This can be seen in Figure 9, where the eﬃciency factor κ falls off rapidly for MR1 > TRH .
Theory of Neutrinos: A White Paper
In the so-called ‘strong washout’ regime, TRH can be an order of magnitude smaller than M1 [185].
Theory of Neutrinos: A White Paper
Unstable gravitinos with masses below ∼ 10 TeV lead to severe constraints on the reheat temperature TRH [204] which are in conﬂict with thermal leptogenesis where TRH >∼ 109 GeV.
Theory of Neutrinos: A White Paper
However, the ‘overclosure’ constraint leads to TRH <∼ (109 − 1010 ) GeV.
Theory of Neutrinos: A White Paper
Here we have used the expression for the radiation entropy S (tRH ) = T 3 RH a3 (tRH ).
Cosmological Entropy Bounds
However, this value of γ does not follow from recent N body simulations, but from the assumptions that tdis scales linearly with trh, a contant Λ and a constant cluster density.
Conference summary: Mass loss from stellar clusters
Trh νAν ∗ = ν ∗ A⊗e−βY ν, (This implies in particular that M satisﬁes the DBC for e−βK / Tr e−βK ).
Reduced and Extended Weak Coupling Limit
If the reservoir is at inverse temperature β, then ν satisﬁes Trh νAν ∗ = ν ∗ A⊗e−βY ν, This implies in particular that M satisﬁes the DBC for e−βK / Tr e−βK .
Reduced and Extended Weak Coupling Limit
C ∼ 0.5, and TRH is the reheating temperature.
Leptogenesis: Theory and Neutrino Masses
On the other hand, it is remarkable that for typical gravitino and gluino masses in gravity mediated supersymmetry breaking, a reheating temperature TRH ∼ 1010 GeV yields the right order of magnitude for the dark matter abundance if the gravitino is the LSP.
Leptogenesis: Theory and Neutrino Masses
On the other hand, the ‘reheating temperature’ TRH is roughly constant, since there is a balance between temperature decrease due to expansion and temperature increase due to B-L Higgs boson decays.
Leptogenesis: Theory and Neutrino Masses
Note that contrary to conventional reheating mechanisms, the reheating temperature TRH is now determined by neutrino parameters! For neutrino masses consistent with leptogenesis and dark matter, the reheating temperature varies between 107 GeV and 1012 GeV (cf.
Leptogenesis: Theory and Neutrino Masses
If the reheat temperature (TRH ) after inﬂation is less than TGU T, then the monopoles are simply inﬂated away.
GUT's have the ability to defy sphalerons
H is the Hubble velocity, T0 is the temperature today, TRH is the reheating temperature, and ΩR h2 ≈ 4.31 × 10−5 is the fraction of critical energy density that is in radiation today.
Superheavy Dark Matter
For the channel Φ ⊗ Ψ we consider the constraint deﬁned by the requirements σΦ av := TrKσav ∈ A and σΨ av := TrHσav ∈ B, where σav is the average state of an input ensemble {µi, σi}.
On Shor's channel extension and constrained channels
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