Andreas Ringwald Astroteilchenseminar Max-Planck-Institut für Kernphysik Heidelberg, D 13 November 2017 Unifying Inflation with the Axion, Dark Matter, Baryogenesis, and the Seesaw Mechanism. [Guillermo Ballesteros, Javier Redondo, AR, Carlos Tamarit, 1608.05414; 1610.01639]
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Andreas Ringwald
AstroteilchenseminarMax-Planck-Institut für KernphysikHeidelberg, D 13 November 2017
Unifying Inflation with the Axion, Dark Matter, Baryogenesis, and
the Seesaw Mechanism.
[Guillermo Ballesteros, Javier Redondo, AR, Carlos Tamarit, 1608.05414; 1610.01639]
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 particleswith remarkable accuracy
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 particleswith remarkable accuracy
> Big fundamental problems in par-ticle physics and cosmology seemto 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 4
Fundamental Problems > Standard Model (SM) describes
interactions of all known particleswith remarkable accuracy
> Big fundamental problems in par-ticle physics and cosmology seemto 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 5
> Topological theta termviolates P and T, and thus CP
> Most sensitive probe of P and T violation in flavor conserving interactions: electric dipolemoment of neutron; prediction:
> Experiment:
/ Gaµ⌫G̃
a,µ⌫ / Ea ·Ba
[Baker et al. 06]
[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 10
Axionic Solution of Strong CP Problem
> Peccei-Quinn (PQ) solution of strong CP problem based on observationthat the vacuum energy in QCD, inferred from chiral effective fieldtheory, 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 11
Axionic Solution of Strong CP Problem
> Peccei-Quinn (PQ) solution of strong CP problem based on observationthat the vacuum energy in QCD, inferred from chiral effective fieldtheory, has localised minimum at :
> If were a dynamical field, its vev would be zero
> Add to SM angular field , respecting a shift symmetryaaaaaaaaaaaaaa , broken only by coupling to topological charge,
§ Can eliminate by shift ; effective potential pre-dicts vanishing vev, , i.e. P, T, and CP conserved
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
> Non-minimal couplings stretch scalar potential in Einstein frame; makesit convex and asymptotically flat at large field values
[Fairbairn,Hogan,Marsh `14]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 17
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
> Non-minimal couplings stretch scalar potential in Einstein frame; makesit convex and asymptotically flat at large field values
> Potential has valleys = attractors for Higgs Inflation (HI), Hidden ScalarInflation (HSI) or mixed Higgs Hidden Scalar Inflation (HHSI), depen-ding on relative signs of
[Ballesteros,Redondo, AR,Tamarit, 1610.01639]
[Fairbairn,Hogan,Marsh `14]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 18
§ For BH lighter than 10^7 solar masses, accretion can not replenishspin
> Existence of bosonic WISPs leads to gaps in mass vs. spinplots of rapidly rotating BHs
> Stellar BH spin measurementsexclude
[Arvanitaki et al. 14]
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
> In post-inflationary PQ breaking scenario:
> Exploiting results from field theoretic lattice simulations, updated to latestdetermination of topological susceptibility, and artificially separating
find
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
[Hiramatsu et al. 11,12,13; Kawasaki,Saikawa,Segikuchi 15;Borsanyi et al. 16;Ballesteros et al. 16]
[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 thelong range PQ field ( ) becomeless important relative to stringevolution under tension ( )
> For , string behavior shouldapproach that of infinitely thin, i.e. localNambu-Goto strings [Klaer,Moore `17]
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
> For , string‘s interactions with thelong range PQ field ( ) becomeless important relative to stringevolution under tension ( )
> For , string behavior shouldapproach that of infinitely thin, i.e. localNambu-Goto strings
> New method: exploit UV extension ofPQ field theory, with additional comp-lex scalar and additional local U(1) symmetry,
[Klaer,Moore `17]
Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 52
Back Up: DM Axion Mass in Post-Infl. PQ SB Scenario
> Exploiting lattice results on topologicalsusceptibility of :
> Axion production efficiency smallerthan angle-average of ``realignment'' mechanism
§ Simple sum
double counts
§ Energy in domain walls is the energy of fieldmisalignment, from values