Types of Inflationary Scenarios  

In General > s.a. 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 ht/05-in [including string cosmology]; Mukhanov ap/05.
@ 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].

(Hyper)Extended Inflation
* Idea: Variable G to get 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 copmology; phenomenology.
* Idea: Use an extra scalar field, and get inflation only in the regions where starts at a large V(); Because of large friction, evolves slowly at first, then faster; Disadvantage: One also gets a cosmological constant, Vmin = eff.
@ 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].

Other Models and Theoretical Issues > s.a. (A)dS-cft; higher-order gravity; general relativity and cosmology; inflation [quantum gravity]; quantum gravity phenomenology.
* And Big Bang: Inflation has been used to try to avoid the initial singularity by giving bounce solutions.
* "Curvaton" model: A second scalar field, the "curvaton", is responsible for the observed inhomogeneity.
* Warm inflation: A picture that takes into account the importance of dissipation and fluctuation to inflationary dynamics.
@ General references: Lyth & Riotto PRP(99); Faraoni PRD(00)gq, IJTP(01)ht/00-in [non-minimal coupling]; Linde JCAP(03)ap-in [closed, > 1].
@ Hybrid inflation: Linde PRD(94); Lazarides a0706-in [followed by modular inflation].
@ Eternal inflation: 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"].
@ 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); Wands ap/07-in [and curvaton].
@ Higher dimensions: Mazumdar PLB(99); Arkani-Hamed et al PRL(03)ht [5D gauge theory]; Madriz & Bellini PLB(04)gq [non-compact Kaluza-Klein].
@ Inflaton potential: Lidsey et al RMP(97) [rev]; Easther & Kinney PRD(03)ap/02 [Monte Carlo reconstruction].
@ From string theory: Kachru et al JCAP(03)ht; Cline ht/05-in [rev]; > s.a. string phenomenology.
@ In brane world: Lidsey & Seery PRD(06)ap/05 [test of holographic inflation]; Tye ht/06 [intro + review]; > s.a. brane cosmology
@ Pre-big bang: Maggiore & Sturani PLB(97) [fine tuning].
@ 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.
@ Stochastic: Matacz PRD(97); Tsamis & Woodard NPB(05) [quantum gravitational]; Tolley & Wyman a0801.
@ From instantons: Linde PRD(99)hp/98 [Coleman-de Luccia instanton in single-field toy model]; > s.a. inflation [and quantum cosmology].
@ 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 ht/06 [without inflaton fields]; Enqvist et al a0706 [MSSM]; Golovnev et al JCAP(08)-a0802 + pw(08)feb [vector-driven inflation]; Boehmer a0804 [dark-spinor-driven]; > s.a. inflation [topological], MOND [TeVeS].
@ Issues: Hawking et al PRD(01)ht/00 [and trace anomaly]; > s.a. Boltzmann Brains; chaos in general relativity; energy conditions; tachyons.

Alternatives > s.a. branes; Ekpyrotic Scenario.
@ References: Hollands & Wald GRG(02)gq, ht/02; Kofman et al JHEP(02)ht [re Hollands & Wald]; Linde ht/02-in [inflation vs ekpyrotic/cyclic]; Brandenberger ht/07-in [from string theory], PT(08)mar [rev].

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