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![Page 1: Quintom Bounce with a Galileon Model Chung-Yuan Christian University, Taiwan & Institute of High Energy Physics, Beijing Based on 1108.0593 Collaborated.](https://reader036.fdocuments.in/reader036/viewer/2022062408/56649e915503460f94b9615f/html5/thumbnails/1.jpg)
Quintom Bounce with a Quintom Bounce with a Galileon ModelGalileon Model
Chung-Yuan Christian University, Taiwan
&
Institute of High Energy Physics, Beijing
Based on 1108.0593
Collaborated with J. Evslin, Y. F. Cai, M. Z. Li, X. M. Zhang
Speaker: Taotao Qiu
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OutlineOutlineWhy Quintom bounce?Quintom bounce of galileon model◦Background◦Perturbation
Conclusionoutlook
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WHY QUINTOM WHY QUINTOM BOUNCE?BOUNCE?
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Problems/constraints from theoretical/observational aspects: (such as BBN,CMB(COBE), etc)
Big Bang
Standard Models of the Early UniverseBig Bang Cosmology vs. Inflation Cosmology
The age of galaxies The redshift of the galactic spectrum
The He abundance The prediction of CMB temperature
Flatness problem Horizon problem
Singularity problem
Monopole problem
Structure formation problem
Inflation
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Problems/constraints from theoretical/observational aspects: (such as BBN,CMB(COBE), etc)
Big Bang
Standard Models of the Early UniverseBig Bang Cosmology vs. Inflation Cosmology
The age of galaxies The redshift of the galactic spectrum
The He abundance The prediction of CMB temperature
Flatness problem Horizon problem
Singularity problem
Monopole problem
Structure formation problem
Inflation
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The Alternatives of The Alternatives of InflationInflation
Pre-big bang ScenarioEkpyrotic ScenarioString gas/Hagedorn Scenario
Non-local SFT ScenarioBouncing Scenario
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Ekpyrotic ModelThe collision of two M branes in 5D gives rise to a nonsingular cyclic universe, and the description of effective field theory in 4D is
1 DE domination2 decelerated expansion3 turnaround4 ekpyrotic contracting phase5 before big crunch6 a singular bounce in 4D7 after big bang8 radiation domination9 matter domination
J. Khoury, B. Ovrut, P. Steinhardt and N. Turok,Phys. Rev. D 64, 123522 (2001)
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Ekpyrotic ModelThe collision of two M branes in 5D gives rise to a nonsingular cyclic universe, and the description of effective field theory in 4D is
1 DE domination2 decelerated expansion3 turnaround4 ekpyrotic contracting phase5 before big crunch6 a singular bounce in 4D7 after big bang8 radiation domination9 matter domination
Failure of effective field theory description, uncertainty involved in perturbations.
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Contraction: Expansion:
BouncingPoint: Nearby:
In order to connect this process to the observable universe (radiation dominant, matter dominant, etc), w goes to above -1
Y. Cai, T. Qiu, Y. Piao, M. Li and X. Zhang, JHEP 0710:071, 2007
(Non-singular) Bounce Cosmology expansioncontraction IR size with Low energy scale
Singularity problem avoided!
( )
Formalism:
So w crosses -1, namely Quintom bounce!
If w>-1 at the beginning, w will cross twice.
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Realization of a Quintom Bounce
As for any kind of matter, which is (1) in 4D classical Einstein Gravity, (2)described by
single simple component (either perfect fluid or single scalar field with lagrangian as
), and (3) coupled minimally to Gravity or other matter, its
Equation of State can never cross the cosmological constant boundary (w=-1).
Quintom realization: No-Go theorem
To realize Quintom, one of the conditions should be violatedi) Double field Quintom bounce:
ii) Single field Quintom bounce with higher derivative term:
Y. Cai, T. Qiu, R. Brandenberger, Y. Piao, X. Zhang, JCAP 0803:013,2008; Y. Cai, T. Qiu, J. Xia, X. Zhang, Phys.Rev.D79:021303,2009.
(also known as Lee-Wick Bounce)
Y. Cai, T. Qiu, R. Brandenberger, X. Zhang, Phys.Rev.D80:023511,2009; J. Karouby, T. Qiu, R. Brandenberger, Phys.Rev.D84:043505,2011.
Bo Feng et al., Phys. Lett. B 607, 35 (2005);A. Vikman, Phys. Rev. D 71, 023515 (2005);Gong-Bo Zhao et al., Phys. Rev. D 72, 123515 (2005);J. Xia, Y. Cai, T. Qiu, G. Zhao and X. Zhang, Int.J.Mod.Phys.D17:1229-1243,2008.
