some problems in string cosmology miao li institute of theoretical physics academia sinica
Post on 19-Dec-2015
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TRANSCRIPT
Some Problems in String Cosmology
Miao Li
Institute of Theoretical Physics
Academia Sinica
The Challenges from Observational Cosmology
1. Cosmological constant or dark energy
• Strong indication from the Hubble diagram of type Ia supernovae
•Supported by other experiments such as Boomerang, Maxima and WMA
P
2. WMAP Results on CMB
Universe is flat (total density = critical density)
Atoms 4%Dark Matter 23%
Dark Energy (cosmological constant?) 72%
Adiabatic, scale invariant, Gaussian Fluctuations
(Harrison-Zeldovich-Peebles, Inflation)
Best fit model
cosmic variance
Temperature
Temperature-polarization
1 deg
85% of sky
n=0.99
8 = 0.9
bh2 = 0.024
xh2 = 0.126
H0 = 72
= 0.17
The most interesting, yet tentative result is the running the spectral index
There have been many proposals on the nature
of the dark energy, but this is not a subject of
the present talk.
We concentrate on a couple of theoretical
problem associated with the CMB power
spectrum
Strictly, there has been no accurate definition of stringtheory in a time-dependent background when spacetimeis not asymptotically Minkowskian, since in stringtheory the only physical observables are S-matrixelements.String cosmology studies cosmology using either lowenergy effective action or equations of motion withstringy corrections.Motivated by recent observations, string theorists aregetting serious about possible physical effects of short distance physics.
There are at least two schemes which have
attracted considerable attention.
1. Short distance physics set by “boundary conditions” at a cut-off
2. Noncommutative spacetime effects
CMB. of
spectrumpower thegcalculatinby correct
isintuition her thischeck whetcan We
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1. The boundary conditions
This has been considered by many people
including
U. Danielsson, Eather, B. Greene, Kinney,
Shiu, Martin, Brandenberger, Goldstein, Lowe.
And is a controversial issue regarding whether
the correction to CMP power spectrum is of
order .)(H/or H/ 2
0|a
, at time k/a
: off-cut a toequal is
mode thisof size physical when thevacuum
Sitter de ain be k to modegiven a of state
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k
k
))2
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(P
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2k
2k
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2. Noncommutative spacetime
theory.string gfor testinmotion"Brownian "
of kind ofrelation that thisis hope best we The
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A scheme incorporating noncommutativity of
spacetime in the inflation scenario was
proposed by Brandenberger and Ho, we
should not write down the detailed formulas.
The main idea is to modify the relation
between the wave-length of the perturbation
and the creation time of the perturbation.
For the power-law inflation
nltt )/()a(
dlnk
dn ,
dlnk
dlnP(k)1n
defined are running its andindex spectral The
length.-wave
cmacroscopi a is k n, largely sufficient aFor tivity.noncommuta spacetime
todue is termsecond The .on depends k andn on depends where
))/(1()/((k)
have We
ss
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kkkkkl ncn
nc
cm1086.3 cm,1015.2 12,n
parameterswith
modelinflation tivenoncommuta theusing data theseallfit can We
077.0)0.002Mpck(dlnk
dn ,20.1)0.002Mpck(n
,031.0)0.05Mpck(dlnk
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are results WMAPThe
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In conclusion, the noncommutative inflation
model can rather easily explain the WMAP
CMB data, especially the running of the
spectral index. As a comparison, people have
tried to understand these data within the
standard inflation scenario, and found that a
rather contrived and ugly potential of the
inflaton is needed.
Since the WMAP result on the runningspectral index is of only 2-sigma, we still need to wait for the second year results to seewhether there is indeed a large deviation from the scaling invariant spectrum.
We are rather hopeful that the futurecosmology experiments will bring about a lot of excitements, and possible signature of Planck scale physics!