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SUMMARY:Linear inflation from quartic potential
DTSTART;VALUE=DATE-TIME:20160523T130000Z
DTEND;VALUE=DATE-TIME:20160523T132000Z
DTSTAMP;VALUE=DATE-TIME:20240223T010009Z
UID:indico-contribution-336-2869@indico.ific.uv.es
DESCRIPTION:Speakers: Antonio Racioppi (NICPB)\nWe show that if the inflat
on has a non-minimal coupling to gravity and the Planck scale is dynamical
ly generated\, the results of Coleman-Weinberg inflation are confined in b
etween two attractor solutions: quadratic inflation\, which is ruled out b
y the recent measurements\, and linear inflation which\, instead\, is in t
he experimental allowed region. The minimal scenario has only one free par
ameter -- the inflaton's non-minimal coupling to gravity -- that determine
s all physical parameters such as the tensor-to-scalar ratio and the rehea
ting temperature of the Universe. Should the more precise future measureme
nts of inflationary parameters point towards linear inflation\, further in
terest in scale-invariant scenarios would be motivated.\n\nhttps://indico.
ific.uv.es/event/2534/contributions/2869/
LOCATION:
URL:https://indico.ific.uv.es/event/2534/contributions/2869/
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SUMMARY:Do current data prefer a non minimally coupled inflation?
DTSTART;VALUE=DATE-TIME:20160523T142000Z
DTEND;VALUE=DATE-TIME:20160523T144000Z
DTSTAMP;VALUE=DATE-TIME:20240223T010009Z
UID:indico-contribution-336-2850@indico.ific.uv.es
DESCRIPTION:Speakers: Héctor Ramírez Rodríguez (IFIC\, CSIC-Univ Valenc
ia)\nInflation provides the most theoretically attractive and observationa
lly successful cosmological scenario able to generate the initial conditio
ns of our universe. From the theoretical viewpoint\, this picture is usual
ly understood as the dynamics of a single new scalar degree of freedom\, t
he inflaton\, minimally coupled to gravity. However\, generally the inflat
on is expected to have a nonminimal coupling to the Ricci scalar. While th
e minimally-coupled version of the chaotic model of inflation is ruled out
at more than 99% confidence level (for 50 e-folds of inflation)\, in this
talk we will see that the presence of such coupling\, for the chaotic mod
el\, is highly favoured with respect to the latest analysis of Planck and
BICEP2.\n\nhttps://indico.ific.uv.es/event/2534/contributions/2850/
LOCATION:
URL:https://indico.ific.uv.es/event/2534/contributions/2850/
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BEGIN:VEVENT
SUMMARY:D6-branes and axion monodromy inflation
DTSTART;VALUE=DATE-TIME:20160523T134000Z
DTEND;VALUE=DATE-TIME:20160523T140000Z
DTSTAMP;VALUE=DATE-TIME:20240223T010009Z
UID:indico-contribution-336-2826@indico.ific.uv.es
DESCRIPTION:Speakers: Aitor Landete (IFT\, UAM-CSIC)\nWe develop new scena
rios of large field inflation in type IIA string compactifications in whic
h the key ingredient is a D6-brane that generates a bilinear superpotentia
l which couples the brane position modulus to a Kahler modulus\, this allo
ws us to construct two different models where the inflaton candidate could
be the B-field axion or the D6-brane Wilson Line. The scalar potential ha
s the multi-branched structure typical of F-term axion monodromy models an
d\, near its supersymmetric minima\, it is described by a 4d supergravity
model of chaotic inflation with a stabiliser field. \nWe analyse both case
s in the context of type IIA moduli stabilisation\, finding an effective p
otential for the inflaton system and a simple mechanism to lower the infla
ton mass with respect to closed string moduli stabilised by fluxes. \nFina
lly\, we analyze the B-field potential for trans-Planckian field values by
means of the DBI action. The effect of Planck suppressed corrections is a
flattened potential which\, in terms of the compactification parameters\,
interpolates between linear and quadratic inflation. This renders the cos
mological parameters of these models compatible with current experimental
bounds\, with the tensor-to-scalar ratio ranging as 0.08 \n\nhttps://indic
o.ific.uv.es/event/2534/contributions/2826/
LOCATION:
URL:https://indico.ific.uv.es/event/2534/contributions/2826/
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BEGIN:VEVENT
SUMMARY:Inflation from f(R) theory with all possible terms
DTSTART;VALUE=DATE-TIME:20160523T132000Z
DTEND;VALUE=DATE-TIME:20160523T134000Z
DTSTAMP;VALUE=DATE-TIME:20240223T010009Z
UID:indico-contribution-336-2820@indico.ific.uv.es
DESCRIPTION:Speakers: Michal Artymowski (Jagiellonian University)\nIn my t
alk I will present the $f(R) = \\sum _n \\alpha_n R^n$ model with finite a
nd infinite amount of higher order terms. By the assumption of existence o
f one stationary point positioned anywhere at the Einstein frame potential
I will obtain a theory with Starobinsky-like Einstein frame potential\, w
hich will include all $R^n$ terms. I will compare results with the Palnck
data and discuss the stability of the GR vacuum of the model.\n\nhttps://i
ndico.ific.uv.es/event/2534/contributions/2820/
LOCATION:
URL:https://indico.ific.uv.es/event/2534/contributions/2820/
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BEGIN:VEVENT
SUMMARY:Natural Inflation with Hidden Scale Invariance
DTSTART;VALUE=DATE-TIME:20160523T140000Z
DTEND;VALUE=DATE-TIME:20160523T142000Z
DTSTAMP;VALUE=DATE-TIME:20240223T010009Z
UID:indico-contribution-336-2756@indico.ific.uv.es
DESCRIPTION:Speakers: Shelley LIANG (Univ Sydney)\nWe propose a new class
of natural inflation models based on a hidden scale invariance. In a very
generic Wilsonian effective field theory with an arbitrary number of scala
r fields\, which exhibits scale invariance via the dilaton\, the potential
necessarily contains a flat direction in the classical limit. This flat d
irection is lifted by small quantum corrections and inflation is realised
without need for an unnatural fine-tuning. In the conformal limit\, the ef
fective potential becomes linear in the inflaton field\, yielding to speci
fic predictions for the spectral index and the tensor-to-scalar ratio\, be
ing respectively: n_s−1≈−0.025(N⋆/60)−1 and r≈0.0667(N⋆/60)
−1\, where N⋆≈30−65 is a number of e-folds during observable infla
tion. This predictions are in reasonable agreement with cosmological measu
rements. Further improvement of the accuracy of these measurements may tur
n out to be critical in falsifying our scenario. \n\nThe paper is availabl
e under the arXiv number 1602.04901\, and has been accepted by Physics Let
ters B.\n\nhttps://indico.ific.uv.es/event/2534/contributions/2756/
LOCATION:
URL:https://indico.ific.uv.es/event/2534/contributions/2756/
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