arXiv subjects
Publications and source records attributed to Jihn E. Kim.
We report that the hypothesis that the upper bound on the axion decay constant can be moved up beyond $10^{12}$ GeV in models with a stronger QCD in the early universe is not realized. This proof is possible by studying the superpotential in the dual model and obtaining the form of the axion potential respecting the original global symmetries.
We suggest a simple modification of the maximal mixing scenario (with $S_3$ permutation symmetry) for three light neutrinos. Our neutrino mass matrix has smaller permutation symmetry $S_{2}$ ($ν_μ \leftrightarrow ν_{e}$), and is consistent with all neutrino experiments except the $^{37}$Cl experiment. The resulting mass eigenvalues for three neutrinos are $m_{1} \approx (2.55-1.27) \times 10^{-3} eV, m_{2,3} \approx (0.71-1.43) eV$ for $Δm_{LSND}^{2} = 0.5 - 2.0 eV^2$. Then these light neutrinos can account for $\sim (2.4-4.8)% (6.2-12.4 %)$ of the dark matter for $h = 0.8 (0.5)$. Our model predicts the $ν_μ \rightarrow ν_τ$ oscillation probability in the range sensitive to the future experiments such as CHORUS and NOMAD.
We examine in the context of supersymmetric models whether the usual cosmological upper bound on the axion decay constant can be relaxed by assuming a period of stronger QCD in the early universe. By evaluating the axion potential in the early universe and also taking into account the dilaton potential energy, it is argued that a stronger QCD is not useful for raising up the bound.
After a brief review of the axion solution of the strong CP problem, its supersymmetric extension and the superstring axion are discussed. I also present one interesting cosmological scenario, the axino-gravitino cosmology, for the large scale structure of the universe.
We argue that the hidden sector potential energy is generically of order the intermediate scale although the true cosmological constant does vanish. This would significantly change the predicted values of soft parameters for a variety of supergravity models including those derived from string theory. We stress that this point is particularly relevant for supergravity models in which the soft masses of observable fields vanish at tree level. Implications of a nonzero hidden sector potential energy for low energy phenomenology are also studied.
We explore the one-loop electroweak radiative corrections in the context of the traditional minimal $SU(5)$ and the string-inspired $SU(5)\times U(1)$ supergravity models by calculating explicitly vacuum-polarization and vertex-correction contributions to the $ε_1$ and $ε_b$ parameters. We also include in this analysis the constraint from $b\rightarrow sγ$ whose inclusive branching ratio $B(b\rightarrow sγ)$ has been actually measured very recently by CLEO. We find that by combining these three most important indirect experimental signatures and using the most recent experimental values for them, $m_t\gtrsim 170 {\rm GeV}$ is excluded for $μ>0$ in both the minimal $SU(5)$ supergravity and the no-scale $SU(5)\times U(1)$ supergravity. We also find that $m_t\gtrsim 175(185) {\rm GeV}$ is excluded for any sign of $μ$ in the minimal ($SU(5)\times U(1)$) supergravity model.
In supergravity models, the quantum correction to the vacuum energy can be of order $M_I^4$, if the cutoff is of order the Planck mass $M^2_{P}$ and $Str\ {\cal M}^2\ne 0$. Therefore, the tree level cosmological constant must be nonzero (probably negative). Since the current practice of calculating soft parameters in supergravity models assumes the vanishing tree level cosmological constant, the supergravity calculation must be accordingly modified. This implies that the soft parameters in supergravity has an additional contribution depending on the nonvanishing tree level cosmological constant. A simple quantum mechanical model mimicking this situation is also presented.
We have performed a systematic analysis to compute the one-loop electroweak corrections to the Z->b b-bar vertex in terms of $ε_b$ and $R_b$ in the context of the minimal $SU(5)$ and no-scale $SU(5)\times U(1)$ supergravity models. With the measured top mass, $m_t=174\pm 10^{+13}_{-12}$ $\GeV$ , recently announced by CDF, we use the latest LEP data on $ε_b$ and $R_b$ ($\equiv{Γ(Z->b b-bar)/{Γ(Z->hadrons)}}$) in order to constrain further the two models. We find that the present LEP data on $ε_b$ and $R_b$ constrain the two models rather severely. Especially, the low-$\tanβ$ region is constrained more severely. $\tanβ\lsim 2.5$ $(4.0)$ is excluded by $ε_b$ at $90\%$ C.~L. for $m_t\gsim 170$ $(180)$ $\GeV$ in the minimal $SU(5)$ (no-scale $SU(5)\times U(1)$) supergravity. Even more stringent constraint comes from $R_b$. It excludes $\tanβ\lsim 4.0$ at $90\%$ C.~L. for $m_t\gsim 160$ $(170)$ $\GeV$ in the minimal $SU(5)$ (no-scale $SU(5)\times U(1)$) supergravity. We also find that the sign on $μ$ in the two models can be determined from $ε_b$ and $R_b$ at $90\%$ C.~L.
