New oleg - Revision history

Cosmo All at 22:05, 9 April 2015

2015-04-09T22:05:04Z

2015-04-09T22:03:42Z

2015-04-09T22:02:21Z

2015-04-09T22:00:37Z

2015-04-09T21:53:53Z

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    <div class="NavHead">solution</div>
    <div style="width:100%;" class="NavContent">
-     <p style="text-align: left;"></p>
+     <p style="text-align: left;">We can obtain equation which is expressed only in cosmographical parameters
    </div>
 </div></div>

@@ Line 18: / Line 18: @@
 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 $q, j, l, s$.
 <div class="NavFrame collapsed">
    <div class="NavHead">solution</div>
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 \]
 As we can see when $\beta = 0$ the model reduces to the standard $\Lambda$CDM model.
 <div class="NavFrame collapsed">
    <div class="NavHead">solution</div>

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 \]
 is the age of the Universe up to the redshift $z$.
-For estimation of the model parameters authors of the \cite{Quantum} uses such parametrization of  $H(z)$ in which $T(z) \propto H^{-1}$. Then
+For estimation of the model parameters use such parametrization of  $H(z)$ in which $T(z) \propto H^{-1}$. Then
 \begin{equation}
 \left( \frac{H}{H_0} \right)^2 = \Omega_{\text{m}} + \Omega_{\Lambda_{\text{bare}}} + \frac{\beta }{H_{0}^{2}} H^{2}.

@@ Line 50: / Line 50: @@
-<div id="G-interact-1"></div>
+<div id="G-interact-2"></div>
 <div style="border: 1px solid #AAA; padding:5px;">
 '''Problem 2'''
-<p style= "color: #999;font-size: 11px">problem id: G-interact-1</p>
+<p style= "color: #999;font-size: 11px">problem id: G-interact-2</p>
 Make the same calculations as in the previous problem for model with interaction term $Q=3H\delta\rho_{de}$.
 <div class="NavFrame collapsed">
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-<div id=""></div>
+<div id="G-interact-3"></div>
 <div style="border: 1px solid #AAA; padding:5px;">
 '''Problem 3'''
-<p style= "color: #999;font-size: 11px">problem id: </p>
+<p style= "color: #999;font-size: 11px">problem id: G-interact-3</p>
 <div class="NavFrame collapsed">
    <div class="NavHead">solution</div>

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      <p style="text-align: left;">For model with interaction term $Q=3H\delta\rho_{de}$ the equivalent Friedmann equation expressed in cosmographic parameters has the form:
 \begin{equation}\label{fridman_Q_rde}
-+3(w+\delta)=-2(j-3q(1+w+\delta)),
++3(w+\delta)=-2(j-3q(1+w+\delta)).
 \end{equation}
 And coupling constant $\delta$
 \begin{equation}\label{delta-rde}

@@ Line 32: / Line 32: @@
      H^2=\frac 13\left(\rho_{de0} a^{-3(1+w)}-\frac{a^{-3(1-\delta)}\delta\rho_{dm0}}{w+\delta}+\rho_{dm0}a^{-3(1-\delta)} \right).
 \end{equation}
-Note that here we consider a flat ($k=0$) Universe. Using the method described in the previous section we can write the equivalent Friedmann equation expressed in cosmographic parameters:
+Note that here we consider a flat ($k=0$) Universe. Using the method described  in the problem [[New_problems#1301_38]] we can write the equivalent Friedmann equation expressed in cosmographic parameters:
 \begin{equation}\label{fridman_Q_rm}
      (1+3w)(3\delta-1)=2(j-3q(1+w-\delta)).