Unifying Inflation with the Axion, Dark Matter, Baryogenesis, and the Seesaw Mechanism.
Andreas Ringwald
Astroteilchenseminar Max-Planck-Institut für Kernphysik Heidelberg, D 13 November 2017
[Guillermo Ballesteros, Javier Redondo, AR, Carlos Tamarit, 1608.05414; 1610.01639] Fundamental Problems
> Standard Model (SM) describes interactions of all known particles with remarkable accuracy
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 2 Fundamental Problems
> Standard Model (SM) describes interactions of all known particles with remarkable accuracy > Big fundamental problems in par- ticle physics and cosmology seem to require new physics § Dark matter § Neutrino masses and mixing § Baryon asymmetry § Inflation § Strong CP problem
[PLANCK]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 3 Fundamental Problems
> Standard Model (SM) describes interactions of all known particles with remarkable accuracy > Big fundamental problems in par- ticle physics and cosmology seem to require new physics § Dark matter § Neutrino masses and mixing § Baryon asymmetry § Inflation § Strong CP problem > These problems may be intertwin- ed in a minimal way, with a solu- tion pointing to a new physics sca- le around [Ballesteros,Redondo,AR,Tamarit, 1608.05414; 1610.01639]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 4 Strong CP Problem
> Most general gauge invariant Lagrangian of QCD:
§ Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 5 Strong CP Problem
> Most general gauge invariant Lagrangian of QCD:
§ Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ]
> Topological theta term Ga G˜a,µ⌫ Ea Ba / µ⌫ / · violates P and T, and thus CP
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 6 Strong CP Problem
> Most general gauge invariant Lagrangian of QCD:
§ Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ]
> Topological theta term Ga G˜a,µ⌫ Ea Ba / µ⌫ / · violates P and T, and thus CP > Most sensitive probe of P and T violation in flavor conserving interactions: electric dipole moment of neutron
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 7 Strong CP Problem
> Most general gauge invariant Lagrangian of QCD:
§ Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ]
> Topological theta term Ga G˜a,µ⌫ Ea Ba / µ⌫ / · violates P and T, and thus CP > Most sensitive probe of P and T violation in flavor conserving interactions: electric dipole moment of neutron; prediction:
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 8 Strong CP Problem
> Most general gauge invariant Lagrangian of QCD:
§ Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ]
> Topological theta term Ga G˜a,µ⌫ Ea Ba / µ⌫ / · violates P and T, and thus CP > Most sensitive probe of P and T violation in flavor conserving interactions: electric dipole moment of neutron; prediction:
> Experiment: [Baker et al. 06]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 9 Axionic Solution of Strong CP Problem
> Peccei-Quinn (PQ) solution of strong CP problem based on observation that the vacuum energy in QCD, inferred from chiral effective field theory, has localised minimum at :
[Di Vecchia,Veneziano `80; Leutwyler,Smilga 92]
[Aguado,Asorey 10]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 10 Axionic Solution of Strong CP Problem
> Peccei-Quinn (PQ) solution of strong CP problem based on observation that the vacuum energy in QCD, inferred from chiral effective field theory, has localised minimum at :
[Di Vecchia,Veneziano `80; Leutwyler,Smilga 92]
> If were a dynamical field, its vev would be zero > Add to SM angular field , respecting a shift symmetry aaaaaaaaaaaaaa , broken only by coupling to topological charge,
§ Can eliminate by shift ; effective potential pre- dicts vanishing vev, , i.e. P, T, and CP conserved [Peccei,Quinn 77] § Particle excitation of A: Nambu-Goldstone boson “axion” [Weinberg 78; Wilczek 78] § Mass
and strength of its interactions with SM controlled by decay constant f A Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 11 Axionic Solution of Strong CP Problem
> Extend SM by singlet complex scalar field featuring global > Symmetry broken by vev, :
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 12 Axionic Solution of Strong CP Problem
