Toward a Better Understanding of Binding Theory (H. Bennis et al. (eds.), Atomism and Binding)

Abstract

* I am grateful to two anonymous EL reviewers for their invaluable comments and helpful suggestions on an earlier version of this paper.

Flavor structure with multi-moduli in 5D supergravity

“…It would be interesting to study models with different parameter choices from those we have chosen in this paper [31]. We may also extend the following models to the case with multi moduli, e.g., the models with two compensator hypermultiplets [14], a twisted SU(2) U gauge fixing [32], an anomalous U(1) symmetry [33], moduli mixing nonperturbative effects [34] and the one in which both the moduli T 1 and T 2 remain dynamical at low energies [35], and so on.…”

“…The fermion index f and the sfermion indicesf L,R represent f = (u, d, e),f R = (ũ,d,ẽ) andf L = (q,q,l), and then v f = (sin β, cos β, cos β)v, µ f = (cot β, tan β, tan β)µ, respectively, where v ≃ 174 GeV and µ is determined by the Then, roughly speaking, these parameters are typically within the allowed region [22] for M SB = 100 GeV. We would study these issues in more detail in a separate work [31].…”

Neutrino physics: Experimental and theoretical challenges

“…Current experiments include Super‐Kamiokande (Abe et al 2018a), IceCube DeepCore (Aartsen 2018; Aartsen et al 2019) and Antares (Albert et al 2019). Among the future projects are Hyper‐Kamiokande (Abe et al 2018b), IceCube Upgrade (Ishihara 2021), and KM3NeT/ORCA (Aiello et al 2022).…”

“…The current LBL accelerator experiments NO$$$ \nu $$$A (Acero et al 2019; Himmel 2020) and T2K (Abe et al 2020; Dunne 2020) not only measure the mixing angle $$$ {\theta}_{23} $$$ and the mass splitting $$$ \Delta {m}_{31}^2 $$$, but also are sensitive to $$$ {\theta}_{13} $$$ and the Dirac phase $$$ \delta $$$. Future LBL experiments with improved sensitivity include Hyper‐Kamiokande (T2HK) (Abe et al 2018b; Ishida 2013) and DUNE (Abi et al 2020). The excess of electron neutrino flux reported by the SBL experiments LSND (Aguilar‐Arevalo et al 2001) and MiniBooNE (Aguilar‐Arevalo et al 2018) may hint at the existence of new physics.…”

“…This is so because neutrino propagation from a supernova to a neutrino detector will result in an energy‐dependent time delay with respect to propagation at the speed of light given by $$$ \Delta t\kern0.3em \left[\mathrm{s}\right]=0.515\kern0.3em D\left[\mathrm{kpc}\right]\times {\left({m}_{\nu}\left[\mathrm{eV}\right]/{E}_{\nu}\left[\mathrm{MeV}\right]\right)}^2 $$$, where $$$ D $$$ is the distance to the star (Sajjad Athar et al 2022). Although the detectable range for current neutrino detectors is approximately $$$ D\sim $$$ tens of kpc (Milky Way), next‐generation detectors such as Hyper‐Kamiokande (Abe et al 2018b) are expected to reach neutrino events at $$$ D\sim 700 $$$ kpc. At present, the strongest bound coming from these sources is $$$ {m}_{\nu }<6 $$$ eV (Loredo & Lamb 2002; Pagliaroli et al 2010), obtained from a time delay $$$ \Delta t=13 $$$ s of the observed $$$ {\overline{\nu}}_e $$$ burst from SN1987A at $$$ D=55 $$$ kpc.…”