff
• AGN discs even more scattering dominated as less dense !! Factor 2.4 !!
•
Done, Davis, Jin, Blaes Ward 2011
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Disc spectra from 106 M L/LEdd ~1
• Enourmous soft excess in REJ1034
• But actually a lot of it should be the bare disc!
• Plus a little bit of comptonisation !
• More like disc dominated black holes
Done, Davis, Jin, Blaes Ward 2011
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Conclusions• Galactic BHB can’t get to Eddington very easily
• Exceptions are LMXRB in wide binaries with evolved companions – GRS1915+105
• And HMXRB evolving into supergiants – SS 433 and probably ULX.
• And some nearby low mass high mass accretion rate AGN like REJ1034 (QPO AGN).
• Disc in these AGN MUST extend into soft X-rays. Much of soft X-ray excess in these is the bare disc. Then need SMALL comptonisation to get shape of component
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Unsolved problems• How does magnetic field stress dissipate and heat the accretion flow?
Can we get as high as ~0.1? Stress HEATS so eventually gives pressure so alpha prescription OK on average??
• What happens to the disc as we go to Eddington and beyond? – How does it stay optically thick up to ~0.5LEdd?
– How important are winds Fgrav=(1- abs/ es L/LEdd) GM/R2
– How important is advection of radiation – and what fraction of this escapes from the plunging region becoming optically thin: not radiatively inefficient?
• How does the B field manage to get the same (approx) vertical flux to launch the same power jet in lots of different BHB?
• How does thin cool disc truncated into hot flow? Simulations??• what are the HF QPOs ?
– method for measuring a*? But LF QPOs probably don’t !!!!
• Can we understand iron line profiles ? And get all methods for measuring a* giving the same answer?