The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7–3946

Enomoto, R.; Tanimori, T.; Naito, T.; Yoshida, Tatsuo; Yanagita, S.; Mori, M.; Edwards, Philip; Asahara, A.; Bicknell, G. V.; Gunji, Shuichi; Hara, Shinji; Hara, T.; Hayashi, S.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kataoka, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Maeda, Sayaka; Maeshiro, A.; Matsubara, Y.; Mizumoto, Y.; Moriya, M.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishijima, K.; Ohishi, M.; Okumura, Ko; Patterson, Joseph; Sakurazawa, K.; Suzuki, Ryo; Swaby, D. L.; Takano, K.; Takano, Toshiaki; Tokanai, Fuyuki; Tsuchiya, Ken; Tsunoo, Hajime; Uruma, K.; Watanabe, Akira; Yoshikoshi, T.

doi:10.1038/416823a

Cited by 227 publications

(202 citation statements)

References 16 publications

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“…RX J1713-3946 was also detected in very high-energy (VHE: >100 GeV) γ-rays with the CANGAROO (Muraishi et al 2000;Enomoto et al 2002) and HESS telescopes (Aharonian et al 2004(Aharonian et al , 2006. Especially the latter, very detailed observations show a clear shell structure at TeV energies that correlates well with the ASCA contours.…”

Section: Introductionsupporting

confidence: 57%

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Berezhko¹,

Völk²

2010

A&A

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Aims.A nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants (SNRs) is employed to investigate the properties of SNR RX J1713.7-3946. Methods. Observations of the nonthermal radio and X-ray emission spectra, as well as the HESS measurements of the very high energy γ-ray emission, are used to constrain the astronomical and CR acceleration parameters of the system. It is argued that RX J1713.7-3946 is a core collapse supernova (SN) of type II/Ib with a massive progenitor, and it has an age of ≈1600 yr and is at a distance of ≈1 kpc. It is also assumed that the CR injection/acceleration takes place uniformly across the shock surface for this kind of core collapse SNR. Results. The theory gives a consistent description for all the existing observational data, including the nondetection of thermal X-rays and the spatial correlation of the X-ray and γ-ray emission in the remnant. Specifically, it is shown that an efficient production of nuclear CRs, leading to strong shock modification and a strong downstream magnetic field B d ≈ 140 μG can reproduce in detail the observed synchrotron emission from radio to X-ray frequencies, together with the γ-ray spectral characteristics as observed by the HESS telescopes. Conclusions. The calculations are consistent with RX J1713.7-3946 being an efficient source of nuclear CRs.

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Section: Introductionsupporting

confidence: 57%

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Berezhko¹,

Völk²

2010

A&A

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“…It is particularly intriguing that the TeV -ray distribution largely resembles that of the CO distribution in that they are enhanced in the northwestern rim of the SNR as noted by Aharonian et al (2004). While the statistical significance in HESS results may not yet be high enough to make a detailed comparison of the individual peaks, we make a preliminary estimate of the efficiency for proton acceleration over the entire SNR by using a formula from Enomoto et al (2002), (E/10 48 )(M cloud /200)(l/3) À3 (d/1) À5 ¼ 1:35, where E (ergs) is the total energy of cosmic-ray protons, M cloud (M ) the molecular cloud mass interacting with them, l ( pc) the typical length of the cloud, and d (kpc) the distance, the same as that in Paper I. We assume that the interacting molecular cloud mass amounts to $2500 M by summing up the major CO peaks in contact with the SNR (from Table 1).…”

