probing extreme physics with compact objects: black...
TRANSCRIPT
![Page 1: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/1.jpg)
Probing Extreme Physics withProbing Extreme Physics with
Compact Objects:Compact Objects:
Black HolesBlack Holes
Dong Lai
Department of AstronomyCornell University
![Page 2: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/2.jpg)
“Dark Star” Concept: John Michell (1783) Pierre Laplace (1795)
M, REscape velocity:
• Although “correct” answer, derivation/interpretation wrong
![Page 3: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/3.jpg)
“Black Hole” Concept:
• Einstein (1915): General Relativity Gravity is not a force, but rather it manifests as curvature of spacetime caused by matter and energy
• Karl Schwarzschild (1916): The first exact solution to Einstein field equation
The horizon radius (Schwarzschild radius):
Einstein field equation:
• Roy Kerr (1963): Solution for spinning black holes
![Page 4: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/4.jpg)
Astrophysical Black Holes: Kerr Metric
Two parameters: M, a=J/M
![Page 5: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/5.jpg)
Isolated Black Holes are “boring”(unobservable)
![Page 6: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/6.jpg)
Accreting Black Holes
Stellar-mass BHs in binaries
Supermassive BHs in Galaxies
Accreting gas has angular momentum ==> Accretion disk==> Radiation from disk (x-rays) Outflows (jets)
![Page 7: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/7.jpg)
Tidal Disruption of Stars by BH
==> Electromagnetic Flares
BH - Neutron Star Binary Merger ==> (short) GRBs ?
![Page 8: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/8.jpg)
Binary BH Merger
==> Gravitational waves
![Page 9: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/9.jpg)
Black Holes in Astrophysics
Stellar-mass BHs in X-ray BinariesSupermassive BHs in active galaxies Intermediate-mass BHs (ULXs) ?
Tidal disruption of stars
BH/NS or BH/BH mergers
![Page 10: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/10.jpg)
Black Hole Power in Astrophysics
(1) Accretion Power
Binding energy (per unit mass) at ISCO= 5.7% for a=0 42% for a=M
=
Inner-most stable circular orbitrISCO=6M for a=0 =M for a=M
Note: --The above applies to thin (“cold”) disks (radiative efficient disks);--“Radiative Inefficient Disks” (e.g. ADAF), efficiency is smaller…
![Page 11: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/11.jpg)
Black Hole Power in Astrophysics
(2) Spin Power
Extracting spin energy from BH (Penrose Process)
BH area theorem -->
Maximum efficiency of energy extraction =
= 29.3% for a=M
How to do it? Interaction of BH with magnetized plasma (a la pulsar)…Blandford-Znajek (1977)
![Page 12: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/12.jpg)
Blandford-Znajek ProcessInteraction of BH with magnetized plasma (a la pulsar)…
Kip Thorne
![Page 13: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/13.jpg)
Black Hole Power in Astrophysics
(1) Accretion Power
(2) Spin Power
Relative importance ??
![Page 14: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/14.jpg)
![Page 15: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/15.jpg)
Highlight #1: Mass and Spin of BHs
![Page 16: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/16.jpg)
Mass of BHs in X-ray binaries
Well measured for 23 systems
Note: BH mass gap: 2-5 Msun --> implication for supernova ? (O’Connor & Ott 11)
(McClintock et al. 2011)
![Page 17: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/17.jpg)
Mass of Supermassive BHs
McConnell et al. 2011NGC 3842: 9.7x1010MsunNGC 4889: ~1010Msun
![Page 18: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/18.jpg)
Spin of BHs in X-ray Binaries
• Method 1: Continuum Fitting Measure the temperature of the inner disk in thermal state (thin disk) ==> Radius of the inner edge of the disk ==> BH spin
Key assumption: disk inner edge at ISCO (no radiation inside ISCO)
Penna et al. 2011
![Page 19: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/19.jpg)
McClintock et al 2011
BH spin measurement using continuum fitting method
![Page 20: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/20.jpg)
Spin of BHs
• Method 2: Broad Fe K line shape
Fabian et al 2000
Miniutti et al 2007
MGC-6-30-15: a>0.989 (?)
![Page 21: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/21.jpg)
Evidence for jet powered by BH Spin ?
