Modeling of the spatially resolved non-thermal emission from the Vela Jr. supernova remnant

Abstract

Vela Jr. (RX J0852.0$-$4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy ($>100$ GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution 1D hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.

12 pages, 8 figures, 4 tables, accepted for publication in A&A

References in corpus (15)

• PLUTO: a Numerical Code for Computational Astrophysics
• H.E.S.S. observations of the supernova remnant RX J0852.0-4622: shell-type morphology and spectrum of a widely extended VHE gamma-ray source
• Dynamical Feedback of Self-generated Magnetic Fields in Cosmic Ray Modified Shocks
• Hadronic gamma-rays from RX J1713.7-3946?
• On the Expansion Rate, Age, and Distance of the Supernova Remnant G266.2-1.2 (Vela Jr.)
• The Slow X-Ray Expansion of the Northwestern Rim of the Supernova Remnant RX J0852.0-4622
• Deeper H.E.S.S. observations of Vela Junior (RX J0852.0$-$4622): Morphology studies and resolved spectroscopy
• A detailed study of the interstellar protons toward the TeV $\gamma$-ray SNR RX J0852.0$-$4622 (G266.2$-$1.2, Vela Jr.); a third case of the $\gamma$-rays and ISM spatial correspondence
• Measuring surface magnetic fields of red supergiant stars
• Transport of magnetic turbulence in Supernova remnants
• Reacceleration of electrons in supernova remnants
• Post-adiabatic supernova remnants in the interstellar magnetic field. Parallel and perpendicular shocks
• Analysis of GeV-band gamma-ray emission from SNR RX J1713.7-3946
• The properties of non-thermal X-ray filaments in young supernova remnants
• Suzaku observations of the hard X-ray spectrum of Vela Jr

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