Galaxies, Stars and Black Holes: Formation and Energy Budget
Transcript of Galaxies, Stars and Black Holes: Formation and Energy Budget
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Galaxies, Stars and Black Holes: Formation and Energy Budget
Martin ReesCambridge University
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THE HIGHEST-REDSHIFT QUASARS
Becker et al. (2000)
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He
D
Li
Calculations ofthe primal“cooking” ofthe chemicalelements predict
Hydrogen
Helium
Lithium
etc, correctly!
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OUR UNIVERSE
How did our complex cosmos --with hugecontrasts in density and temperature --emerge from near-uniform conditions atearly times?
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FLUCTUATION AMPLITUDE
˜¯
ˆÁË
Ê D@ -
T
TQ ~10 5
Bound Systems* with GravitationalBinding Energy 2QMc
(Virial Velocity )cQ 21
Max Non-:Linear Scale
Q1/2 x (Hubble Radius).
*Formation of Bound System Requires Expansion Factor of >~ Q-1 After System Enters Horizon.
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AN ANAEMIC UNIVERSE (Q = 10-6)
Small loosely-bound galaxies form later than in ouruniverse; star formation is still possible, butprocessed material is likely to be expelled fromshallow potential wells. There may be no second-generation stars containing heavy elements, and sono planetary systems at all.
If Q were significantly lower than 10-6, then gaswould be unable to cool with a Hubble time.*
In a L-dominated universe, isolated clumps could survive for aninfinite time without merging into a larger scale of hierarchy. Soeventually, for any Q > 10-8, a ‘star’ could form – but by that timethere would be merely one minihalo within the entire event horizon!
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POSSIBLE UNIVERSE WITH Q = 10-4
*perhaps more interesting than ours!
Masses >~ 1014 M� condense at 3.108 yrs into huge discgalaxies with orbital velocity ~2000 km/sec (gas wouldcool efficiently via Compton cooling, leading probablyto efficient star formation).
These would, after 1010 yrs, be in clusters of>~ 1016 M�.
There would be a larger range of non-linear scales thanin our actual universe. Only possible ‘disfavouring’feature is that stellar systems may be too packedtogether to permit unperturbed planetary orbits.
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When did the cosmic dark ageend?
Formation of the first stars in‘minihalos’
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Cosmic Structure Formation-Cartoon
linear perturbation theory nonlinear simulations
Reco
mbi
natio
n
Nucl
eosy
nthe
sis
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GALAXIES
(i) Tracers of large-scale cosmicstructure
(ii)‘Ecosystems’ of the cosmos (with central black holes)
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GRAVITATIONAL ENERGY
In ‘ordinary’ stars, release of gravitational energyis less important than nuclear power (by factor1000).
• But When nuclear energy runs out, a star may contract
so much that more gravitational energy isreleased than ever came from nuclear reactions.
(STARS HAVE NEGATIVE SPECIFIC HEAT!)
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BLACK HOLES
Gravity’s final triumph over all otherforces
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"In my entire scientificlife,... the most shatteringexperience has been therealisation that an exactsolution of Einstein'sequations...... provides theabsolutely exactrepresentation of untoldnumbers of massive blackholes that populate theuniverse" S. Chandrasekhar.
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black hole mass scales with bulge mass
stellar velocity dispersion of the bulge
Kormendy 2003
Is this really tighter?
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XMM
Fabian et al 02
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Chandra
ASTRO-E2
XMM-Newton
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3C31:
OpticalRadio
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Formation and evolution of supermassive binaries
1. Dynamical friction
2. Binary hardening due to stars
or accretion of gas
3. Gravitational radiation
t µ a4
t µ a
Do they merge?
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LISA
Will see mergersof 105 –107 Msol
black holes
2011?
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Lisa sensitivity to massive black hole binaries
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