Cosmic-Ray Acceleration Efficiency Versus Temperature Equilibration: The Case of SNR 0509-67.5

Helder, E. A.; Kosenko, D.; Vink, Jacco

doi:10.1088/2041-8205/719/2/l140

Cited by 45 publications

(69 citation statements)

References 36 publications

(47 reference statements)

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“…The point showed in Fig. 3 refers to the FWHM measured in the SW rim of the remnant [19], and the uncertainty in the shock speed correspond to the theoretical estimate done in [20]. Unfortunately the big uncertainty in the determination of the shock speed prevents a firm conclusion on the CR acceleration efficiency.…”

Section: Snr 0509-675mentioning

confidence: 77%

Using optical lines to study particle acceleration at supernova remnants

Morlino

2014

Nuclear Physics B - Proceedings Supplements

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The shocks of several young supernova remnants (SNR) are often associated with very thin optical filaments dominated by Balmer emission resulting from charge-exchange and collisional excitation between neutral Hydrogen from the interstellar medium and shocked protons and electrons. Optical lines are a direct probe of the conditions at the shock, in particular the width of the narrow and broad components reflect the temperature upstream and downstream of the shock, respectively. When the shock accelerate efficiently non-thermal particles, the shock structure changes producing anomalous Balmer lines and it is possible to use their line shape and their spatial profile to check the efficiency of SNR shocks in accelerating cosmic rays. Here we illustrate the kinetic theory of shock acceleration in presence of neutrals with some applications to young SNRs. We show that in three cases (RCW 86, SNR 0509-67.5 and Tycho) anomalous Balmer lines can be explained assuming that a fraction of ∼ 10% of the total shock kinetic energy is converted into not thermal particles, while in one single case, the northwestern part of SN 1006, there is no evidence of efficient acceleration.

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Section: Snr 0509-675mentioning

confidence: 77%

Using optical lines to study particle acceleration at supernova remnants

Morlino

2014

Nuclear Physics B - Proceedings Supplements

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“…In this paper we report our analysis of SNR0509−67.5, one of the three smallest Type Ia SNRs in the LMC (i.e. Helder et al 2010;di Stefano & Kilic 2012). SNR0509−67.5 has been studied extensively in the past.…”

Section: Introductionmentioning

confidence: 99%

Nature of the Diffuse Source and Its Central Point-like Source in SNR 0509–67.5

Litke

Chu

Holmes

et al. 2017

ApJ

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We examine a diffuse emission region near the center of SNR0509−67.5 to determine its nature. Within this diffuse region we observe a point-like source that is bright in the near-IR, but is not visible in the B and V bands. We consider an emission line observed at 6766 Å and the possibilities that it is Lyα, Hα, and [O II]λ3727. We examine the spectral energy distribution (SED) of the source, comprised of Hubble Space Telescope B, V, I, J, and H bands in addition to Spitzer/IRAC 3.6, 4.5, 5.8,and8 μm bands. The peak of the SED is consistent with a background galaxy at z≈0.8±0.2 and a possible Balmer jump places the galaxy at z≈0.9±0.3. These SED considerations support the emission line's identification as [O II]λ3727. We conclude that the diffuse source in SNR0509−67.5 is a background galaxy at z≈0.82. Furthermore, we identify the point-like source superposed near the center of the galaxy as its central bulge. Finally, we find no evidence for a surviving companion star, indicating a double-degenerate origin for SNR 0509−67.5.

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“…We obtained VLT/FORS2 observations for the LMC remnant 0509-67.5 as well [8], resulting in kT p of 15.9±0.9 keV for the SW shock, for which we obtained a lower limit on the shock velocity of 5000 km/s, leading to β ≤ 0.58. This velocity is based on the line broadening as obtained with the XMM-Newton/RGS instrument [12], together with the age as determined from light echos [17] and models for the evolution of a supernova remnant.…”

Section: Snr 0509-675mentioning

confidence: 90%

Cosmic-ray acceleration efficiency of the supernova remnants RCW 86 and SNR 0509-67.5

Helder¹,

Vink²

2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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We study the effect of cosmic-ray acceleration on the plasma temperature behind shock fronts, in order to characterize the cosmic-ray acceleration efficiencies. We combine post-shock plasma temperatures with shock velocities and show that this leads to a direct measurement of the cosmicray pressure behind the shock front. Additionally, we tie this pressure directly to the fraction of energy taken away from the shock by escaping particles. We show that at least some young supernova remnants transfer a significant amount of their energy into cosmic rays and these cosmic rays take away a substantial amount of the supernova energy by escaping the remnant. PoS(Texas 2010)142Cosmic-ray acceleration efficiency of RCW 86 and SNR 0509-67.

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Cosmic-Ray Acceleration Efficiency Versus Temperature Equilibration: The Case of SNR 0509-67.5

Cited by 45 publications

References 36 publications

Using optical lines to study particle acceleration at supernova remnants

Using optical lines to study particle acceleration at supernova remnants

Nature of the Diffuse Source and Its Central Point-like Source in SNR 0509–67.5

Cosmic-ray acceleration efficiency of the supernova remnants RCW 86 and SNR 0509-67.5

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