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Exact Solutions and Scalar Fields in Gravity - Instituto Avanzado de ...

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SCALAR FIELD DARK MATTER<br />

Tonatiuh Matos, F. Siddhartha Guzmán, L. Arturo Ureña–López<br />

Departamento <strong>de</strong> Física, Centro <strong>de</strong> Investigación y <strong>de</strong> Estudios <strong>Avanzado</strong>s <strong>de</strong>l IPN,<br />

AP 14–740, 07000 México D.F., México.<br />

Dario Núñez<br />

<strong>Instituto</strong> <strong>de</strong> Ciencias Nucleares,<br />

Universidad Nacional Autónoma <strong>de</strong> México,<br />

A.P. 70–543, 04510 México D.F., México.<br />

Abstract<br />

The ma<strong>in</strong> goal of this work is to put the last results of the <strong>Scalar</strong> Field<br />

Dark Matter mo<strong>de</strong>l of the Universe at cosmological <strong>and</strong> at galactic level<br />

<strong>in</strong> a work together. We present the complete solution to the 95% scalar<br />

field cosmological mo<strong>de</strong>l <strong>in</strong> which the dark matter is mo<strong>de</strong>led by a scalar<br />

field with the scalar potential <strong>and</strong> the<br />

dark energy is mo<strong>de</strong>led by a scalar field endowed with the scalar<br />

potential This mo<strong>de</strong>l has only two free<br />

parameters, <strong>and</strong> the equation of state The results of the mo<strong>de</strong>l<br />

are: 1) the f<strong>in</strong>e tun<strong>in</strong>g <strong>and</strong> the cosmic co<strong>in</strong>ci<strong>de</strong>nce problems are ameliorated<br />

for both dark matter <strong>and</strong> dark energy <strong>and</strong> the mo<strong>de</strong>ls agrees<br />

with astronomical observations. 2) The mo<strong>de</strong>l predicts a suppression<br />

of the Mass Power Spectrum for small scales hav<strong>in</strong>g a wave number<br />

where for This last fact<br />

could help to expla<strong>in</strong> the <strong>de</strong>arth of dwarf galaxies <strong>and</strong> the smoothness of<br />

galaxy core halos. 3) From this, all parameters of the scalar dark matter<br />

potential are completely <strong>de</strong>term<strong>in</strong>ed. 4) The dark matter consists<br />

of an ultra-light particle, whose mass is <strong>and</strong> all<br />

the success of the st<strong>and</strong>ard cold dark matter mo<strong>de</strong>l is recovered. 5) If<br />

the scale of renormalization of the mo<strong>de</strong>l is of or<strong>de</strong>r of the Planck Mass,<br />

then the scalar field can be a reliable mo<strong>de</strong>l for dark matter <strong>in</strong> galaxies.<br />

6) The predicted scatter<strong>in</strong>g cross section fits the value required for<br />

self-<strong>in</strong>teract<strong>in</strong>g dark matter. 7) Study<strong>in</strong>g a spherically symmetric fluctuation<br />

of the scalar field <strong>in</strong> cosmos we show that it could be the halo<br />

dark matter <strong>in</strong> galaxies. 8) The local space–time of the fluctuation of<br />

the scalar field conta<strong>in</strong>s a three dimensional space–like hypersurface<br />

with surplus of angle. 9) We also present a mo<strong>de</strong>l for the dark matter <strong>in</strong><br />

the halos of spiral galaxies, we obta<strong>in</strong> that 10) the effective energy <strong>de</strong>nsity<br />

goes like <strong>and</strong> 11) the result<strong>in</strong>g circular velocity profile<br />

<strong>Exact</strong> <strong>Solutions</strong> <strong>and</strong> <strong>Scalar</strong> <strong>Fields</strong> <strong>in</strong> <strong>Gravity</strong>: Recent Developments<br />

Edited by Macias et al., Kluwer Aca<strong>de</strong>mic/Plenum Publishers, New York, 2001<br />

165

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