Brane interaction as the origin of inflation
By N. Jones, Horace Stoica, S. Tye. 2002
269 citations recorded by the source corpus.
We reanalyze brane inflation with brane-brane interactions at an angle, which include the special case of brane-anti-brane interaction. If nature is described by a stringy realization of the brane world scenario today (with arbitrary compactification), and if some additional branes were present in the early universe, we find that an inflationary epoch is generically quite natural, ending with a big bang when the last branes collide. In an interesting brane inflationary scenario suggested by generic string model-building, we use the density perturbation observed in the cosmic microwave background and the coupling unification to find that the string scale is comparable to the GUT scale.
Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/a1eb6f19e52e84df03e7c32bcd436a8480283563
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In Astronomy and Astrophysics
- Andrei Linde
- R. Kallosh
- Liam McAllister
- F. Quevedo
- E. Silverstein
- D. Baumann
- S. Kachru
- J. Polchinski
In Instrumentation
In Nuclear and High Energy Physics
Citations in the corpus
- Cosmic strings and superstrings (2009, background): “It is expected that the only objects that will be produced in any significant numbers will be one-dimensional objects in the noncompact dimensions lying entirely within the region of reheating (Jones et al 2002, 2003, Sarangi et al 2002).”
- Towards inflation in string theory (2003, background): “We should mention that there are other proposals which might evade the above problem, such as branes at angles or branes with fluxes, see [14,15,16,17,18].”
- Cosmic string production towards the end of brane inflation (2002, background): “Suppose we have U(N) Chan-Paton bundles on one stack of Dp-branes and U(N + M) Chan-Paton bundles on a second stack of Dp-branes, which is at an angle θ with respect to the first stack.”
- Collisions of cosmic F- and D-strings (2004, background): “These can be produced after inflation [2-7], and in some models they are stable or at least metastable on cosmic time scales [8, 9].”
- Inflation from a tachyon fluid (2002, unknown): “ar X iv :h ep -t h/ 02 04 07 0v 3 ∗mfairbai@ulb.ac.be †mtytgat@ulb.ac.be”