1 Astrophysical black holes Chris Reynolds Department of Astronomy.
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Astrophysical black holesAstrophysical black holes
Chris ReynoldsDepartment of Astronomy
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TopicsTopics
Observational evidence for black holesX-ray studies of strong-gravity regionFirst observational studies of BH spinFuture directions
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Observational evidence for Observational evidence for black holesblack holes
Early X-ray observations [1965] discovered a powerful X-ray source in Cygnus
Cygnus X-1– Binary star system… black
hole in orbit around a massive O-star
– Black hole mass 7-13 M– X-rays produced due to
accretion of stellar wind from O-star
– 2kpc away
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How do we know the black How do we know the black hole mass?hole mass?
Period 5.6 days K = V sin i = 75km/s Newtonian analysis…
– MBH>f– Cyg X-1… f=0.24MBH
Feed in knowledge of i and companion mass… M=7-13Msun
6 “golden” cases with f>3Msun
Brocksopp et al. (1998)
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9A. Ghez (UCLA)
Strong evidence for a 3-4 million solar mass BH at the Galactic Center (closest stellar approach only 40AU!)
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Chandra+VLA image of GC (Baganoff et al. 2001)
X-ray studies of black holesX-ray studies of black holes
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MCG-6-30-15 (Seyfert gal)(LX~1036 W)
3C273 (Quasar)LX ~1038 W
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X-ray “reflection” imprints well-defined features in the spectrum
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Relativistic effects imprint characteristic profile Relativistic effects imprint characteristic profile on the emission line…on the emission line…
Iron line profile inMCG-6-30-15
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16MCG-6-30-15 Suzaku(Miniutti et al. 2006)
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Also see Suzaku results on broad iron lines at this meeting:• MCG-5-23-16 (Reeves et al.)• NGC 3516 (Markowitz et al.)
Systematic surveys of the XMM archive are showing that ~1/2 of type-1 AGN show broad iron lines (largely confirming ASCA results)
MCG-5-23-16 (Dewangan 2003)
NGC2992
IRAS 18325 (Iwasawa 2004)
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19Brenneman & Reynolds (2006)
Assuming no emission from within rms
a>0.987 (formal 90% limit)
XMM analysis of MCG-6-30-15
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Black Hole Quasi-periodic Black Hole Quasi-periodic oscillationsoscillations
High-frequency QPOs– Comparable frequency to
orbital frequency in inner accretion flow
– Often found in pairs with 3:2 ratio
Stable frequencies– probably determined by
gravitational potential– Could be an excellent probe
of the mass and spin!!
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QPO theoryQPO theory Lack of standard QPO
theoretical framework is problem
Global modes of accretion disk– “Diskoseismology”; Wagoner,
Nowak, Kato…– Produce g-, p-, and c-modes– Linear theory… no natural
explanation for 3:2 ratio Resonance model
– Parametric resonance between vertical/radial epicyclic frequencies (Abramowicz & Kluzniak)
– Source of free energy?
Fundamental g-mode (Nowak & Wagoner)Movie by Mike Nowak
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The Future of BH X-ray StudiesThe Future of BH X-ray Studies
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Armitage & Reynolds (2004)
Dynamical timescale variability… probes orbital motions in accretion disk
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Powerful probe of turbulent disk physics. Also, arcs approximately trace test-particle Keplerian orbits in = plane.
Iwasawa et al. (2004)
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Light crossing timescale allows reverberation effects to be studied.
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27Chandra Deep Field
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Constellation-X simulations…Constellation-X simulations…
Simulated 100ks; F2-10=10-12erg/s/cm2 Simulated 1Ms; z=1; F2-10=10-14erg/s/cm2
~4 such source per Con-X field
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Imaging a black holeImaging a black holemm-VLBImm-VLBI
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Imaging a black holeImaging a black holeMicro-arcsecond X-ray Imaging Micro-arcsecond X-ray Imaging
Mission (MAXIM)Mission (MAXIM)
HST (0.1 arcsec)
MAXIM (0.05 -arcsec)
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~20,000 km
Current MAXIM conceptCurrent MAXIM concept
Group and package Primary and Secondary Mirrors as “Periscope” Pairs
•“Easy” Formation Flying (microns)
•All s/c act like thin lenses- Higher Robustness
•Possibility to introduce phase control within one space craft- an x-ray delay line- More Flexibility
•Offers more optimal UV-Plane coverage- Less dependence on Detector Energy Resolution
•Each Module, self contained- Lower Risk.
~500-1000 m Baseline
A scalable MAXIM concept.