Classical relativistic constituent particles and composite states. II

Abstract

A classical theory of interacting relativistic constituent and composite particles is developed further. The Lorentz-invariant Lagrangian, a function of the single unmeasurable evolution parameter s, is considered for attractive and repulsive harmonic-oscillator forces acting pairwise between constituent particles. Nonrelativistic Newtonian equations of motion can be derived by letting c --t cc in "equal-time" solutions, but, in general, there is a "surplus" of solutions which have no nonrelativistic counterpart. These solutions are used to construct classical models of strongly interacting composite particles. Asymptotic selection rules and constituent confinement are postulated and lead to space-time conservation laws for systems of scattering composite particles. Constituent four-vectors are linear combinations of "kinematic" terms and "intrinsic" normal modes. The latter are identified with internal symmetries of the composite particles, which are labeled by sets of "intrinsic numbers" analogous to additive quantum numbers. Formation of two-and three-body composite particles follows an exact analogy to the color quark model, in which the meson is composed of a quark and an antiquark of the same color, and the baryon is formed from three quarks of three different colors. Scattering examples are given analogous to MM-MM, MB +MB, and BB +BB. The reactions take place through constituent exchange, and total intrinsic numbers are conserved. There are other similarities to quantum field theory, such as particle-antiparticle pair creation and annihilation, fixed relative values of internal angular momenta, fixed orbital angular momentum, and many-particle systems characterized by a vacuum state (lowest energy state) and the existence of virtual composite particles as well as physically observable composite particles.

Lowly Polarized Light from a Highly Magnetized Jet of GRB 190114C

“…After RINGO3 polaroid, the light is split by two dichroic mirrors in three beams that are simultaneously recorded by three EMCCD cameras (Arnold et al 2012). In Figure 2, we derive the photonic response function of RINGO3 instrument which accounts for at-mospheric extinction (King 1985), telescope optics 4 , instrument dichroics 5 , lenses (Arnold 2017), filters 67 transmission and the quantum efficiency of the EMC-CDs (Arnold 2017). The total throughput results in three broad bandpasses with the following mean photonic wavelengths λ 0, {BV,R,I} = 5385 Å, 7030 Å, 8245 Å and full-widths-at-half-maximum FWHM {BV,R,I} = 2232 Å, 1130 Å, 835 Å.…”

“…For the BV band, the stacking does not reach the signal-to-noise ≥ 20 threshold for the last ∼ 800 -s of observations and therefore, the photometry is discarded. Magnitudes and flux density are corrected for atmospheric extinction with M c, {BV,R,I} = 0.14 mag, 0.04 mag, 0.02 mag and F c, {BV,R,I} = 0.89, 0.96, 0.98, respectively, which we compute from a weighted mean of the bandpasses throughput and the theoretical atmospheric extinction of the site (King 1985). We also correct for the mean Galactic extinction, A {BV,R,I} /E B−V = 3.12, 2.19, 1.73 with E B−V,MW = 0.0124 ± 0.0005 (Schlegel et al 1998), which we derive using Pei (1992) Milky Way dust extinction profile.…”

MEGADES: MEGARA Galaxy Discs Evolution Survey. Data Release I: central fields

“…To ensure that we do not miss flux when measuring in the image of the star we compute the position of the centroid using the spectra of 3 concentric rings around the brightest spaxel (37 spaxels in total). In this step an atmospheric extinction correction is also applied using a reference file provided by GTC (King 1985). With this information we can run the MegaraLcbStdStar task that produces the sensitivity curve needed to flux calibrate our data.…”