> Extend SM by singlet complex scalar field featuring global > Symmetry broken by vev, :
§ Excitation of modulus: (saxion) § Excitation of argument:
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 13 Axionic Solution of Strong CP Problem
> Extend SM by singlet complex scalar field featuring global > Symmetry broken by vev, :
§ Excitation of modulus: (saxion) § Excitation of argument: > Extend particle content further by vector- like quark with chiral assignment of PQ charges (KSVZ) [Kim 79;Shifman,Vainshtein,Zakharov 80]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 14 Axionic Solution of Strong CP Problem
> Extend SM by singlet complex scalar field featuring global > Symmetry broken by vev, :
§ Excitation of modulus: (saxion) § Excitation of argument: > Extend particle content further by vector- like quark with chiral assignment of PQ charges (KSVZ) [Kim 79;Shifman,Vainshtein,Zakharov 80] > Color triangle anomaly induces low ener- gy coupling of in form of term
> term can be eliminated by shift; shifted field has zero vev [Peccei,Quinn 78]
> Particle excitation, axion: [Weinberg 79; Wilczek 79]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 15 Saxion as Inflaton
> Take into account non-minimal coupling of Higgs and PQ field to gravity,
§ Generated anyway radiatively even if set to zero at some scale [Fairbairn,Hogan,Marsh `14] > Non-minimal couplings stretch scalar potential in Einstein frame; makes it convex and asymptotically flat at large field values
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 16 Saxion as Inflaton
> Take into account non-minimal coupling of Higgs and PQ field to gravity,
§ Generated anyway radiatively even if set to zero at some scale [Fairbairn,Hogan,Marsh `14] > Non-minimal couplings stretch scalar potential in Einstein frame; makes it convex and asymptotically flat at large field values > Potential has valleys = attractors for Higgs Inflation (HI), Hidden Scalar Inflation (HSI) or mixed Higgs Hidden Scalar Inflation (HHSI), depen- ding on relative signs of
[Ballesteros,Redondo, AR,Tamarit, 1610.01639] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 17 Saxion as Inflaton
> CMB observables � ��-� ��-� ��-� ��-� ��-� fit by ��-� ��-� ��-� ��-� where ��-�� ��-�� ��-�� ��-�� ��-�� ��-�� ��-� ��-� ��-� ��-� � �� ��� ��� ���
[Ballesteros,Redondo, AR,Tamarit, 1610.01639]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 18 Saxion as Inflaton
> HI requires huge non-minimal � -� coupling of the Higgs: �� ��-� ��-� ��-� -� Perturbative unitarity lost in HI �� > ��-� ��-� ��-� -� No unitarity problem in HSI/HHSI, �� > ��-�� if , since then ��-�� ��-�� ��-�� ��-�� ��-�� ��-� ��-� ��-� ��-� � �� ��� ��� ���
[Ballesteros,Redondo, AR,Tamarit, 1610.01639]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 19 Saxion as Inflaton
> Both in HSI and HHSI with , slow-roll inflation ends at a value of > Inflaton starts to undergo Hubble- damped oscillations in a quartic potential, with Universe expanding as in a radiation-dominated era
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 20 Saxion as Inflaton
> Both in HSI and HHSI with , � slow-roll inflation ends at a value of ��-� ��-� > Inflaton starts to undergo Hubble- ��-� damped oscillations in a quartic ��-� potential, with Universe expanding ��-� as in a radiation-dominated era ��-� > PQ symmetry restored after infla- ��-� tion already in preheating stage ��-� when PQ field undergoes Hubble ��-� damped oscillations in quartic ��-�� potential ��-�� ��-�� �� ���
[Ballesteros,Redondo, AR,Tamarit `16]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 21 Saxion as Inflaton
> Both in HSI and HHSI with , slow-roll inflation ends at a value of ξσ=1
12 -1 > Inflaton starts to undergo Hubble- 10 10 damped oscillations in a quartic 10-2
potential, with Universe expanding 10-3 as in a radiation-dominated era 1011 [GeV]
> PQ symmetry restored after infla- f tion already in preheating stage T when PQ field undergoes Hubble damped oscillations in quartic potential 1010 > Large reheating temperature
§ for mixed PQ scalar/Higgs 102 103 104 105 inflation τ > Axion dark radiation: [Ballesteros,Redondo, AR,Tamarit `16]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 22 Saxion as Inflaton
> Sharp prediction of vs for fixed pivot scale, e.g.
