aspen center for physics, february 9, 2017 (ucla and kavli ...€¦ · astrophysical black holes....
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Primordial black holes Alexander Kusenko
(UCLA and Kavli IPMU)
Aspen Center for Physics, February 9, 2017
Supported by U.S. DOE Office of Science (HEP)
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Astrophysical black holes
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Primordial black holes● Can be produced in the early universe● Can account for dark matter. (The only dark matter candidate that
is not necessarily made of new particles.)
● Can seed supermassive black holes● Can contribute to the LIGO signal
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Bounds on PBH = all DMNote:
● NS bounds should be ignored
(no DM in globular clusters)
● CMB bounds challenged
[Bird, Cholis et al.,
arXiv:1603.00464]
● Fig. from Niikura et al.,
arxiv:1701.02151
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Black holes Schwarzschild radius: R= 2GM = 3 (M/M
☉) km
Density: ⍴=1018(M☉
/M)2 g/cm3
A large density is required to form a black hole.
CMB: early universe was very uniform. Rare small fluctuations
not sufficient
Gravity can increase the density: structure growth.
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Primordial black hole formation● Spectrum of primordial density perturbations may not be scale invariant and may
have an extra power on some scale: PBH are produced when the corresponding
modes (re)enter horizon.
● The above, plus a matter domination epoch, during which the perturbations grow.
● Violent events, such as phase transitions
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Early Universe
radiation dominated
structures don’t grow
Inflation
origin of primordial perturbatinos
matter dominated
structures grow
modern era(dark energydominated)
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Inflation: density perturbations
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Jeans instabilityIf an overdensity is to collapse, it has to be larger than the crossing time
of the speed of sound on the dynamical time scale:
L > (speed of sound) ⨉ (dynamical time scale)
For radiation dominated epoch,
so that speed of sound
Dynamical time scale:
This means L > (⅓) (horizon size)
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Size of a perturbationGaussian fluctuation of mass M: ε(M)
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Primordial black holes scenarios: use inflation
Kawasaki, AK, Tada, YanagidaarXiv:1606.07631
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Primordial black holes scenarios: use inflation
Kawasaki, AK, Tada, YanagidaarXiv:1606.0763
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Primordial black holes scenarios: use inflation
Kawasaki, AK, Tada, YanagidaarXiv:1606.07631
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Supersymmetry (and other scalar fields)● SUSY is a very well motivated symmetry beyond Standard Model
● SUSY predicts many scalar fields: squarks and sleptons
● At the end of inflation, these fields form a coherent condensate, which can play a
role in generating the matter-antimatter asymmetry of the universe
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Scalar fields in de Sitter space during inflationA scalar with a small mass develops a VEV (for low- k modes, averaged over superhorizon scales). [Bunch,
Davies; Linde; Starobinsky; Vilenkin, Gibbons, Hawking; Lee, Weinberg; Starobinsky, Yokoyama]
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Scalar fields in de Sitter space during inflation
● If m=0, V=0, the field performs random walk:
● Massive, non-interacting field:
●
● Standard Model Higgs:
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Supersymmetry and Q-balls● SUSY predicts many scalar fields: squarks and sleptons
● At the end of inflation, these fields form a coherent condensate
● Condensate unstable: breaks into Q-balls
AK 1997; AK, Shaposhnikov 1998;...
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Numerical simulations of fragmentation
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Fragmentation as pattern formation
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Early Universe
radiation dominated
structures don’t grow
Inflation
origin of primordial perturbatinos
matter dominated
structures grow
modern era(dark energydominated)
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SUSY Q-ball formation can lead to PBHsIntermittent matter
dominated epoch
allows for growth of
structure
[Cotner, AK]
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SUSY Q-ball formation can lead to PBHsparameter space for
PBH = all DM
[Cotner, AK]
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Conclusion● PBH can form in the early universe● Sizes can span a broad range; abundance can vary
○ Can account for all or part of DM○ Can seed supermassive black holes○ Can account for some part of LIGO events