We stress that a natural solution of the $μ$ problem requires two ingredients: a symmetry that would enforce $μ= 0$ as well as the occurence of a small breaking parameter that generates a nonzero $μ$. It is suggested that both the Peccei-Quinn symmetry and the spontaneously broken $R$ symmetry may be the sources of the needed $μ$ term in the minimal supersymmetric standard model provided that they are spontaneously broken at a scale $10^{10}-10^{12}$ GeV. To solve the strong CP problem with a hidden sector confining group, both of these symmetries are needed in superstring models with an anomalous $U(1)_A$.
Since it became evident that the CDM model for cosmic structure formation predicts smaller power on large scales than observed, many alternatives have been suggested. Among them, the existence of late decaying particle can cure it by delaying the beginning of the matter domination and increasing the horizon length at that time. We discuss the realization of this scenario and present the light neutrino and the light axino as possible examples of working particle physics model. We point out that the increased power at sub-galaxy scale predicted by this scenario could lead to rich sub-galaxy structures.
Some of the soft SUSY breaking parameters in hidden sector supergravity model depend on the expectation value of the hidden sector scalar potential, $ $, whose tree level value is equal to the tree level cosmological constant. The current practice of calculating soft parameters assumes that $ =0$. Quantum correction to the cosmological constant can differ from the correction to $ $ by an amount of order $m^2_{3/2}M_{Pl}^2/8π$. This implies that, for the vanishing cosmological constant, the $ $--dependent parts of soft terms can be sizable, and hence the supergravity phenomenology should be accordingly modified.
We suggest the fermion doubling for all quarks and leptons. It is a generalization of the neutrino doubling of the seesaw mechanism. The new quarks and leptons are $SU(2)$ singlets and carry the electromagnetic charges of their lighter counterparts. An $SU(3)$ {\it anomaly free global symmetry} or a discrete symmetry can be introduced to restrict the Yukawa couplings. The form of mass matrix is belonging to that of Nelson and Barr even though our model does not belong to Barr's criterion. The weak CP violation of the Kobayashi-Maskawa form is obtained through the spontaneous breaking of CP symmetry at high energy scale. The strong CP solution is through a specific form of the mass matrix. At low energy, the particle content is the same as in the standard model. For a model with a global symmetry, in addition there exists a massless majoron.
We show that heavy quark axion is not necessarily a hadronic axion, which manifests in the quark and lepton seesaw mechanism. We introduce a heavy $SU(2)$ singlet fermion for each known fermion in order to unify the axion scale and the seesaw scale. The light quarks and leptons gain their masses by the seesaw mechanism. Even though our axion model gives a kind of heavy quark axion, the axion has tree level lepton--axion coupling suppressed by $F_a$, contrary to a widely known belief that heavy quark axions are hadronic.
It is suggested that the axino mass in the 1 MeV region and gravitino mass in the eV region can provide an axino lifetime of order of the time of photon decoupling. In this case, some undecayed axinos act like cold dark matters and some axino decay products (gravitinos and hot axions) act like hot dark matters at the time of galaxy formation.
The recent LEP data for gauge coupling constants constrain many grand unified models. In this paper, we study several possibilities for unification of gauge coupling constants. Without an intermediate mass scale, the minimal supersymmetric standard model is the only possibility. For one intermediate mass scale, it is possible to have many routes toward grand unification: $SO(10)\rightarrow SU(3)_c\times SU(2)_L\times SU(2)_R\times U(1) , SU(7), SU(8)$, etc. We present also simple relations for the possibility of unification.
We investigate a model with an extra $Z_{2}$ gauge symmetry in the Standard Model. We assume that only the scalars and the leptons carry non-zero charge. The symmetry gives a structure to the mass matrix for the neutrinos. With two extra Higgs singlets and two extra singlet right-handed neutrinos we can build a model that fits the requirements of the MSW-solution of the Solar neutrino problem. With a third singlet right-handed neutrino it is also possible to have a 10 eV neutrino, a dark matter candidate.
We obtain a three generational $SU(3)_c\times SU(3)_w \times U(1)^4\times [SO(12)\times U(1)^2]^\prime$ model from an orbifold construction with the requirement that three generations arise from twisted sectors. There exist supersymmetric vacua realizing the standard model. In one example the anomalous $U(1)$ breaks the gauge symmetry down to $SU(3)_c\times SU(2)_w\times U(1)_Y\times SO(12)^\prime$.
The $μ$ term in the supersymmetric standard model is known to" be nonzero. Supersymmetry breaking at the intermediate scale may provide the needed $μ$ term and the invisible axion. A possible solution of this $μ$ problem in superstring models is also discussed.