Types of Inflationary Scenarios |
In General
> s.a. cosmological models [variants and alternatives to inflation];
general-relativistic cosmology; quintessence.
* Types of fields: Conformally coupled
fields tend not to drive inflation; A cosmological constant does drive (exponential) inflation.
* GUT-era inflation:
The first type of scenario; Inflation occurs because of a symmetry breaking
phase transition related to a Higgs field; In the original proposal, the universe
cools down to a false (metastable) vacuum, from which it eventually tunnels out;
In the new inflation, the effective potential for the Higgs field is very flat near
the old vacuum, and inflation occurs not because the universe is stuck in a
false vacuum, but because it spends time rolling down the potential.
@ Reviews: Kolb PRP(93);
Linde JPCS(05)ht [including string cosmology];
Mukhanov ap/05;
Baumann & McAllister 15-a1404 [and string theory].
@ General references:
Lyth & Riotto PRP(99);
Linde JCAP(03)ap-in [closed, Ω > 1];
Weinberg PRD(10)-a0911 [in asymptotically safe theories of gravity];
Martin et al PRD(11)-a1009 [Bayesian evidence for the best model];
Maleknejad et al PRP(13)-a1212 [role of gauge fields];
Martin et al PDU-a1303 [comparison of predictions];
Martin et al JCAP(14)-a1312,
Martin a1312-conf [ranking of scenarios based on Planck data];
Baumann et al JCAP(15)-a1407 [using B-modes];
Pieroni a1611-PhD [classification of inflationary models];
Gomes et al PRD(18)-a1803.
@ Original models: Guth PRD(81);
Linde PLB(82),
Albrecht & Steinhardt PRL(82) [new inflation].
Double Inflation
* Motivation:
Was introduced to decouple large and small-scale density perturbations.
@ References: Silk & Turner PRD(87);
Parkinson et al PRD(05) [testing with WMAP].
Eternal Inflation
> s.a. inflation [and no-boundary wave function]; multiverse.
* Idea: The term describes
a number of different scenarios, classified by Winitzki; The usual one
predicts that the observable universe is inside a bubble embedded in a vast
multiverse, most of which is still undergoing super-accelerated expansion,
a de Sitter background in which pocket universes nucleate at a steady rate.
@ References:
Vilenkin PRD(92) [need for a beginning];
Borde & Vilenkin PRL(94) [initial singularity];
Garriga et al PRD(99)ap/98,
Vilenkin IJTP(99)ht/98 [open universes and anthropic principle];
Guth in(01)ap/03;
Bousso et al PRD(06)ht;
Mersini-Houghton & Parker a0705 ["expensive"];
Winitzki 08;
Aguirre & Johnson RPP(11)-a0908 [observability of bubble collisions];
Ellis & Stoeger GRG(09)-a1001;
Sekino et al PRD(10)-a1003 [topological phases];
Linde & Noorbala JCAP(10)-a1006 [probability measures];
Feeney et al PRL(11)-a1012,
PRD(11)-a1012
+ news ns(10)dec,
bbc(11)aug [cmb observational test of bubble collisions];
Johnson & Lehners PRD(12) [cyclic bubble universes];
Susskind a1205 [is the multiverse past-eternal?];
Mersini-Houghton & Perry CQG-a1211 [not eternal];
Brandenberger et al PRD(15)-a1504 [back-reaction of long-wavelength fluctuations, and termination].
(Hyper)Extended Inflation
* Idea: Assume that
G is variable to get a graceful exit without fine tuning.
@ Extended: La et al PLB(89);
La & Steinhardt PRL(89);
Laycock & Liddle PRD(94).
@ Hyper-extended: Kolb et al PRD(90);
Steinhardt & Accetta PRL(90);
Liddle & Wands PRD(92);
Crittenden & Steinhardt PLB(92).
Chaotic Inflation > s.a. boundary
conditions in quantum cosmology; phenomenology.
* Idea: Use an extra scalar field
φ, and get inflation only in the regions where φ starts at
a large V(φ); Because of the large effective friction, φ
evolves slowly at first, then faster; Disadvantage: One also gets a cosmological constant,
Vmin = Λeff.
@ References: Linde PLB(88);
Linde & Zelnikov PLB(88) [baby universes with fluctuating dimension];
Khalfin IJTP(89) [against];
Susperregi PLB(98) [potentials];
Vilenkin gq/04 [vs eternal, terminology];
Bertolami & Duvvuri PLB(06) [and Chaplygin gas];
Kaloper & Sorbo PRL(09)-a0811;
De Felice et al JCAP(11) [in modified gravitational theories];
Enqvist et al JCAP(12)-a1107 [in non-metric gravity];
Bachlechner et al PRD(15)-a1404.
Other Models
> s.a. (A)dS-cft; inflation [issues];
inflation and planck-scale physics [and quantum gravity];
quantum-gravity phenomenology.
