Difference between revisions of "Homogeneous Universe"

From Universe in Problems
Jump to: navigation, search
(Homogeneous and isotropic Universe, Hubble’s law)
 
(30 intermediate revisions by 3 users not shown)
Line 1: Line 1:
[[Category:Dynamics of the Expanding Universe]]
+
[[Category:Dynamics of the Expanding Universe|1]]
  
= Homogeneous and isotropic Universe, Hubble’s law =
+
<!-- = Homogeneous and isotropic Universe, Hubble’s law = -->
 +
__TOC__
  
<div id="02001"></div>
+
<div id="equ1"></div>
=== Problem 1. ===
+
<div style="border: 1px solid #AAA; padding:5px;">
A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous.
+
=== 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.
 
<div class="NavFrame collapsed">
 
<div class="NavFrame collapsed">
 
   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>
 
   <div style="width:100%;" class="NavContent">
 
   <div style="width:100%;" class="NavContent">
     <p style="text-align: left;"> A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous. </p>
+
     <p style="text-align: left;">A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous.</p>
 
   </div>
 
   </div>
</div>
+
</div></div>
  
<div id="02002"></div>
+
 
=== Problem 2. ===
+
<div id="equ2"></div>
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 [[#Problem_1 | problem #1]]).
+
<div style="border: 1px solid #AAA; padding:5px;">
 +
=== Problem 2: global isotropy ===
 +
Show that if some spatial distribution is everywhere isotropic then it is also homogeneous. Is the opposite true?
 
<div class="NavFrame collapsed">
 
<div class="NavFrame collapsed">
 
   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>
 
   <div style="width:100%;" class="NavContent">
 
   <div style="width:100%;" class="NavContent">
     <p style="text-align: left;"> A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous. </p>
+
     <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>
 
   </div>
 
   </div>
</div>
+
</div></div>
 +
 
  
 +
<div id="equ3"></div>
 +
<div style="border: 1px solid #AAA; padding:5px;">
  
<div id="02003"></div>
+
=== Problem 3: examples ===
=== Problem 3. ===
+
What three-dimensional geometrical objects are both homogeneous and isotropic?
There are three cases: three-dimensional plane (zero curvature), sphere (positive curvature) and hyperboloid (negative curvature).
+
 
<div class="NavFrame collapsed">
 
<div class="NavFrame collapsed">
 
   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>
 
   <div style="width:100%;" class="NavContent">
 
   <div style="width:100%;" class="NavContent">
     <p style="text-align: left;"> A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous. </p>
+
     <p style="text-align: left;">There are three cases: three-dimensional plane (zero curvature), sphere (positive curvature) and hyperboloid (negative curvature).</p>
 
   </div>
 
   </div>
</div>
+
</div></div>
  
  
<div id="02004"></div>
+
<div id="equ4"></div>
=== Problem 4. ===
+
<div style="border: 1px solid #AAA; padding:5px;">
The main qualitative difference from the usual explosion lies in the fact that the explosive charge is usually surrounded by atmospheric air. The expansion is then caused by the difference between the huge pressure of the gaseous products of the explosion and comparatively small pressure of the surrounding air. But when considering the expanding Universe, one assumes that the pressure (according to the cosmological principle) is uniformly distributed too. Therefore there are neither pressure gradients nor forces that could cause or even affect the expansion. The expansion of the Universe itself is the result of initial velocity distribution.
+
=== 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?
 
<div class="NavFrame collapsed">
 
<div class="NavFrame collapsed">
 
   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>
 
   <div style="width:100%;" class="NavContent">
 
   <div style="width:100%;" class="NavContent">
     <p style="text-align: left;"> A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous. </p>
+
     <p style="text-align: left;">The main qualitative difference from the usual explosion lies in the fact that the explosive charge is usually surrounded by atmospheric air. The expansion is then caused by the difference between the huge pressure of the gaseous products of the explosion and comparatively small pressure of the surrounding air. But when considering the expanding Universe, one assumes that the pressure (according to the cosmological principle) is uniformly distributed too. Therefore there are neither pressure gradients nor forces that could cause or even affect the expansion. The expansion of the Universe itself is the result of initial velocity distribution.</p>
 
