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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, A http:/www.fis.cinvestav.mx/~tmatos. Superstrings Model Braneword
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From Inflation to Galaxies Formation in the Braneword ScenarioTonatiuh 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
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.
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
Scalar Field FluctuationsT. Matos and L. Ureña,Phys. Rev. D63(2001)063506
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
Numerical SimulationsMiguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez, Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav19(2002)5017.
Scalar Field Fluctuation=HaloTonatiuh Matos and F. Siddhartha GuzmanClass. Q. Grav. 17(2000)L9; Tonatiuh Matos, F. Siddhartha Guzman and Dario Nuñez, Phys. Rev. D62(2000)061301(R);
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 >>
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
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
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
Conclusion • The scalar field is a good candidate to be the Dark Matter of the Universe