* Starobinski model: A model developed as
a cosmology without singularity in the 1980s, usingan action with leading Einstein term
R, a quantum-gravity motivated R2
term with a huge coefficient, and negligible higher-order terms.
* Warm inflation: A picture that takes
into account the importance of dissipation and fluctuation to inflationary dynamics.
@ Non-minimal couplings: Faraoni PRD(00)gq,
IJTP(01)ht/00-conf;
Pallis PLB(10).
@ Hybrid inflation: Linde PRD(94);
Lazarides IJMPA(07)-a0706-proc [followed by modular inflation].
@ Warm inflation: Bellini CQG(99)gq,
CQG(00)gq/99;
Berera CP(06) [rev].
@ Assisted inflation, multiple scalars:
Liddle et al PRD(98);
Copeland et al PRD(99)ap;
Kanti & Olive PLB(99),
PRD(99) [5D];
Aguirregabiria et al GRG(02)gq/01 [Bianchi VI0];
Wands et al PRD(02)ap [2-field];
Kim & Liddle PRD(06)ap [Nflation, numerical];
Hartong et al CQG(06);
Peterson & Tegmark a1111 [geometric approach to tests];
> s.a. Curvaton.
@ Inflaton potential:
Lidsey et al RMP(97) [rev];
Easther & Kinney PRD(03)ap/02 [Monte Carlo reconstruction];
Grozdanov et al NPB(16)-a1508 [from the exact renormalisation group].
@ Without big bang:
Goldwirth & Piran GRG(91);
Durrer & Laukenmann CQG(96);
Minkevich gq/03,
NPCS(03)gq.
@ In Bianchi models:
Cervantes-Cota CQG(99) [V, Brans-Dicke];
Aguirregabiria et al PRD(00)gq,
GRG(02)gq/01 [assisted],
CQG(04) [I, braneworld];
Chakraborty & Paul PRD(01) [with scalar, no-hair];
Paul PRD(02)gq [brane world];
> s.a. bianchi IX models.
@ Stochastic: Matacz PRD(97);
Tsamis & Woodard NPB(05) [quantum gravitational];
Tolley & Wyman JCAP(08)-a0801;
Kohli & Haslam CQG(15)-a1408 [and general relativity];
Pinol et al a1806 [critical look];
Pattison et al a1905 [beyond slow roll].
@ Natural inflation:
Freese et al PRL(90);
Freese & Kinney PRD(04)hp;
Freese & Kinney JCAP(15)-a1403 [and Planck and BICEP2 data].
@ From instantons: Linde PRD(99)hp/98 [Coleman-de Luccia instanton in single-field toy model];
> s.a. inflation and planck-scale physics [quantum cosmology].
@ Spinor-driven: Böhmer PRD(08)-a0804 [dark spinor];
Barenboim JHEP(09)-a0811 [right-handed neutrino condensate];
Shankaranarayanan IJMPD(09)-a0905-GRF [spinor condensate],
a1002-MG12 [dark spinor].
@ Higgs inflation: Bezrukov CQG(13);
Cook et al PRD(14)-a1403,
Hamada et al PRL(14)-a1403 [and BICEP2 results]
@ Other models:
Damour & Mukhanov PRL(98) [without slow roll];
Borde et al PRL(03)gq/01 [past];
Sami G&C(02) [with oscillations];
Kaloper PLB(04)hp/03 [disformal];
Arkani-Hamed et al JCAP(04)ht/03 [ghost];
González-Díaz & Jiménez-Madrid PLB(04) [phantom, and "big trip"];
Copeland & Rajantie JCAP(05)ap [locked inflation, end];
Boubekeur & Lyth JCAP(05)hp [hilltop inflation];
Barenboim & Lykken PLB(06)ap/05 ["slinky", and dark energy];
Watson et al JCAP(07)ht/06 [without inflaton fields];
Golovnev et al JCAP(08)-a0802
+ pw(08)feb [vector-driven inflation];
Barnaby CJP(09)-a0811-proc [non-local fields];
Biswas & Alexander PRD(09)-a0812 [cyclic];
Germani & Kehagias AIP(10)-a0911 [non-conventional scalar field];
Afshordi et al JCAP(11)-a1006 [with spherical underdense or overdense regions];
Cline et al JCAP(11)-a1106 [chain inflation];
Asselmeyer-Maluga & Król a1301,
AHEP-a1401 [geometric, from exotic smoothness];
Gwyn & Lehners JHEP(14) [supergravity and non-canonical kinetic terms];
Mukhanov FdP(15)-a1409 [extension without self-reproduction];
Fertig et al JCAP(16)-a1507 [conflation, in scalar-tensor theories];
Asaka et al PTEP(16)-a1507 [Starobinski model, from higher dimensions];
> s.a. quantum phase transitions [QCD]; finsler
spacetimes; unimodular gravity; weyl unified theory.
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