From Inflation to Galaxies Formation in the Braneword Scenario Tonatiuh Matos, Miguel Alcubierre,...
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Transcript of From Inflation to Galaxies Formation in the Braneword Scenario Tonatiuh Matos, Miguel Alcubierre,...
![Page 1: From Inflation to Galaxies Formation in the Braneword Scenario Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, Hugo Compean, F. Siddhartha.](https://reader030.fdocuments.in/reader030/viewer/2022032702/56649cc95503460f94991292/html5/thumbnails/1.jpg)
From Inflation to Galaxies Formation in the Braneword Scenario
Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, Hugo Compean,
F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal,
Ahttp:/www.fis.cinvestav.mx/~tmatos
• Superstrings Model • Braneword • Inflation DM• SnIa• Mass Power Spectrum• Angular Power Spectrum• Galaxies Formation
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The ModelT. Matos, H. Compean, R. Cordero, in preparation.
• Braneword Scenario:• The radion must be stabilized• Superstrings • V f1exp() + f2exp(-) + …
• V = V0[cosh() – 1] exp()
• H2 = 8/(3Mpl2) (1 + /b)
• Inflation graceful exit• BBN Cosmology • Fix the free constants.
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The CosmologyT. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75
• Dark Matter:•
• V0[cosh() –1]
• Dark Energy:•
• Baryons, • Neutrinos, etc.
0.25
0.7
b 0.05
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Scalar Field Fluctuations
T. Matos and L. Ureña, Phys. Rev. D63(2001)063506
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Results:
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Natural Cut-off
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Summarizing
• SFDM model is insensitive to initial conditions
• Behaves as CDM
• Reproduces all the successes CDM above galactic scales.
• Predicts a sharp cut-off in the mass power spectrum
• The favored values for the two free parameters 20 V0 (310-27 Mpl )4 m 10-23 eV
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Numerical SimulationsMiguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez,
Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav 19(2002)5017.
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Oscillatons
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Scalar Field Fluctuation=HaloTonatiuh Matos and F. Siddhartha Guzman Class. Q. Grav. 17(2000)L9;
Tonatiuh Matos, F. Siddhartha Guzman and Dario Nuñez, Phys. Rev. D62(2000)061301(R);
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The Newtonian Force
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WIMPs• Density profile in Galaxies
(r) r as r 0• Numerical Simulations -1.5 NFW(r)1/r 1/(r+b)2
• Observations - 0.5 - 0
• Number of Dwarf Galaxies >>
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Dwarf Galaxies
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The Critical MassTonatiuh Matos and F. Siddhartha Guzman, Class.Q. Grav. 18(2001)5055
• M 0.1 M2Planck /m
• If m 10-23 eV
• M 1012 Mo
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Perfil de densidad
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Galaxy Formation at z=7
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Metalicity in z=2
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Scalar Field DM Cross SectionTonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246.
• cosh is renormalizable
• SFDM 22/ m = 82exp(I2)/[64(m)3]
• Reparametrizations factor = exp[2o2/(322)]
• Internal Contraction I 1/(162)
• If 2 MPl
22/ m = 10-25 - 10-23 cm2/GeV
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The Inflaton as SFDMJames Lidsey, Tonatiuh Matos and Luis A. Ureña, Phys.Rev.,D66(2002)023514.
• Braneworld scenario: H2 = 8/(3Mpl2) (1 + /b)
b 2.881051GeV4
• V V0exp((8)/ Mpl)
• i 1.94 Mpl Vi 1.631056GeV4
end 1.90 Mpl Vend 2.331054GeV4
• Mpbh 109 Mpl tevap 10-16 s 0 10-18
Einst < 1.80 Mpl Einst. << b
pbh > 1.06 Mpl
exp > 0.01 Mpl
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Conclusion
• The scalar field is a good candidate to be the Dark Matter of the
Universe