Narayan & McClintock ‘11
![Page 22: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/22.jpg)
![Page 23: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/23.jpg)
Highlight #2:Rapid Variabilities of Accreting BHs andDynamics of Inner Disks
![Page 24: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/24.jpg)
Remillard & McClintock 2006
High-Frequency QPOs in BH X-Ray Binaries
![Page 25: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/25.jpg)
Basic Facts about HFQPOs
• 40-450 Hz: ~ orbital frequency at risco
• Frequency stable (<10% change when Mdot doubles)
• Some systems: ~2:3 ratio
• Weak QPOs: ~1% flux variation (in hard X-rays), Q~2-10
• Only occur in “Transitional state” (Episodic jet)
![Page 26: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/26.jpg)
X-ray QPO (P ~ 1 hr) from active galaxy RE J1034+396
Gierlinski et al 2008, Nature
![Page 27: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/27.jpg)
QPOs from Ultra-Luminous X-ray Source NGC 5408 X-1(an Intermediate-mass BH?)
Strohmayer & Mushotzky 2009
![Page 28: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/28.jpg)
Remillard & McClintock 2006
High-Frequency QPOs in BH X-Ray Binaries
![Page 29: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/29.jpg)
Ideas/Models of HFQPOs• Orbiting blobs (hot spots) in disks (Stella et al ‘99; Schnittman & Bertschinger ‘04)
• Nonlinear resonances of some kind (Abramowicz, Kluzniak, Horak, Rebusco)
• Acoustic modes in torus (Rezzolla el al ‘03; Lee, Abramowicz & Kluzniak ‘04; Blaes et al. ‘07; Sramkova et al ‘07; Horak’08)
• Disk/Magnetosphere Boundary Layer Oscilations (Li & Narayan ‘04; Tsang & DL ‘09)
• Oscillation modes in relativistic disks (Kato; Wagoner & collaborators)
-- m=0 inertial modes excited by global disk deformation (e.g. warps) (Kato ‘03,’08; Ferreira & Ogilvie ‘08; Henisey et al.10)
-- Rossby modes trapped in special region of a magnetic disk (Tagger & Varniere ‘06; see also Tagger & Pallet ‘99; Varniere & Tagger’02)
-- Cornell effort: Mode growth due to corotational resonance, magnetic fields (DL & Tsang ‘09; Tsang & DL ‘08,’09a,b; Fu & DL ‘09,’11a,b)
![Page 30: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/30.jpg)
P-modes of BH Accretion Disks“inertial-acoustic modes”, “spiral density modes” - -Trapped (partially) in the innermost region of disk
-- Frequencies can be calculated: robust, agree with observations
-- Can grow due to corotation resonance (“corotational instability”)
GR plays an important role
-- B field effect
with David Tsang (Cornell Ph.D. 09 --> Caltech) Wen Fu (Cornell Ph.D. student)
References: DL & Tsang 2009; Tsang & DL 2008, 2009; Fu & DL 2009,2011 Fu & DL 2012
![Page 31: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/31.jpg)
Waves in 2D disks (Spiral density waves):
Lindblad Resonances:
Can propagate only in the region:
where
![Page 32: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/32.jpg)
Wave propagation diagram (effective potential)
![Page 33: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/33.jpg)
Super-reflection
![Page 34: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/34.jpg)
![Page 35: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/35.jpg)
Even more interesting…
Corotation resonance, where
![Page 36: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/36.jpg)
Wave absorption at corotation
Can have both signs !
![Page 37: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/37.jpg)
Calculations of reflectivity/transmission:
• Solve wave equation in different regions
• Match the solutions using asymptotic expansions
• Around corotation: Whittaker function; Stokes phenomenon
Tsang & DL
![Page 38: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/38.jpg)
Reflectivity at ILR: Sign depends on sign of
(vortensity)
![Page 39: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/39.jpg)
Reflectivity at ILR: Sign depends on sign of
(vortensity)
![Page 40: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/40.jpg)
Reflectivity at ILR: Sign depends on sign of
(vortensity)
![Page 41: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/41.jpg)
Overstable mode
Damped mode
Reflectivity at ILR: Sign depends on sign of
(vortensity)
![Page 42: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/42.jpg)
General Relativity Effect
ISCO
Vortensity
GR makes in the Inner-most disk region==> makes the mode grow !
