Shock-Cloud Interaction and Particle Acceleration in the Southwestern Limb of Sn 1006

Miceli, M.; Acero, Fabio; Dubner, G.; Decourchelle, A.; Orlando, S.; Bocchino, F.

doi:10.1088/2041-8205/782/2/l33

Cited by 32 publications

(47 citation statements)

References 28 publications

(25 reference statements)

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“…A different approach was very recently adopted by Miceli et al (2014), where the authors demonstrated the connection between shock-cloud interactions and particle acceleration in the southwestern limb of the historic remnant of SN 1006 based on the comparison of X-ray data with HI data. Figure 5 shows the X-ray image of the SW part of SN1006 in the 0.3-2 keV band with HI contours superimposed.…”

Section: Shell Deformationmentioning

confidence: 99%

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

et al. 2014

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The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and γ-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the γ-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and γ-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.

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Section: Shell Deformationmentioning

confidence: 99%

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

et al. 2014

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“…It seems that this density applies to the rest of the remnant except the northwestern (NW) part, where a bright H α filament is detected, and it can be deduced that the shock in the NW rim is interacting with dense material Article published by EDP Sciences A35, page 1 of 10 (e.g., Raymond et al 2007). Moreover, Miceli et al (2014) performed spatially resolved spectral analysis of the SW bright limb based on the deep observations with XMM-Newton and the archive HI data, and an isolated cloud is derived on the SW region of the remnant. Studies of the radiative properties of SN 1006 can give insight into the particle acceleration process in SNR shocks.…”

Section: Introductionmentioning

confidence: 98%

Three-dimensional magnetohydrodynamic studies of the non-thermal X-ray morphologies of SN 1006

Fang

Zhang

et al. 2015

A&A

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Context. The observations of the synchrotron emission from the supernova remnant (SNR) SN 1006 indicate a bilateral morphology, which is mainly characterized by two opposite bright limbs with knots and filaments along the boundary of the remnant. The morphology is not strictly circular with disturbances and bumps at the rim of the remnant. For instance, one big bump is located on the northeastern (NE) limb and several relatively small ones on the southwestern (SW) limb on the detected morphologies from the observations in the radio and X-rays. Aims. The generation of the asymmetric morphology of non-thermal X-rays for SN 1006 is investigated through three-dimensional (3D) magnetohydrodynamic simulations. Moreover, the density distribution of the ambient material can be investigated by comparing the resulting synchrotron morphology with the detected images of the hard X-ray emission. Methods. First, the remnant was simulated as a supernova explosion evolved in a turbulent plasma with a relatively small amplitude for the turbulence. In the model, several spherical cavities with lower densities compared with the background plasma were employed to reproduce the detected bumps at the bright limbs. Second, the effect of the modification on the morphology of the remnant due to efficient cosmic ray acceleration was investigated by adopting a lower adiabatic index. Results. If we assume that the injection efficiency of electrons into the diffusive shock acceleration process at the shock follows the quasi-parallel scenario, the hard X-ray morphology of SN 1006 with bumps in the bright NE and SW regions can be generally reproduced by employing cavities in the background medium in the non-modification scenario. Furthermore, in the modification case with a lower adiabatic index of 1.2 for the remnant evolved in a uniform medium, bubbles can be produced with relatively small extensions on the SNR boundary that result from the hydrodynamical instabilities that in turn overtake the forward shock. Conclusions. The SNR propagating in the turbulent medium with a relatively small amplitude can reproduce the knotty and filamentary morphology of the remnant better than what evolved in the uniform environment; moreover, the big bump on the NE limb can be explained as the result of a lower-density region, which has a radius of about 2.5 pc and a density of about 0.4 times of the general ambient medium, swept by the shock front, and the other smaller ones on the SW limb can either be reproduced with smaller regions with lower densities swept by the shock or be explained as the protrusions in the scenario of the efficient cosmic ray acceleration when the instability fingers effectively overtake the forward shock.

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“…For example, the young SNR SN 1006 is located far from the galactic plane, which implies that the shock wave may propagate into modestly disturbed medium. Note that several observational results have indicated inhomogeneity of ambient medium around SN 1006( [3,14,10]). In this paper, we will show the case of ∆ρ/ ρ 0 = 0.1 results by the same way as [15].…”

Section: Pos(icrc2015)485mentioning

confidence: 99%

On Cosmic-Ray Production Efficiency at Realistic Supernova Remnant Shocks

Shimoda¹,

Inoue²,

Ohira

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We demonstrate by using three-dimensional magnetohydrodynamics simulations that the cosmicray (CR) production efficiency at supernova remnants (SNRs) is over-predicted if it is based on proper motion measurements of Hα filaments in combination with Rankine-Hugoniot relations. Density fluctuations of upstream medium make shock waves oblique almost everywhere. For oblique shock, the kinetic energy of the shock wave is transferred into that of downstream turbulence as well as thermal energy related to the shock velocity component normal to the shock surface. Our synthetic observations shows that the apparent CR production efficiency as estimated from a lower downstream temperature, depends on the amplitude of density fluctuations of the upstream medium. They are roughly consistent with our analytical estimation of the efficiency. When the upstream medium has density fluctuations of typical diffuse interstellar medium, the apparent CR productions efficiency is observed as 10-40 %.

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Shock-Cloud Interaction and Particle Acceleration in the Southwestern Limb of Sn 1006

Cited by 32 publications

References 28 publications

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

Three-dimensional magnetohydrodynamic studies of the non-thermal X-ray morphologies of SN 1006

On Cosmic-Ray Production Efficiency at Realistic Supernova Remnant Shocks

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