HI
[Ballesteros,Redondo, AR,Tamarit `16]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 23 Saxion as Inflaton
> Sharp prediction of vs for fixed pivot scale, e.g.
CMB-S4 (r=0.01)
[Tamarit] > Can be probed by next generation CMB experiments (e.g. CMB-S4)
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 24 Saxion as Inflaton and Axion as Dark Matter
> After PQ SSB, § Present universe consists of many causally disconnected patches with random initial values of axion field
[Saikawa]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 25 Saxion as Inflaton and Axion as Dark Matter
> After PQ SSB, § Present universe consists of many causally disconnected patches with random initial values of axion field § In any of these regions, axion fro- zen at initial value § Later when , axion field starts to oscillate around zero; behaves like cold dark matter: [Preskill,Wise,Wilczek 83; Abbott,Sikivie 83; Dine,Fischler 83,....] § Naive average over patches, igno- ring inhomogeneities at boundaries
[Borsanyi et al., Nature `16 [1606.0794]]
[Raffelt]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 26 Saxion as Inflaton and Axion as Dark Matter
> After PQ SSB, § Present universe consists of many causally disconnected patches with random initial values of axion field § In any of these regions, axion fro- zen at initial value § Later when , axion field starts to oscillate around zero; behaves like cold dark matter:
[Hiramatsu et al. ] § Naive average over patches, igno- ring inhomogeneities at boundaries
§ Non-negligible inhomogeneities at boundaries: cosmic strings and domain walls [Sikivie `82; Davis `86; Lyth `92] § Axion 100% dark matter, if [Klaer,Moore `17]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 27 Dark-Matter Axion Mass in Post-inflationary PQ SB Scen.
> Current experimental bounds:
10-10
10-11 ORGAN ) -1
10-12 | (GeV γγ
A HAYSTAC 10-13 RBF UF 10-14 KSVZ
Axion Coupling |G ADMX 10-15 QCD Axion CouplingDFSZ
10-16 10-6 10-5 10-4 Axion Mass mA (eV) [AR,Rosenberg,Rybka (RPP) `17 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 28 Dark-Matter Axion Mass in Post-inflationary PQ SB Scen.
> Current experimental bounds vs. prediction:
10-10
10-11 ORGAN ) -1
10-12 | (GeV γγ
A HAYSTAC 10-13 RBF UF 10-14 KSVZ
Axion Coupling |G ADMX 10-15 QCD Axion CouplingDFSZ
10-16 10-6 10-5 10-4 Axion Mass mA (eV) [AR,Rosenberg,Rybka (RPP) `17 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 29 Saxion as Inflaton and Axion as Dark Matter
> Projected experimental sensitivities:
MADMAX
[Caldwell et al. `16 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 30 Saxion as Inflaton and Axion as Dark Matter
> Projected experimental sensitivities vs. prediction:
MADMAX
[Caldwell et al. `16 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 31 Unifying Inflation, Dark Matter, and Seesaw with PQ Field
> Unify symmetry with lepton symmetry: give also the SM leptons and the right-handed neutrinos PQ charges [Shin 88; Dias et al. 14; Ballesteros et al. 16]
SM * Axion * See-saw * Higgs portal inflation [Ballesteros,Redondo, AR,Tamarit, 1608.05414; 1610.01639]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 32 Unifying Inflation, Dark Matter, and Seesaw with PQ Field
