Difference between revisions of "Homogeneous Universe"

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[[Category:Dynamics of the Expanding Universe|1]]
 
[[Category:Dynamics of the Expanding Universe|1]]
  
= Homogeneous and isotropic Universe, Hubble’s law =
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=== Problem 2: global isotropy ===
 
=== Problem 2: global isotropy ===
Show that if some spatial distribution is everywhere isotropic then it is also homogeneous. Is the opposite true?.
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Show that if some spatial distribution is everywhere isotropic then it is also homogeneous. Is the opposite true?
 
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     <p style="text-align: left;">Due to isotropy the distribution must coincide in any two points, because they can be transformed to each other by rotation by $180^\circ$ around the middle of the interval connecting them. The opposite is not true.[[#equ1 | see problem]].</p>
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     <p style="text-align: left;">Due to isotropy the distribution must coincide in any two points, because they can be transformed to each other by rotation by $180^\circ$ around the middle of the interval connecting them. The opposite is not true ,see [[#equ1 |the problem on homogeniety vs isotropy]].</p>
 
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=== Problem 3: examples ===
 
=== Problem 3: examples ===
 
What three-dimensional geometrical objects are both homogeneous and isotropic?
 
What three-dimensional geometrical objects are both homogeneous and isotropic?
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=== Problem 4: on Big Bang ===
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=== Problem 4: the Big Bang "explosion"===
 
Why the notion of ''Big Bang'' regarding the early evolution of the Universe should not be treated too literally?
 
Why the notion of ''Big Bang'' regarding the early evolution of the Universe should not be treated too literally?
 
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=== Problem 5: Hubble law Galilean invariance ===
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=== Problem 5: Galilean invariance of the Hubble law ===
 
Show that the Hubble's law is invariant with respect to Galilean transformations.
 
Show that the Hubble's law is invariant with respect to Galilean transformations.
 
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     <p style="text-align: left;">Suppose the Hubble's law holds in the reference frame $K$, in which matter is at rest at the origin. Consider another frame $K'$, with origin at some point $A$, moving with velocity $\vec{v}_{A}$ relative to $K$. The quantities measured in the latter frame are denoted by primes. Then in $K'$ one has $\vec r' = \vec r - {\vec r_A}$ and
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     <p style="text-align: left;">Suppose the Hubble's law holds in the reference frame $K$, in which matter is at rest at the origin. Consider another frame $K'$, with origin at some point $A$, moving with velocity $\boldsymbol{v}_{A}$ relative to $K$. The quantities measured in the latter frame are denoted by primes. Then in $K'$ one has $\boldsymbol r' = \boldsymbol r - {\boldsymbol r_A}$ and
\[\vec v' = \vec v - {\vec v_A}
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\[\boldsymbol v' = \boldsymbol v - {\boldsymbol v_A}
= H\vec r' = H\vec r - H{\vec r_A}
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= H\boldsymbol r' = H\boldsymbol r - H{\boldsymbol r_A}
= H\left( {\vec r - {{\vec r}_A}} \right) = H\vec r'.\]
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= H\left( {\boldsymbol r - {{\boldsymbol r}_A}} \right) = H\boldsymbol r'.\]
 
Therefore the distribution law for velocities in the new frame has the same form with the same value of Hubble's parameter as in the original one.</p>
 
Therefore the distribution law for velocities in the new frame has the same form with the same value of Hubble's parameter as in the original one.</p>
 
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=== Problem 6: Hubble law from homogeniety and isotropy ===
 
=== Problem 6: Hubble law from homogeniety and isotropy ===
 
Show that the Hubble's law represents the only form of expansion compatible with homogeneity and isotropy of the Universe.
 
Show that the Hubble's law represents the only form of expansion compatible with homogeneity and isotropy of the Universe.
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=== Problem 7: homogeniety conservation ===
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=== Problem 7: preservation of homogeniety ===
 
Show that if expansion of the Universe obeys the Hubble's law then the initial homogeneity is conserved for all its subsequent evolution.
 
Show that if expansion of the Universe obeys the Hubble's law then the initial homogeneity is conserved for all its subsequent evolution.
 