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Galileon Galileon TheoriesTheories
Galileon Models: Lagrangian with higher derivative operator, but the equation of motion remains second order, so the model can have w cross -1 without ghost mode.
Basically 5 kinds of Galileon model:
But can be generalized…
Usually, both of the two cases have more than two DYNAMICAL degrees of freedom, which will contain ghost modes.
Problem with Quintom bounce:
Recently: a kind of Galileon theory has been proposed!
A. Nicolis et al., Phys.Rev.D79:064036,2009;C. Deffayet et al., Phys.Rev.D79:084003,2009.
C. Deffayet et al., arXiv:1103.3260 [hep-th]
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Cosmological Applications of Cosmological Applications of Galileon TheoriesGalileon Theories
Galileon as dark energy models:R. Gannouji,M. Sami, Phys.Rev.D82:024011,2010. A. De Felice, S. Tsujikawa, Phys.Rev.Lett.105:111301,2010. C. Deffayet,O. Pujolas,I. Sawicki, A. Vikman, JCAP 1010:026,2010.
Galileon as inflation and slow expanstion models:P. Creminelli, A. Nicolis, E. Trincherini, JCAP 1011:021,2010.T. Kobayashi,M. Yamaguchi,J. Yokoyama, Phys.Rev.Lett.105:231302,2010. C. Burrage,C. de Rham,D. Seery,A. Tolley, JCAP 1101:014,2011. K. Kamada, T. Kobayashi, M. Yamaguchi, J. Yokoyama, Phys.Rev.D83:083515,2011.Z. Liu, J. Zhang, Y. Piao, arXiv:1105.5713 [astro-ph.CO]
Observational constraints on Galileon models:S. Nesseris,A. De Felice, S. Tsujikawa, Phys.Rev.D82:124054,2010A. Ali,R. Gannouji, M. Sami, Phys.Rev.D82:103015,2010.
Galileon as spherically symmetric models:D. Mota, M. Sandstad,T. Zlosnik, JHEP 1012:051,2010.… … … … … …
Can Galileon be used as bounce models???
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QUINTOM BOUNCE WITH A QUINTOM BOUNCE WITH A GALILEON MODELGALILEON MODEL
BACKGROUNDBACKGROUNDPERTURBATIONPERTURBATION
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Our New Bounce Model with Galileon
The action:
Stress energy tensor:
From which we get energy density and pressure:
which was also used in arXiv: 1007.0027 for “Galileon Genesis”.
where
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Considering , and thus is monotonic increasing, so the first term in H, is always larger than 0.
Solution for Bounce to Happen
So we get one property of the field: evolve as a monotonic function!
In order to have bounce, H must reach 0, so negative branch is chosen.
Reality of square root:
From the Friedmann Equation we get the Hubble parameter:
where
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Asymptotic solution of Our Model
with
Equation of motion:
Hubble parameter:
In contracting phase:
Analysis of the asymptotic behavior when
Terms in EoM has different orders of t inconsistent !
EoM becomes:
inconsistent !inconsistent !
consistent !
The only consistent solution has a radiation dominant behavior!
iii)
I.II. i)
ii)
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Numerical Plots of Our Model (1)Plots of Hubble parameter and scale factor in our model:
Parameter choice:
Bounce can happen naturally in our model around t=30.
Reheating?
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Plots of field and EoS w in our model:
behaves as a monotonic function, and the equation of state is approximately 1/3 (radiation-dominant like) in contracting phase, and cross -1 before bounce in our model.
Numerical Plots of Our Model (2)
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QUINTOM BOUNCE WITH A QUINTOM BOUNCE WITH A GALILEON MODELGALILEON MODEL
BACKGROUNDBACKGROUNDPERTURBATIONPERTURBATION
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Perturbation Theoryy
Theoretical aspects: stability must be guaranteed!
Observational aspects: should obtain a (nearly) scale-invariant power spectrum and small tensor-to-scalar ratio
Why perturbations?
Primordial perturbations provide seeds for structure formation and explains why our current universe is not complete isotropic.
Two constraints for linear perturbations:
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Perturbations of Our Bounce Model
Perturbed metric in ADM form:
Perturbed action:
Gauge: uniform
lapse function
inverse shift vector
Constraint equations:
Solution:
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is positive definite: no ghost instability!is model dependent: have to be checked numerically.
Up to second order
Ghost instability: Gradient instability:
In our model,
There are two kinds of instabilities at linear level:
Stability of Perturbation of Our Model
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Stability of Perturbation of Our Model
Numeric plots for and
Both and are positive all over the bouncing process, and we have which also behaves like radiation!