> Unify symmetry with lepton symmetry: give also the SM leptons and the right-handed neutrinos PQ charges [Shin 88; Dias et al. 14; Ballesteros et al. 16]
SM * Axion * See-saw * Higgs portal inflation [Ballesteros,Redondo, AR,Tamarit, 1608.05414; 1610.01639]
> Field content suffices to solve five pro- blems in one stroke: 1. Strong CP problem 2. Dark matter 3. Inflation 4. Neutrino masses and mixing 5. Baryogenesis
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 33 Unifying Inflation, Dark Matter, and Seesaw with PQ Field
> Unify symmetry with lepton symmetry: give also the SM leptons and the right-handed neutrinos PQ charges [Shin 88; Dias et al. 14; Ballesteros et al. 16]
SM * Axion * See-saw * Higgs portal inflation [Ballesteros,Redondo, AR,Tamarit, 1608.05414; 1610.01639]
> Field content suffices to solve five pro- blems in one stroke: 1. Strong CP problem 2. Dark matter 3. Inflation 4. Neutrino masses and mixing 5. Baryogenesis
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 34 Unifying Inflation, Dark Matter, and Seesaw with PQ Field
> Unify symmetry with lepton symmetry: give also the SM leptons and the right-handed neutrinos PQ charges [Shin 88; Dias et al. 14; Ballesteros et al. 16]
SM * Axion * See-saw * Higgs portal inflation [Ballesteros,Redondo, AR,Tamarit, 1608.05414; 1610.01639]
> Field content suffices to solve five pro- blems in one stroke: 1. Strong CP problem 2. Dark matter 3. Inflation 4. Neutrino masses and mixing 5. Baryogenesis
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 35 Unifying Inflation, Dark Matter, and Seesaw with PQ Field
> Complete and consistent history of the universe from inflation to now
�� ��
�� ��
� �
-�� -�� -�� -�� -�� �
[Ballesteros,Redondo, AR,Tamarit, 1610.01639] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 36 Towards a GUT SMASH
> In non-SUSY SO(10), gauge coupling unification needs at least one intermediate scale; often discussed SSB chain:
[Di Luzio `11]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 37 Towards a GUT SMASH
> In non-SUSY SO(10), gauge coupling unification needs at least one intermediate scale; often discussed SSB chain: 50
40
30
20
106 109 1012 1015
[Ernst,AR,Tamarit in prep.]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 38 Towards a GUT SMASH
> In non-SUSY SO(10), gauge coupling unification needs at least one intermediate scale; often discussed SSB chain: > Most general Yukawas:
> SSB vevs: > SO(10) GUT automatically featu- res: > Fermion masses/mixing: § Neutrino masses and mixing § Baryogenesis via leptogenesis
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 39 Towards a GUT SMASH
> In non-SUSY SO(10), gauge > PQ symmetry imposed: coupling unification needs at least one intermediate scale; often discussed SSB chain: > Most general Yukawas:
> SSB vevs: > SO(10) GUT automatically featu- res: > Fermion masses/mixing: § Neutrino masses and mixing § Baryogenesis via leptogenesis [Bajc et al. 06; > PQ extension adds Altarelli,Meloni 13; Babu,Khan 15] § Predictivity of fermion masses/mixing § Solution of strong CP problem § Axion dark matter Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 40 Towards a GUT SMASH
> Various models: [Ernst,AR,Tamarit in prep.]
