Difference between revisions of "New oleg"

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will deviate from the standard case ($\rho_{m0}$ is the present value of $\rho_m$).
 
will deviate from the standard case ($\rho_{m0}$ is the present value of $\rho_m$).
  
For this model find dependence of the dark energy density on the scale factor and using the method described in the problem [New_problems#1301_38] express Friedmann equation in terms of the cosmographic parameters $q, j, l, s$
+
For this model find dependence of the dark energy density on the scale factor and using the method described in the problem [[New_problems#1301_38]] express Friedmann equation in terms of the cosmographic parameters $q, j, l, s$
 
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   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>

Revision as of 21:49, 9 April 2015


Problem 1

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Let us consider a very simple model with the following conservation equations: \begin{equation}\label{conserv_Qm} \dot{\rho_{dm}}+3H\rho_{dm}=Q, \end{equation} \begin{equation}\label{conserv_Qe} \dot{\rho_{de}}+3H\rho_{de}(1+w)=-Q, \end{equation} where $Q=3H\delta\rho_{dm}$ is the source of interaction and $w$ is the state equation parameter for dark energy. The positive small coupling constant $\delta$ will eventually characterize how evolution of the matter energy density \begin{equation}\label{rho-m1} \rho_{dm}= \rho_{dm0}a^{-3(1-\delta)}, \end{equation} will deviate from the standard case ($\rho_{m0}$ is the present value of $\rho_m$).

For this model find dependence of the dark energy density on the scale factor and using the method described in the problem New_problems#1301_38 express Friedmann equation in terms of the cosmographic parameters $q, j, l, s$


Problem 2

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Problem 3

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Problem 4

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Problem 5

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Problem 6

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