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     <p style="text-align: left;">The continuity equation takes the form:
 
     <p style="text-align: left;">The continuity equation takes the form:
 
\[\frac{\partial \rho}{dt}
 
\[\frac{\partial \rho}{dt}
+\mbox{div}\left(\vec v\rho\right) = 0.\]
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+\mbox{div}\left(\boldsymbol v\rho\right) = 0.\]
It follows from the homogeneity of the Universe that $\rho$ can depend on time but it is independent on coordinates, i.e. $\rho  = \rho (t)$. Then in accordance with the Hubble's law  $\vec v = H\vec r$ one obtains
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It follows from the homogeneity of the Universe that $\rho$ can depend on time but it is independent on coordinates, i.e. $\rho  = \rho (t)$. Then in accordance with the Hubble's law  $\boldsymbol v = H\boldsymbol r$ one obtains
\[\text{div}(\rho\vec v)
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\[\text{div}(\rho\boldsymbol v)
= \rho\text{div}(\vec v)
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= \rho\text{div}(\boldsymbol v)
=\rho\text{div}(H\vec r) = 3\rho H.\]
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=\rho\text{div}(H\boldsymbol r) = 3\rho H.\]
Therefore, if the distribution $\rho$ was coordinate independent in some reference frame, then the expansion law $\vec v = H\vec r$ preserves the homogeneity of $\rho$ in all subsequent moments of time. Thus the initial homogeneity is conserved forever.</p>
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Therefore, if the distribution $\rho$ was coordinate independent in some reference frame, then the expansion law $\boldsymbol v = H\boldsymbol r$ preserves the homogeneity of $\rho$ in all subsequent moments of time. Thus the initial homogeneity is conserved forever.</p>
 
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=== Problem 10: age of the Universe ===
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=== Problem 10: the age of the Universe ===
 
Estimate the age of the Universe basing on the observed value of the Hubble's constant (the Hubble time $t_H$).
 
Estimate the age of the Universe basing on the observed value of the Hubble's constant (the Hubble time $t_H$).
 
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=== Problem 11: Olbers' paradox resolution ===
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=== Problem 11: Olbers paradox resolved ===
 
Show that the model of the expanding Universe allows one to eliminate the Olbers' paradox.
 
Show that the model of the expanding Universe allows one to eliminate the Olbers' paradox.
 
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Latest revision as of 01:56, 13 December 2013


Problem 1: homogeniety vs isotropy

Most cosmological models are based on the assumption that the Universe is spatially homogeneous and isotropic. Give examples to show that the two properties do not automatically follow one from the other.


Problem 2: global isotropy

Show that if some spatial distribution is everywhere isotropic then it is also homogeneous. Is the opposite true?


Problem 3: examples

What three-dimensional geometrical objects are both homogeneous and isotropic?


Problem 4: the Big Bang "explosion"

Why the notion of Big Bang regarding the early evolution of the Universe should not be treated too literally?


Problem 5: Galilean invariance of the Hubble law

Show that the Hubble's law is invariant with respect to Galilean transformations.


Problem 6: Hubble law from homogeniety and isotropy

Show that the Hubble's law represents the only form of expansion compatible with homogeneity and isotropy of the Universe.


Problem 7: preservation of homogeniety

Show that if expansion of the Universe obeys the Hubble's law then the initial homogeneity is conserved for all its subsequent evolution.


Problem 8: stationary model of the Universe

In the 1940-ties Bondi, Gold and Hoyle proposed a stationary model of the Universe basing on the generalized cosmological principle, according to which there is no privileged position either in space or in time. The model describes a Universe, in which all global properties and characteristics (density, Hubble parameter and others) remain constant in time. Estimate the rate of matter creation in this model.


Problem 9: Hubble flow and peculiar velocities

Galaxies typically have peculiar (individual) velocities of the order of $V_p \approx 100~\mbox{km/s}.$ Estimate how distant a galaxy should be for its peculiar velocity to be negligible compared to the velocity of Hubble flow $V_H=H_{0}R$.


Problem 10: the age of the Universe

Estimate the age of the Universe basing on the observed value of the Hubble's constant (the Hubble time $t_H$).


Problem 11: Olbers paradox resolved

Show that the model of the expanding Universe allows one to eliminate the Olbers' paradox.