> Axion predictions, taking into account constraints from unification, pro- ton decay, seesaw scale, stellar cooling, superradiance of black holes:
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 41 Axion Dark Matter Direct Detection Experiments
> Upcoming generation of axion dark matter direct detection experiments can probe entire mass range: ��[GeV] 1018 1017 1016 1015 1014 1013 1012 1011 1010 109 108
tuned tuned pre-inf. dominant / subdominant subdominant θi → 0 θi →π
dominant overclosure subdominant post-inf. (NDW = 1) (uncertainty?) post-inf. (NDW = 6) overclosure dominant / subdominant
[Saikawa `17] 10-6 10-5 10-4 10-3 10-2 10-1 1 10 102 103 104 105 ��[μeV]
CASPEr ABRACADABRA ADMX MADMAX BRASS KLASH HAYSTAC ORPHEUS CULTASK ORGAN QUAX
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 42 Summary
> Remarkably simple extension of SM involving just one new dimension- ful scale provides solution of five fundamental problems 1. Neutrino oscillations 2. Baryon asymmetry 3. Dark matter 4. Inflation 5. Non-observation of strong CP violation
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 43 Summary
> Firm predictions in reach of upcoming experiments:
MADMAX
[Caldwell et al. `16 ]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 44 Summary
> Firm predictions in reach of upcoming experiments:
CMB-S4 (r=0.01)
[Ballesteros,Redondo, AR,Tamarit `16]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 45 Outlook
> Variants of SMASH § Embedding into non-supersymmetric SO(10) in progress § Other variants of see-saw mechanism? § Relaxation mechanism to solve naturalness problems (hierarchy problem, cosmological constant problem) inherent to SMASH? > Ultraviolet completion of SMASH including quantum gravity? § Embedding in string theory?
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 46 Back Up: Axion/ALP bounds from BH superradiance
> If ALP Compton wavelength of order black hole size: § Bound states around BH nucleus formed § Occupation numbers grow exponentially by extracting rotational energy and angular momentum from the ergosphere § Forming rotating Bose-Einstein condensate emitting gravitational waves § For BH lighter than 10^7 solar masses, accretion can not replenish spin [Arvanitaki,Dimopoulos,Dubovsky,Kaloper,March- Russell 10] > Existence of bosonic WISPs leads to gaps in mass vs. spin plots of rapidly rotating BHs
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 47 Back Up: Axion/ALP bounds from BH superradiance
> If ALP Compton wavelength of > Stellar BH spin measurements order black hole size: exclude § Bound states around BH nucleus formed § Occupation numbers grow exponentially by extracting rotational energy and angular momentum from the ergosphere § Forming rotating Bose-Einstein condensate emitting gravitational waves [Arvanitaki et al. 14] § For BH lighter than 10^7 solar masses, accretion can not replenish spin > Existence of bosonic WISPs leads to gaps in mass vs. spin plots of rapidly rotating BHs
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 48 Back Up: DM Axion Mass in Post-Infl. PQ SB Scenario
> In post-inflationary PQ breaking scenario: > Exploiting results from field theoretic lattice simulations, updated to latest determination of topological susceptibility, and artificially separating
find [Hiramatsu et al. 11,12,13; Kawasaki,Saikawa,Segikuchi 15; Borsanyi et al. 16; Ballesteros et al. 16]
CDM explained for
> Large uncertainty to account for errors due to extrapolation of string ten- sion , with , from the values affordable in the simulations, , to physical values, > New simulation method allows to simulate at physical string tension [Klaer,Moore `17]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 49 Back Up: DM Axion Mass in Post-Infl. PQ SB Scenario
> For , string‘s interactions with the long range PQ field ( ) become less important relative to string evolution under tension ( ) > For , string behavior should approach that of infinitely thin, i.e. local Nambu-Goto strings [Klaer,Moore `17]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 50 Back Up: DM Axion Mass in Post-Infl. PQ SB Scenario
> For , string‘s interactions with the long range PQ field ( ) become less important relative to string evolution under tension ( ) > For , string behavior should approach that of infinitely thin, i.e. local Nambu-Goto strings [Klaer,Moore `17] > New method: exploit UV extension of PQ field theory, with additional comp- lex scalar and additional local U(1) symmetry,
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 51 Back Up: DM Axion Mass in Post-Infl. PQ SB Scenario
> Exploiting lattice results on topological susceptibility of [Borsanyi et al. `16]:
[Klaer,Moore `17] > Axion production efficiency smaller than angle-average of ``realignment'' mechanism
§ Simple sum
double counts § Energy in domain walls is the energy of field misalignment, from values [Klaer,Moore `17] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 52