   </div>
 
   </div>
</div>
+
</div></div>
  
  
<div id="02005"></div>
+
<div id="equ5"></div>
=== Problem 5. ===
+
<div style="border: 1px solid #AAA; padding:5px;">
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 <math>\vec {r}' = \vec {r} - {\vec {r}_A}</math> and
+
=== Problem 5: Galilean invariance of the Hubble law ===
\[\vec {v}' = \vec {v} - {\vec {v}_A}
+
Show that the Hubble's law is invariant with respect to Galilean transformations.
= H\vec r' = H\vec r - H{\vec r_A}
+
= H\left( {\vec r - {{\vec r}_A}} \right) = H\vec r'.\]
+
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.
+
 
<div class="NavFrame collapsed">
 
<div class="NavFrame collapsed">
 
   <div class="NavHead">solution</div>
 
   <div class="NavHead">solution</div>
 
   <div style="width:100%;" class="NavContent">
 
   <div style="width:100%;" class="NavContent">
     <p style="text-align: left;"> A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous. </p>
+
     <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
 +
\[\boldsymbol v' = \boldsymbol v - {\boldsymbol v_A}
 +
= H\boldsymbol r' = H\boldsymbol r - H{\boldsymbol r_A}
 +
= H\left( {\boldsymbol r - {{\boldsymbol r}_A}} \right) = H\boldsymbol r'.\]
 +
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>
 
   </div>
 
   </div>
</div>
+
</div></div>
 
+
 
+
 
+
 
+
{| class="wikitable collapsible collapsed"
+
! '''Problem 1.''' A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous.
+
|-
+
| A system with constant magnetic field is homogeneous but not isotropic, because the direction along the field and perpendicular to it are not equivalent. On the contrary, a spherically symmetric distribution of electric charges is by construction isotropic, but not, in general, homogeneous.
+
|}
+
 
+
  
  
 +
<div id="equ6"></div>
 +
<div style="border: 1px solid #AAA; padding:5px;">
 +
=== 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.
 +
<!-- <div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;"></p>
 +
  </div>
 +
</div> --></div>
  
  
 +
<div id="equ7"></div><div style="border: 1px solid #AAA; padding:5px;">
 +
=== 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.
 +
<div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;">The continuity equation takes the form:
 +
\[\frac{\partial \rho}{dt}
 +
+\mbox{div}\left(\boldsymbol v\rho\right) = 0.\]
 +
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  $\boldsymbol v = H\boldsymbol r$ one obtains
 +
\[\text{div}(\rho\boldsymbol v)
 +
= \rho\text{div}(\boldsymbol v)
 +
=\rho\text{div}(H\boldsymbol r) = 3\rho H.\]
 +
Therefore, if the distribution $\rho$ was coordinate independent in some reference frame, then the expansion law $\boldsymbol v = H\boldsymbol r$ preserves the homogeneity of $\rho$ in all subsequent moments of time. Thus the initial homogeneity is conserved forever.</p>
 +
  </div>
 +
</div></div>
  
  
 +
<div id="equ9"></div><div style="border: 1px solid #AAA; padding:5px;">
 +
=== 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.
 +
<div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;">Constant Hubble's parameter provides exponential expansion of the Universe with $a = {a_0}{e^{Ht}}$. Consider a region of space with initial volume $V_0$  and density $\rho_0$. Then at time $t$ the density in the chosen region is
 +
\[\rho  = \frac{V_{0}\rho _0}{V}
 +
= \frac{V_{0}\rho_{0}}
 +
{\frac{4}{3}\pi a_0^3{e^{3Ht}}}
 +
= {\rho _0}{e^{ - 3Ht}},\]
 +
and one obtains $\dot \rho =  - 3H\rho$. Then to preserve the constant density of the Universe one has to introduce additional density growth rate equal to $3H\rho$. Note that $ H \approx 2 \cdot {10^{-18}\;s^{- 1}}\approx 6\cdot 10^{ - 11} \;\mbox{year}^{-1}$ and
 +
\[3H\rho
 +
\approx 3H\rho _{cr}
 +
\approx 2 \cdot 10^{ - 39}\mbox{ g}
 +
\cdot \mbox{cm}^{-3} \cdot \mbox{ yr}^{-1}
 +
\approx m_p\,\mbox{km}^{- 3}
 +
\cdot \mbox{ yr}^{ - 1},\]
 +
where ${m_p} = 1.67 \cdot {10^{ - 24}}\;\mbox{ g}$. Thus the constancy of the Hubble's parameter along with constant density requires creation "from nothing" of on average one proton in cubic kilometer per year. So, for example, our Earth during its lifetime would have "gained weight" of about $\sim 10^{-2} {\rm g}$.
  
