Supernova of 1006 (G327.6+14.6)

Abstract

SN 1006 (G327.6+14.6) was the brightest supernova (SN) witnessed in human history. As of one thousand years later, it stands out as an ideal laboratory to study Type Ia SNe and shocks in supernova remnants (SNRs). The present state of knowledge about SN 1006 is reviewed in this article. No star consistent with a surviving companion expected in the traditional single-degenerate scenario has been found, which favors a double-degenerate scenario for the progenitor of SN 1006. Both unshocked and shocked SN ejecta have been probed through absorption lines in ultraviolet spectra of background sources and thermal X-ray emission, respectively. The absorption studies suggest that the amount of iron is < 0.16 M_sun, which is significantly less than the range for normal SNe Ia. On the other hand, analyses of X-ray data reveal the distribution of shocked ejecta to be highly asymmetric especially for iron. Therefore, most of iron might have escaped from the ultraviolet background sources. Another important aspect with SN 1006 is that it was the first SNR in which synchrotron X-ray emission was detected from shells of the remnant, providing evidence that electrons are accelerated up to ~100 TeV energies at forward shocks. The bilateral symmetry of the synchrotron emission (bright in northeastern and southwestern limbs) is likely due to a polar cap geometry. The broadband (radio, X-ray, and gamma-ray) spectral energy distribution suggests that the gamma-ray emission is predominantly leptonic. At the northwestern shock, evidence for extreme, but less than mass proportional, temperature non-equilibration has been found by optical, ultraviolet, and X-ray observations.

A chapter in "Handbook of Supernovae" edited by Athem W. Alsabti and Paul Murdin (20 pages, 6 figures). Final print version can be found here: http://link.springer.com/referenceworkentry/10.1007/978-3-319-20794-0_45-2

References in corpus (15)

• Observational constraints on energetic particle diffusion in young SNRs: amplified magnetic field and maximum energy
• First detection of VHE gamma-rays from SN 1006 by H.E.S.S
• Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006
• Fast Variability of Nonthermal X-Ray Emission in Cassiopeia A: Probing Electron Acceleration in Reverse-Shocked Ejecta
• Spatial Structure and Collisionless Electron Heating in Balmer-dominated Shocks
• No surviving evolved companions to the progenitor of supernova SN 1006
• Variation of cosmic ray injection across supernova shocks
• The gas density around SN 1006
• The First X-Ray Proper-Motion Measurements of the Forward Shock in the Northeastern Limb of SN 1006
• Study of TeV shell supernova remnants at gamma-ray energies
• Evidence of a Curved Synchrotron Spectrum in the Supernova Remnant SN 1006
• Magnetic-Field Amplification in the Thin X-ray Rims of SN1006
• Probing Multiple Sight Lines through the SN 1006 Remnant by UV Absorption Spectroscopy
• 3D MHD simulation of polarized emission in SN 1006
• A high resolution UV absorption spectrum of supernova ejecta in SN1006

Cited by in corpus (6)

• Evolution and observational signatures of the cosmic ray electron spectrum in SN 1006
• Constraining the coherence scale of the interstellar magnetic field using TeV gamma-ray observations of supernova remnants
• Simulating TeV gamma-ray morphologies of shell-type supernova remnants
• Element Stratification in the Middle-Aged Type Ia Supernova Remnant G344.7-0.1
• Witnessing History: Rates and Detectability of Naked-Eye Milky-Way Supernovae
• Momentum deposition of supernovae with cosmic rays