![Page 43: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/43.jpg)
DL & Tsang 2009,2010
Linear Mode Calculation (Mode freq. and growth rate)
![Page 44: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/44.jpg)
Nonlinear Simulation (2D) of Growing Modes
Wen Fu & DL 2012, in prep
![Page 45: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/45.jpg)
Properties of Overstable Disk P-Modes:
Low-order p-modes trapped between inner disk edge and ILR
Grow due to corotation resonance (GR plays important role)
and inner BC
• Mode frequencies robust, consistent with known BH mass (and spin)• Frequency ratio approximately: 1:2:3:4… (not exactly)
A promising candidate for HFQPOs
![Page 46: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/46.jpg)
Complications…
![Page 47: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/47.jpg)
Complications…• Mode damping due to radial infall Competition: mode growth (due to corotation) and damping ==> HFQPOs do not always appear e.g. in thermal state (standard thin disk) no QPOs observed
• Effects of magnetic fields
-- Mode frequencies are slightly affected-- Large-scale B field enhances the growth rate
![Page 48: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/48.jpg)
Disks threaded by large-scale poloidal magnetic fields (embedded in a corona)
-- Increase the p-mode growth rate due to corotation resonance Disk + Corona (coupled by B field) oscillate together,
the “clock” is mainly set by disk
![Page 49: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/49.jpg)
Disks threaded by large-scale poloidal magnetic fields (embedded in a corona)
-- Increase the p-mode growth rate due to corotation resonance Disk + Corona (coupled by B field) oscillate together,
the “clock” is mainly set by disk
-- Such large-scale field is ideal for producing jets/outflows QPOs are observed at the same time as episodic jets
![Page 50: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/50.jpg)
Recap of HFQPOs• Intriguing puzzle --- Dynamics of inner-most region of BH accretion disks (No standard models yet)
• P-modes (spiral density modes) partially trapped in the inner-most region of disks is promising candidate:
-- Frequencies can be calculated from first principle, robust, agree with observations (consistent mass, spin)
-- Can grow naturally due to corotation resonance (GR important)
Incomplete: Complications, other issues (turbulence)…
![Page 51: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/51.jpg)
![Page 52: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/52.jpg)
Highlight #3:Merging Binary Black Holes/Neutron Stars
![Page 53: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/53.jpg)
Merging Neutron Stars:
Taylor & Weisberg 2005
Nobel Prize 1993
![Page 54: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/54.jpg)
Shibata et al. 2006
NS-NS Merger
![Page 55: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/55.jpg)
F. Foucart et al (Cornell) 2011
BH-NS Merger
![Page 56: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/56.jpg)
Merging NSs (NS/BH or NS/NS) as CentralEngine of (short/hard) GRBs
![Page 57: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/57.jpg)
The last few minutes: Gravitational Waveform
![Page 58: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/58.jpg)
Gravitational Waves• Warpage of Spacetime• Generated by time-dependent quadrupoles• Detector response to passage of GWs:
![Page 59: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/59.jpg)
Kip Thorne
Gravitational Wave Interferometer
![Page 60: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/60.jpg)
![Page 61: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/61.jpg)
Final merger wave form probes NS EOS
![Page 62: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/62.jpg)
Probe NS EOS using Inspiral Waveform
Idea:
• For point masses, the number of GW cycles is known exactly
• Rosonant tidal excitations of NS oscillation modes during inspiral ==> transfer orbital energy to NS ==> Missing GW cycles
![Page 63: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/63.jpg)
Resonant Excitations of NS Modes During Binary InspiralNon-rotating NS:
G-mode (Reisenegger & Goldreich 1994; DL 1994)Rotating NS:
G-mode, F-mode, R-mode (Wynn Ho & DL 1999)Inertial modes (DL & Yanqin Wu 2006)R-mode (excited by gravitomagnetic force; Racine & Flanagan 2006)
Results:• For R=10 km NS, the number of missing cycles < 0.1, unlikely measurable (unless NS is rapidly rotating)• Number of missing cycles Important for larger NS• Crustal modes: important? Could shatter crust, pre-cursor of short GRB (D. Tsang et al. 2011)
![Page 64: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/64.jpg)
BH-BH Merger
Cornell-Caltech collaboration
![Page 65: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/65.jpg)
Summary• Compact Objects (White dwarfs, Neutron stars and Black Holes) have diverse observational manifestations can be studied in many different ways: radio -- gamma rays, GWs
• They present a rich set of astrophysics/physics problems Ideal laboratory for probing physics under extreme conditions
![Page 66: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/66.jpg)
Obrigado !!
![Page 67: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/67.jpg)
![Page 68: Probing Extreme Physics with Compact Objects: Black Holeshosting.astro.cornell.edu/~dong/talks/brazil-part2.pdf• Compact Objects (White dwarfs, Neutron stars and Black Holes) have](https://reader033.vdocument.in/reader033/viewer/2022042406/5f20831cd1f3a157d65afc2b/html5/thumbnails/68.jpg)
Black Hole Power in Astrophysics
Accretion Power
“Spin” Power
Binding energy (per unit mass) at ISCO= 5.7% for a=0 42% for a=M
=
Inner-most stable circular orbitrISCO=6M for a=0 =M for a=M
Extracting spin energy from BH (Penrose)
BH area theorem -->
Maximum efficiency of energy extraction = = 29.3% for a=M