Introduction In the last 30 years we have made great progress both ...

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Calculation of Relic Densityomega= darkOmega(&Xf, fast); // calculates Ω dm h 2fast = 1 – optimized fast calculation ; 0 – robust calculation.Xf = Mcdm/Tf - return parameter. Tf is freeze-out temperaturedefined by conditionρ dm (T f ) = 2.5 ρ dm_equilibrium (T f )28
Coannihilation and Beps parameterAs a rule we have several particles in odd sector. We assumethat all of them are in chemical equilibriumNi / Nj = exp ( -( mi – mj )/T)All reactions like ~i,~j -> SM are responsible for DM formation.This is a reason we need a lot of matrix elements to to calculatecoannihilation channels. But density of heavy odd particles issuppressed my Boltzmann factor an can be omitted.We have Beps parameter which cuts calculation of suppressedcoannihilation channels:~i, ~j -> SMIs omitted ifExp( -(mi + mj – 2*Mcdm)/T) < BepsDefault value Beps = 1.E-3.29
Page 1 and 2: MicrOMEGAs - a package for calculat
Page 3 and 4: Massive Stable ParticleTo describe
Page 5 and 6: In the framework of a given model o
Page 7 and 8: C) Solar neutrinos. In some sense t
Page 9 and 10: To Downloadhttp://lapth.in2p3.fr/mi
Page 11 and 12: Compilation of CalcHEP and micromeg
Page 13 and 14: Module structure of main programs.m
Page 15 and 16: Parameters of main programs.Default
Page 17 and 18: ==== Physical Constraints: =====del
Page 19 and 20: Free parameters of the model.Free m
Page 21 and 22: Constrained parameter of the model.
Page 23 and 24: err = sortOddParticles( stext)This
Page 25 and 26: Shared libraries of matrix elements
Page 27: Calculation of particle widths in m
Page 31 and 32: We define abundance Y=N/s to remove
Page 33 and 34: Ω = M cdm [GeV] * Y * (2.889 10 9
Page 36 and 37: vSigma[pb] & Yeqfor MSUGRA modelM0

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