Primordial Black Holes and Cosmological Phase Transitions Report ...

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$Kawasaki dynamic in continuum Math. Encounters XXXV ... - CCM$

PBHs and Cosmological Phase Transitions 46 like Ñ1 LSP; nearly degenerate wino–like Ñ2, ˜ C1; and higgsino–like Ñ3, Ñ4, ˜ C2. The gluino is the heaviest superpartner. The squarks are all much heavier than the sleptons, and the lightest sfermion is an stau (e.g. Martin, 2006). The mass spectrum of supersymmetric particles and Higgs boson according to the SPS1a scenario is represented in Figure 11 and in Table 11. Note that in this scenario the masses of the second family coincide with the masses of the first family. At the moment we only have lower limit masses for these particles (cf. Table 11) and a list of assumptions that we see as reasonable. For example, it is perhaps not unlikely that (e.g. Martin, 2006): • The LSP is the lightest neutralino Ñ1. • The gluino will be much heavier than the lighter neutralinos and charginos. • The squarks of the first and second families are nearly degenerate and much heavier than the sleptons. • The lighter stop ˜t1 and the lighter sbottom ˜ b1 are probably the lightest squarks. • The lightest charged slepton is probably a stau ˜τ. • The left–handed charged sleptons are likely to be heavier than their righthanded counterparts. • The lightest neutral Higgs boson h 0 is lighter than about 150 GeV, and may be much lighter than the other Higgs scalar mass eigenstates A 0 , H ± , H 0 . Extensions of the MSSM can be introduced, where the Higgs sector is further enlarged and the Higgs masses are less constrained. As an example we have the so–called Next–to–Minimal Supersymmetric Standard Model (NMSSM), whose Higgs sector includes not only two Higgs doublets, but also an additional singlet. Such an extension may slightly decrease the level of fine–tuning required to reconcile the present stringent lower bounds on supersymmetric particles and Higgs boson masses with the measured value of the Fermi scale (e.g. Ellis et al., 2007). 1.10 Degrees of freedom In the early Universe collision and decay processes are continuously creating and destroying particles. Considering thermal equilibrium (i.e., each process is taking place at the same rate as its inverse) then the number of particles of a given species i, per momentum state, is given by (e.g. Lyth, 1993) f(p) =gi(T ) e E−µ −1 T ± 1 (95) where gi(T ) counts the effective number of relativistic helicity degrees of freedom of that particle species at a given photon temperature T ; p is the momentum, E
PBHs and Cosmological Phase Transitions 47 Table 10: The MSSM particles in terms of gauge eigenstates and mass eigenstates. In the MSSM there are 32 distinct masses to be determined corresponding to 32 undiscovered particles. Particles Spin Parity Gauge Eigenstates Mass Eigenstates Higgs bosons 0 +1 H 0 u H0 d H+ u H− d h 0 H 0 A 0 H ± ũL ũR ˜ dL ˜ dR (same) squarks 0 −1 ˜sL˜sR˜cL˜cR (same) ˜tL ˜tR ˜bL ˜bR ˜t1 ˜t2 ˜b1 ˜b2 ˜eL ˜eR ˜νe (same) sleptons 0 −1 ˜µL˜µR˜νµ (same) ˜τL ˜τR ˜ντ neutralinos 1/2 −1 ˜ B 0 ˜ W 0 ˜ H 0 u ˜ H 0 d charginos 1/2 −1 ˜ W ± ˜ H + u ˜ H − d ˜τ1 ˜τ2 ˜ντ Ñ1 Ñ2 Ñ3 Ñ4 ˜C ± 1 ˜ C ± 2 gluino 1/2 −1 ˜g (same)
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CCM-Centro de Ciências Matemática
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Contents List of Figures vii List o
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PBHs and Cosmological Phase Transit
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List of Tables 1 The Universe timel
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Table 49 (continued). PBHs and Cosm
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Table 49 (continued). Radiation EW
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