  
 +
Paul Dirac was one of active supporters of cosmological models with matter creation. In regard to his and Hoyle's models he wrote the following: "... Hoyle assumed that the Universe is in a homogeneous and isotropic state, and continuous creation of matter is aimed to supply the substance which leaves the observable zone due to the expansion. The Hoyle's theory sets the quantity $G$ constant, while in mine $G$ changes with time, and it makes the main distinction from the Hoyle's theory. I propose a theory where continuous creation of matter is combined with variable $G$. Both assumptions result from the large numbers' hypothesis".</p>
 +
  </div>
 +
</div></div>
  
  
 +
<div id="equ10"></div><div style="border: 1px solid #AAA; padding:5px;">
 +
=== 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 $V_H=H_{0}R$.
 +
<div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;">From the condition $\frac{V_p}{V_H} \ll 1$ one gets $R \gg \frac{V_p}{H_0} \approx 1.5~\mbox{Mpc}$.</p>
 +
  </div>
 +
</div></div>
  
  
 +
<div id="equ11"></div><div style="border: 1px solid #AAA; padding:5px;">
 +
=== 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 $t_H$).
 +
<div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;">We assume that the Universe expanded in the past with constant velocity equal to its modern value. Then the physical distance between any two cosmological objects equals to $R = V_Ht_H = H_0Rt_H,$ and $t_H = H_0^{-1} \approx 4 \cdot 10^{17} ~\mbox{ s} \approx 14\cdot10^9~\mbox{years.}$</p>
 +
  </div>
 +
</div></div>
  
  
 +
<div id="equ13"></div><div style="border: 1px solid #AAA; padding:5px;">
 +
=== Problem 11: Olbers paradox resolved ===
 +
Show that the model of the expanding Universe allows one to eliminate the Olbers' paradox.
 +
<div class="NavFrame collapsed">
 +
  <div class="NavHead">solution</div>
 +
  <div style="width:100%;" class="NavContent">
 +
    <p style="text-align: left;">A star with absolute luminosity $L$, situated at distance $r$, has the apparent luminosity equal to $4\pi r^2L$. If the number density of the stars is constant and equals to $n$, then the number of stars in a spherical layer between $r$ and $r+dr$ equals to $4\pi n r^2dr$, and the total density of radiation energy from all the stars is equal to
 +
\[\rho _s
 +
= \int\limits_0^{R_H}
 +
\frac L {4\pi r^2} 4\pi r^2 dr
 +
= Ln\int\limits_0^{R_H} dr  = LnR_H.\]
  
<div id="02004"></div>'''Problem 4.''' The main qualitative difference from the usual explosion lies in the fact that the explosive charge is usually surrounded by atmospheric air. The expansion is then caused by the difference between the huge pressure of the gaseous products of the explosion and comparatively small pressure of the surrounding air. But when considering the expanding Universe, one assumes that the pressure (according to the cosmological principle) is uniformly distributed too. Therefore there are neither pressure gradients nor forces that could cause or even affect the expansion. The expansion of the Universe itself is the result of initial velocity distribution.
+
The solution of the Olbers' paradox is thus possible due to the fact that an observer registers radiation from the stars inside of the Hubble's sphere only, rather than from the infinite Universe.</p>
 
+
  </div>
 
+
</div></div>
<div id="02005"></div>'''Problem 5.''' Show that the Hubble's law is invariant with respect to Galilean transformations.
+
 
+
 
+
<div id="02006"></div>'''Problem 6.'''  Show that the Hubble's law represents the only form of expansion compatible with homogeneity and isotropy of the Universe.
+
 
+
 
+
<div id="02007"></div>'''Problem 7.'''  Show that if expansion of the Universe obeys the Hubble's law then the initial homogeneity is conserved for all its subsequent evolution.
+
 
+
 
+
<div id="02009"></div>'''Problem 8.'''  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.
+
 
+
 
+
<div id="020010"></div>'''Problem 9.'''  Galaxies typically have peculiar (individual) velocities of the order of $V_p \approx 100~\mbox{\it km/s}.$ Estimate how distant a galaxy should be for its peculiar velocity to be negligible compared to the velocity of Hubble flow $V_H=H_{0}R$.
+
 
+
 
+
<div id="02011"></div>'''Problem 10.'''  Estimate the age of the Universe basing on the observed value of the Hubble's constant (the Hubble time $t_H$).
+
 
+
 
+
<div id="020013"></div>'''Problem 11.''' Show that the model of the expanding Universe allows one to eliminate the Olbers' paradox.
+
----
+

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.