- #1
bolahab
- 7
- 0
Hey guys, can someone please help with this question.
We now live in a time when the energy balance of the universe is dominated
by Λ. A long time from now, at t2× the universe will have doubled
in size, i.e.: a(t2×) = 2. At present, radiation is negligible: Ωr,0 ~ 0,
and will remain so, while Ωm,0 = 0.3 and ΩΛ,0 = 0.7 now. Note that
since ΩΛ,0 + m,0 = 1 now, their sum will remain the same.
a) Estimate the value of Ωm at t2×. Consider how the ratio Ωm/ΩΛ
changes with time, and use the flatness constraint mentioned above.
b) Estimate the time from now until t2×.
c) What will the Hubble distance be at t2×?
We now live in a time when the energy balance of the universe is dominated
by Λ. A long time from now, at t2× the universe will have doubled
in size, i.e.: a(t2×) = 2. At present, radiation is negligible: Ωr,0 ~ 0,
and will remain so, while Ωm,0 = 0.3 and ΩΛ,0 = 0.7 now. Note that
since ΩΛ,0 + m,0 = 1 now, their sum will remain the same.
a) Estimate the value of Ωm at t2×. Consider how the ratio Ωm/ΩΛ
changes with time, and use the flatness constraint mentioned above.
b) Estimate the time from now until t2×.
c) What will the Hubble distance be at t2×?