The Slow X-Ray Expansion of the Northwestern Rim of the Supernova Remnant RX J0852.0–4622

Katsuda, Satoru; Tsunemi, H.; Mori, Koji

doi:10.1086/588499

Cited by 81 publications

(106 citation statements)

References 22 publications

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“…Although an expansion of the shock front over a time span of 6.5 yr was reported by Katsuda et al (2008), we did not consider this because the possible displacement (∼0.1 ) due to the remnant expansion is quite small. Figure 1 shows the combined image in an energy range of 0.5-10 keV without exposure correction.…”

Section: Spectral Analysismentioning

confidence: 99%

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

Kishishita

Hiraga

Uchiyama

2013

A&A

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The supernova remnant (SNR) RX J0852.0-4622 (Vela Jr., G266.6-1.2) is one of the most important SNRs for investigating the acceleration of multi-TeV particles and the origin of Galactic cosmic rays because of its strong synchrotron X-ray and TeV γ-ray emission, which show a shell-like morphology similar to each other. Using the XMM-Newton archival data consisting of multiple pointing observations of the northwestern rim of the remnant, we investigate the spatial properties of the nonthermal X-ray emission as a function of distance from an outer shock wave. All X-ray spectra are well reproduced by an absorbed power-law model above 2 keV. It is found that the spectra show gradual softening from a photon index Γ = 2.56 in the rim region to Γ = 2.96 in the interior region. We show that this radial profile can be interpreted as a gradual decrease of the cutoff energy of the electron spectrum due to synchrotron cooling. By using a simple spectral evolution model that includes continuous synchrotron losses, the spectral softening can be reproduced with the magnetic field strength in the post-shock flow to less than several tens of μG. If this is a typical magnetic field in the SNR shell, γ-ray emission would be accounted for by inverse Compton scattering of high-energy electrons that also produce the synchrotron X-ray emission. Future hard X-ray imaging observations with Nustar and ASTRO-H and TeV γ-ray observations with the Cherenkov Telescope Array (CTA) will allow us to explore other possible explanations of the systematic softening of the X-ray spectra.

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Section: Spectral Analysismentioning

confidence: 99%

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

Kishishita

Hiraga

Uchiyama

2013

A&A

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“…Although the multiwavelength spectrum of these sources can be obtained directly from observations, it is very difficult to determine their distance and age (Aharonian et al 2007a;Katsuda et al 2008;Abramowski et al 2011), which makes further exploration of their nature challenging. The distance of an SNR is usually constrained by observations of emission or absorption lines from molecular clouds along the line of sight whose distance can be inferred from the Doppler shift of the line and the spiral structure of the Milky Way galaxy (e.g., Eisenhauer et al 2005;Tian et al 2008Tian et al , 2010.…”

Section: Introductionmentioning

confidence: 99%

FermiLarge Area Telescope observations of the supernova remnant HESS J1731-347

Yang

Zhang

Yuan

et al. 2014

A&A

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Context. HESS J1731-347 has been identified as one of the few TeV-bright shell-type supernova remnants (SNRs). These remnants are dominated by nonthermal emission, and the nature of TeV emission has been continuously debated for nearly a decade. Aims. We carry out the detailed modeling of the radio to γ-ray spectrum of HESS J1731-347 to constrain the magnetic field and energetic particles sources, which we compare with those of the other TeV-bright shell-type SNRs explored before. Methods. Four years of data from Fermi Large Area Telescope (LAT) observations for regions around this remnant are analyzed, leading to no detection correlated with the source discovered in the TeV band. The Markov chain Monte Carlo method is used to constrain parameters of one-zone models for the overall emission spectrum. Results. Based on the 99.9% upper limits of fluxes in the GeV range, one-zone hadronic models with an energetic proton spectral slope greater than 1.8 can be ruled out, which favors a leptonic origin for the γ-ray emission, making this remnant a sibling of the brightest TeV SNR RX J1713.7-3946, the Vela Junior SNR RX J0852.0-4622, and RCW 86. The best-fit leptonic model has an electron spectral slope of 1.8 and a magnetic field of ∼30 μG, which is at least a factor of 2 higher than those of RX J1713.7-3946 and RX J0852.0-4622, posing a challenge to the distance estimate and/or the energy equipartition between energetic electrons and the magnetic field of this source. A measurement of the shock speed will address this challenge and has implications on the magnetic field evolution and electron acceleration driven by shocks of SNRs.

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“…The distance to the remnant and its age can be constrained by its angular size and its angular expansion rate measured by Katsuda et al (2008) and Allen et al (2015) using XMM-Newton and Chandra data respectively. XMM-Newton data taken between 2001 and 2007 implies an expansion rate of 0.84 ± 0.23 yr −1 (Katsuda et al, 2008) while Chandra data from 2003 to 2008 suggests an expansion rate of 0.42 ±0.10 yr −1 Allen et al (2015).…”

Section: Pos(icrc2017)580mentioning

confidence: 99%

Magnetic field damping in the Vela Jr. SNR

Sushch¹,

Brose²,

Pohl³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with the 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 steepening of the spectrum towards the interior of the remnant. In this study we aim for the self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its spatially-dependent features. 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. We show that accounting for the damping of strong magnetic turbulence downstream of the forward shock might explain the observed radial dependence of the X-ray spectrum.

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The Slow X-Ray Expansion of the Northwestern Rim of the Supernova Remnant RX J0852.0–4622

Cited by 81 publications

References 22 publications

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

FermiLarge Area Telescope observations of the supernova remnant HESS J1731-347

Magnetic field damping in the Vela Jr. SNR

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