Radio emission from SNe and young SNRs

Abstract

Abstract. Study of radio supernovae (RSNe), the earliest stages of supernova remnant (SNR) formation, over the past 20 years includes two dozen detected objects and more than 100 upper limits. Prom this work we are able to identify classes of radio properties, demonstrate conformance to and deviations from existing models, estimate the density and structure of the circumstellar material and, by inference, the evolution of the presupernova stellar wind, and reveal the last stages of stellar evolution before explosion. It is also possible to detect ionized hydrogen along the line of sight, to demonstrate binary properties of the stellar system, and to show dumpiness of the circumstellar material. More speculatively, it may be possible to provide distance estimates to RSNe.

FORTE satellite constraints on ultrahigh energy cosmic particle fluxes

“…Since FORTE threshold for detection of a weakly interacting particles (∼ 10 22 eV) is higher than the GZK limit (∼ 5 × 10 19 eV), it sets the limits on neutrinos producing super-GZK cosmic rays through resonant interaction with background neutrinos within ∼50 Mpc distance from us, the Z burst mechanism [42,43,44,45,46,47]. Although FORTE sets limits on parameters of Z burst models, the uncertainties in the models and the measured super-GZK cosmic ray flux still make most Z burst scenarios consistent with FORTE data.…”

“…The limit is compared to predicted neutrino fluxes from various sources: GRB: gamma ray bursts [48]; AGN: active galactic nuclei [49]; GZK: neutrinos produced in GZK mechanism from cosmic rays [50]; TD: topological defect model (non-SUSY) [51]; Z burst models are: the slanted box by [44], the diamonds showing the 1σ level errors are by [47,52], and the arrow is by [45, default value of parameters]. The limits from other experiments are also shown: AMANDA [53], RICE [54] (determined using (7) from the effective volume and time of observation), GLUE [12,13].…”

Searching for Lorentz Violation

“…There should consequently be a cutoff in the spectrum of observed protons at about 50 EeV (or 5 × 10 7 TeV), if they were created in processes at distances of more than about 100 Mpc. But up to 300 EeV cosmic rays (presumably protons) appear to be observed, although this is not entirely certain [38], and there are also theoretical ideas for a closer origin [36]. We conclude by mentioning some reviews of terrestrial and space-based experiments.…”

“…Again, however, a superluminal velocity of any size in the present theory does not imply a violation of causality. Now let us turn to the GZK cutoff, [2,[33][34][35][36][37][38] which results from collision of a charged fermion with a blackbody photon. The incoming photon has energy ω and momentum (−ω cos θ, −ω sin θ, 0) in units with h = c = 1.…”

Experimental Study of Acoustic Ultra–High‐Energy Neutrino Detection

“…[8] using Poisson's statistics and the fact that no events are observed. The resulting limit (multiplied by E 2 , as customary) is shown in Figure 17 along with the limits already available from FORTE [8], RICE [7] and GLUE [6], and with fluxes predicted by various theories [29,30,31,32,33,34].…”