Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · hep-ph/0406048

Early SU(4)_PS x SU(2)_L x SU(2)_R x SU(2)_H Unification of Quarks and Leptons

Andrzej J. Buras·P. Q. Hung·Ngoc-Khanh Tran·Anton Poschenrieder·Elmar Wyszomirski
View original source ↗Read source document ↗Export metadata ↓

Abstract

We discuss various aspects of the early petite unification (PUT) of quarks and leptons based on the gauge group G_PUT=SU(4)_PS x SU(2)_L x SU(2)_R x SU(2)_H. This unification takes place at the scale M= O(1-2 TeV) and gives the correct value of sin^2 theta_W(M_Z^2) without the violation of the upper bound on the K_L -> mu e rate and the limits on FCNC processes. These properties require the existence of three new generations of unconventional quarks and leptons with charges up to 4/3 (for quarks) and 2 (for leptons) and masses O(250 GeV) in addition to the standard three generations of quarks and leptons. The horizontal group SU(2)_H connects the standard fermions with the unconventional ones. We work out the spontaneous symmetry breaking (SSB) of the gauge group G_PUT down to the SM gauge group, generalize the existing one-loop renormalization group (RG) analysis to the two-loop level including the contributions of Higgs scalars and Yukawa couplings, and demonstrate that the presence of three new generations of heavy unconventional quarks and leptons with masses O(250 GeV) is consistent with astrophysical constraints. The NLO and Higgs contributions to the RG analysis are significant while the Yukawa contributions can be neglected.

Explore related subjects

hep-ph

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Andrzej J. Buras, P. Q. Hung, Ngoc-Khanh Tran, Anton Poschenrieder, Elmar Wyszomirski. 2004-06-04. Early SU(4)_PS x SU(2)_L x SU(2)_R x SU(2)_H Unification of Quarks and Leptons. https://doi.org/10.1016/j.nuclphysb.2004.08.024

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

QCD Axion Conversion in Magnetospheres of Neutron Stars

The axion-converted-photons flux plays a key role in searches of QCD axions as a dark matter (DM) candidate. In addition to solving the strong CP problem, these may explain the properties of the mysterious DM. Neutron star (NS) cooling by neutrino/axion emissions rate constrains the astrophysical properties of superdense matter. We attempt to analyse the impact of strong magnetic fields on the emission properties of axions by employing the APR, FPS, and SLY equation of State (EoS). We modify the Tolman Oppenheimer Volkoff (TOV) equations by considering effects of strong fields' and generate profiles. We assume Cooper-pair-breaking formation (PBF) and the Bremsstrahlung process occurring in the core of NS. We use the radial distance-dependent magnetic field configuration within the permissible limit of the central magnetic field. Our work explores the variations in the axion masses of 10 meV, 15 meV, and 20 meV as a cooling source for spherically symmetric magnetised NSs. We have also shown the energy spectrum of axions and their conversion to photons. Our analysis shows that the cooling rate and the luminosity of observables (axions) for NSs change significantly due to the magnetic field. The results for the luminosity of axions is quite sensitive to its mass and EoS, as the less separation is observed for SLY EoS in comparison to the FPS and APR EoS. We report that the spectrum of axions from the Bremsstrahlung process dominates over the PBF process at lesser axion energies, within the possible axion mass range for PSR J1357-6429 NS. Our results reveal that the impact of the magnetic field is less at lower axion energies, indicating the necessity for including a magnetic field in axion-to-photon conversion mechanisms. The results for the axions mass 10 meV and 15 meV as compared to 20 meV confirms the existing report of the 16 meV.

hep-ph↗
arXiv2026

Search for Vector-Like Singlet Top ($T$) Quark in a Future Muon-Proton ($μp$) Collider at $\sqrt{s} = 5.29, 6.48,$ and $9.16$ TeV using Advanced Machine Learning Architectures

We study the sensitivity of a future $μp$ collider to singly produced singlet vector-like $T$ quarks in the $T\to Wb$ decay mode across both fully hadronic ($bjj$) and leptonic ($b\ellν$) final states at $\sqrt{s}=5.29$, $6.48$, and $9.16~\mathrm{TeV}$. Utilizing resolved-object reconstruction and TMVA-based multivariate classifiers (BDT, BDTG, MLP, and Likelihood), we perform a fast-simulation scan over $m_T=2$--$5~\mathrm{TeV}$ and the $(g^{*},m_T)$ parameter space. To quantify improvements, we compare this multivariate selection against the closest cut-based baseline at a benchmark point of $m_T=3~\mathrm{TeV}$, $\sqrt{s}=9.16~\mathrm{TeV}$, and $\mathcal{L}=3000~\mathrm{fb}^{-1}$, incorporating a $20\%$ background-normalization uncertainty via the Asimov significance $Z_A$. At this benchmark, the hadronic channel exhibits a substantial enhancement in both $S/\sqrt{S+B}$ and $Z_A$, improving from $18.05$ and $1.44$ to $273.51$ and $42.24$, respectively. Similarly, the leptonic channel improves from $3.51$ and $0.330$ to $113.85$ and $21.51$. In the full parameter scan, the $\sqrt{s}=9.16~\mathrm{TeV}$ configuration provides the strongest sensitivity at $\mathcal{L}=3000~\mathrm{fb}^{-1}$. The hadronic channel excludes (discovers) regions with $g^{*}\in[0.20,0.50]$ ($[0.30,0.50]$) up to $m_T\approx4.0~(3.5)~\mathrm{TeV}$, while the leptonic channel remains sensitive up to $m_T\approx5.0~\mathrm{TeV}$ for $g^{*}\in[0.10,0.50]$. These gains arise from the higher-purity multivariate signal regions evaluated under a common significance prescription, and not from a change of the collider configuration. The projections assume resolved-object reconstruction and fast detector simulation, and the absolute reach should be read with these assumptions in mind.

hep-ph↗
arXiv2026

Particle--antiparticle asymmetry from charge separation at expanding horizons

In a Friedmann universe with a time-varying cosmological term, massive particle--antiparticle pairs are produced continuously from the spacetime vacuum, and their members are separated by horizons. Along the cosmic history that explains $n_s$, $A_s$, $r$ and the low-$\ell$ power anomaly, we show how this separation generates the observed asymmetry. Horizons absorb the charge they separate, since gravity does not conserve global charges. Charge separation at the many horizons inside today's Hubble volume then acts as a volume violation of the U(1) charge, at a rate $Γ_C=κ_CΓ_M$ proportional to pair production. The sign requires a C- and CP-odd coupling to the time arrow. We describe both by an effective Lagrangian with a U(1)-violating coupling $g_c\,δ\mathcal O_SΦ^2$ to the spacetime vacuum and a time bias $-\partial_μf(R)\,J^μ$. For $f=c_a\ln|R|$ the chemical potential of producing a particle is $μ\simeq2c_a\dot H/H$. The asymmetry per pair reaches an attractor in the pair-dominated episode and freezes when the cosmological term is exhausted. The observed value requires $|c_a|/τ_S\simeq(0.65$--$1.0)\times10^{-4}$, with $T_S=τ_SH/2π$ the temperature of the spacetime vacuum, and its sign is fixed by the arrow of time. The Yukawa decays of the pairs transfer the asymmetry, with a uniform sign, to baryons and leptons and to dark-matter particles. The current of the charged decay products generates a magnetic field of $10^{-14}$--$10^{-11}$ G today on the coherence length of reheating.

hep-ph↗