Evidence for shock acceleration of high-energy electrons in the supernova remnant SN1006

Koyama, K.; Petre, Robert; Gotthelf, E. V.; Hwang, U.; Matsuura, M.; Ozaki, Masanori; Holt, S. S.

doi:10.1038/378255a0

Cited by 832 publications

(733 citation statements)

References 20 publications

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“…The evigweight procedure was used to facilitate the spectral analysis, but the imaging analysis was carried out via exposure maps. This data offers the same spatial resolution as ROSAT HRI (Winkler & Long 1997) but with energy resolution similar to that of ASCA (Koyama et al 1995). It is better in both respects than ROSAT PSPC (Willingale et al 1996).…”

Section: X-raymentioning

confidence: 97%

See 1 more Smart Citation

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

125

158

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Abstract. SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is thus a tracer of the maximum energy electrons may reach behind a shock. We have put together all XMM-Newton observations to build a full map of SN 1006. The very low brightness above 2 keV in the interior indicates that the bright non-thermal limbs are polar caps rather than an equator. This implies that the ambient magnetic field runs southwest to northeast, along the Galactic plane. We used a combined VLA/Parkes radio map to anchor the spectrum at low energy, and model the spectra with synchrotron emission from a cut-off power-law electron distribution, plus a thermal component. We present radial and azimuthal profiles of the cut-off frequency. The cut-off frequency decreases steeply with radius towards the center and with position angle away from the maximum emission. The maximum energy reached by accelerated particles, as well as their number, must be higher at the bright limbs than elsewhere. This implies interesting constraints for acceleration at perpendicular shocks. Overall the XMM-Newton data is consistent with the model in which the magnetic field is amplified where acceleration is efficient.

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Section: X-raymentioning

confidence: 97%

“…It dominates in the two bright limbs (northeast and southwest), whereas thermal (line) emission dominates in the center and towards the northwest and southeast (Koyama et al 1995). The spectral index in the X-rays (α = 1.9) is much steeper than in the radio (α = 0.6).…”

Section: Introductionmentioning

confidence: 97%

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

125

158

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“…CRs of heavier species like iron may reach energies near the "second knee" at around 10 17 eV. The detections of synchrotron X-rays in some SNRs have already shown evidence for the acceleration of electrons to ultrarelativistic energies at SNR shocks (Koyama et al 1995). On the other hand, there remains the unresolved issue as to how efficiently SNRs are accelerating high-energy protons compared to electrons.…”

Section: Origin Of Galactic Cosmic Raysmentioning

confidence: 95%

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Acero¹,

Aloisio²,

Amans³

et al. 2017

ApJ

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“…X-ray synchrotron emission from high energy electrons accelerated at the shock front up to TeV energies has been first observed in SN 1006 (Koyama et al 1995) and then in other young SNRs as, for example, G1.9+0.3 (Reynolds et al 2009), Vela Jr. (Slane et al 2001, Bamba et al 2005, and G353.6-0.7 (Tian et al 2010). Recently, TeV emission has been detected in SN 1006 (Acero et al 2010).…”

Section: Introductionmentioning

confidence: 97%

Probing the effects of hadronic acceleration at the SN 1006 shock front

et al. 2013

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Abstract. Supernova remnant shocks are strong candidates for being the source of energetic cosmic rays and hadron acceleration is expected to increase the shock compression ratio, providing higher post-shock densities. We exploited the deep observations of the XMM-Newton Large Program on SN 1006 to verify this prediction. Spatially resolved spectral analysis led us to detect X-ray emission from the shocked ambient medium in SN 1006 and to find that its density significantly increases in regions where particle acceleration is efficient. Our results provide evidence for the effects of acceleration of cosmic ray hadrons on the post-shock plasma in supernova remnants.

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Evidence for shock acceleration of high-energy electrons in the supernova remnant SN1006

Cited by 832 publications

References 20 publications

Geometry of the non-thermal emission in SN 1006

Geometry of the non-thermal emission in SN 1006

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Probing the effects of hadronic acceleration at the SN 1006 shock front

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