Section: Origin Of Gamma Rays and Cosmic-ray Protonsmentioning

confidence: 99%

“…Uchiyama et al (2003) showed that the synchrotron cutoff energy is unusually high beyond 10 keV, corresponding to 10 14 eV as the highest particle energies. G347.3À0.5 was also detected at the TeV -ray range with the CANGAROO telescope (Muraishi et al 2000;Enomoto et al 2002), and models of broadband emission point to IC scattering as the origin of the TeV -ray photons (Muraishi et al 2000;Ellison et al 2001). More recently, follow-up TeV -ray observations have led to a different conclusion, suggesting pion decay as the source of energetic photons ( Enomoto et al 2002), but the nature of this emission is still uncertain (see Butt et al 2002;Reimer & Pohl 2002;Aharonian et al 2004).…”

Section: Introductionmentioning

confidence: 99%

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Moriguchi

Tamura

Tawara

et al. 2005

ApJ

108

134

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The supernova remnant G347.3À0.5 (J1713.7À3946) is known as one of the unique SNRs that emit TeV -rays, as well as nonthermal X-rays. We present a detailed study of molecular gas toward this SNR obtained with the 4 m millimeter and submillimeter telescope NANTEN at an angular resolution of 2A6. This study has revealed that several intensity peaks and the overall distribution of the molecular gas with radial velocities from À12 to À3 km s À1 show a remarkably good correlation with the X-ray features, strongly supporting the recently derived kinematic distance around 1 kpc, as opposed to the 6 kpc previously claimed. In addition, we show that absorption of X-rays is caused by local molecular gas at softer X-ray bands. Subsequent measurements of the submillimeter J ¼ 3 2 transition of CO made with the ASTE 10 m and CSO 10.4 m submillimeter telescopes toward three of the molecular intensity peaks have revealed higher excitation conditions, most likely higher temperatures above $30 K , in contrast to the typical gas temperature, 10 K, in low-mass dark clouds. This temperature rise is most likely caused by enhanced heating by the high-energy events in the SNR, where possible mechanisms include heating by X-rays, -rays, and/or cosmic-ray protons, although we admit that additional radiative heating by young protostars embedded may be working as well. In one of the CO peaks, we have confirmed the presence of broad molecular wings of $20 km s À1 velocity extent in the CO J ¼ 3 2 transition. Two alternative interpretations for the wings are presented; one is shock acceleration by the blast wave, and the other is molecular outflow driven by an embedded protostar. The SNR evolution is well explained as the free expansion phase based on the distance of 1 kpc. The molecular data set should be valuable for making a further detailed comparison with the -ray and X-ray distributions in order to examine the cosmic-ray acceleration quantitatively. Subject headingg s: cosmic rays -ISM: individual (SNR J1713.37À3946) -ISM: kinematics and dynamicssupernova remnants

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“…The steep photon spectra has been found in the high energy gamma-ray spectra of some other remnants measured by, e.g., the CANGAROO (Enomoto et al 2002), H.E.S.S (Aharonian et al 2006) and MAGIC (Carmona 2011) atmospheric Cherenkov telescopes. Particles accelerated by DSA mechanism generally comprised two distinct populations -CRs confined in the accelerator and the CRs escaping the system and these two populations have very different spectral shapes.…”

Section: Gamma-ray Observationsmentioning

confidence: 96%

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

Bykov

Malkov

Raymond

et al. 2013

Microphysics of Cosmic Plasmas

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In this review we discuss some observational aspects and theoretical models of astrophysical collisionless shocks in partly ionized plasma with the presence of nonthermal components. A specific feature of fast strong collisionless shocks is their ability to accelerate energetic particles that can modify the shock upstream flow and form the shock precursors. We discuss the effects of energetic particle acceleration and associated magnetic field amplification and decay in the extended shock precursors on the line and continuum multi-wavelength emission spectra of the shocks. Both Balmer-type and radiative astrophysical shocks are discussed in connection to supernova remnants interacting with partially neutral clouds. Quantitative models described in the review predict a number of observable line-like emission features that can be used to reveal the physical state of the matter in the shock precursors and the character of nonthermal processes in the shocks. Implications of recent progress of gamma-ray observations of supernova remnants in molecular clouds are highlighted.

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The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7–3946

Cited by 227 publications

References 16 publications

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

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