GeV-TeV gamma-rays and neutrinos from the Nova V407 Cygni

TL;DR

This paper explores gamma-ray and neutrino emissions from Nova V407 Cygni, modeling electron and hadron acceleration to predict observable signals in GeV to TeV energies for current and future telescopes.

Contribution

It introduces a detailed model of particle acceleration and radiation processes in Nova V407 Cygni, predicting high-energy emissions and neutrinos for the first time.

Findings

GeV gamma-ray emission explained by inverse Compton scattering of stellar radiation.

Hadron acceleration can produce TeV gamma-rays and neutrinos.

Predicted fluxes are within detection capabilities of IceCube and CTA.

Abstract

The Fermi-LAT telescope has unexpectedly discovered GeV gamma-ray emission from the symbiotic Nova V407 Cygni. We investigate the radiation processes due to electrons and hadrons accelerated during the explosion of this Nova. We consider a scenario in which GeV gamma-ray emission observed by Fermi is produced by the electrons with energies of a few tens of GeV in the inverse Compton scattering of stellar radiation. On the other hand, the hadrons are expected to reach larger energies, due to the lack of radiation losses during acceleration process, producing TeV gamma-rays and neutrinos. We predict the fluxes of very high energy gamma-rays and neutrinos from Novae of the V407 type for two models of hadron acceleration and discuss their possible detectability by the present and future telescopes (e.g. IceCube, CTA)