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Spectrum of Perturbation of Our Model
Blue spectrum inconsistent with observational data!
Equation of motion: set
In radiation dominant phase:
Effective mass
Solution:
like a massless scalar field!
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Mechanism of Getting Scale Invariant Power Spectrum
D. Lyth and D. Wands, Phys.Lett.B524:5-14,2002.
An alternative: Curvaton Mechanism
Curvaton: a light scalar field other than inflaton to produce curvature perturbation.The simplest curvaton model:
Curvature perturbation:
For Gaussian part:
where
The equation of motion:
with
Solution: Power spectrum:
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Curvaton Mechanism in Our Model
Our curvaton action:
The general solution:
Our model: due to the background, in order to have scale invariant power spectrum, curvaton have to couple kinetically to the Galileon field
The equation of motion:
In radiation dominant phase:
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Scale Invariant Power Spectrum from Curvaton
growing constant
constantdecaying
Superhorizon solution:
There are two cases of getting scale invariant power spectrum:
Subhorizon solution:
From matching condition: and are independent of k!
q=2:
q=-4:
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Back reaction of the Curvaton Field
The energy density of :
In contracting phase where the universe is radiation-like:
From the equation of motion:
In order for not to destroy the background evolution: one needs
Question: will the growth of energy density of destroy the process of bounce?
In our case which can produce scale invariant power spectrum:
q=2: Safe from back reaction of q=-4: Needs severe fine-tuning.
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Tensor Perturbation of Our ModelPerturbed metric:
Perturbed action (up to second order):
Expand the tensor perturbation:
Equation of motion:
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Tensor Perturbation of Our Model
In radiation dominant phase:
Solution:
Tensor spectrum:
Spectrun index:
In observable region we have , namely the spectrum is severely suppressed, so the tensor-to-scalar ratio
like a massless scalar field!
Blue spectrum!
WMAP data predicts quite small r, so is consistent with our model!D. Larson et al. [WMAP collaboration], arXiv:1001.4635 [astro-ph.CO].
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Conclusion Bounce needs equation of state w cross -1, namely Quintom Bounce can be in form of galileon, where there are only two
dynamical degrees of freedom and ghost can be eliminated. Quintom bounce in Galileon form:
◦ Background behavior: Radiation-dominant like.◦ Perturbation1: free from instability but cannot provide scale
invariant power spectrum◦ Perturbation2: The way of providing scale-invariant power
spectrum is curvaton. In our model there are two cases. ◦ Perturbation3: The back reaction is small in one case, but the other
case needs fine tuning.◦ Perturbation4: The tensor spectrum is blue and the tensor-to-
scalar ratio is small.
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Outlook
Final state of reheating
Nongaussianities
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Reheating
Through reheating, inflaton decay to matter and radiation after inflation
In galileon cosmology, reheating can help avoid divergenceL. Levasseur, R. Brandenberger, A. Davis, arXiv:1105.5649
In bouncing cosmology, reheating is also important and maybe different from normal inflation
T. Qiu, K. Yang, JCAP 1011:012,2010. Y. Cai, R. Brandenberger, X. Zhang, arXiv:1105.4286
What is the reheating process like of our Galileon bounce model???
Reheating is important in inflationary scenario!
Reheating mechanisms:
The motivation of reheating in our bounce model:
Normal: L. Kofman, A. Linde, A. Starobinsky, Phys.Rev.Lett.73:3195-3198,1994. Geometric: B. Bassett, S. Liberati, Phys.Rev.D58:021302,1998.Curvaton: Bo Feng, Ming-zhe Li, Phys.Lett.B564:169-174,2003. ……
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Non-gaussianities
WMAP-7 data:
Planck data:
E. Komatsu et al., arXiv:1001.4538.
Planck collaboration, astro-ph/0604069.
For canonical single scalar field inflation:X. Chen, M. Huang, S. Kachru, G. Shiu, JCAP 0701:002,2007.
For bounce cosmology: new shape with sizable amplitude and
Y. Cai, W. Xue, R. Brandenberger, X. Zhang, JCAP 0905:011,2009.
Non-Gaussianities is important for 1) meeting the more and more accurate observational data and 2) distinguishing the over models for early universe
Definition:
Observational constraints:
Theoretical results:
What will the non-Gaussianities behave like for our Galileon bounce model???
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THANKS FOR THANKS FOR ATTENTION!ATTENTION!
谢谢!谢谢!
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Galileon genesisGalileon genesis
Our bounce model “Galileon genesis”, 1007.0027