Thermal and Nonthermal Emission from the Forward Shock in Tycho's Supernova Remnant

Details Thermal and Nonthermal Emission from the Forward Shock in Tycho's Supernova Remnant Thermal and Nonthermal Emission from the Forward Shock in Tycho's Supernova Remnant

2002-08-27

arxiv.org/abs/astro-ph/0208485v2

Astrophys.J. 581 (2002) 1101-1115

Astronomy and Astrophysics

Astrophysics

ApJ, in press; 32 pages LaTeX, 9 postscript figures; replaced version to better match ApJ version

Scientific paper

10.1086/344366

We present Chandra X-ray images of Tycho's supernova remnant that delineate its outer shock as a thin, smooth rim along the straight northeastern edge and most of the circular western half. The images also show that the Si and S ejecta are highly clumpy, and have reached near the forward shock at numerous locations. Most of the X-ray spectra that we examine along the rim show evidence of line emission from Si and S ejecta, while the continuum is well-represented by either a thermal or nonthermal model. If the continuum is assumed to be thermal, the electron temperatures at the rim are all similar at about 2 keV, while the ionization ages are very low, because of the overall weakness of the line emission. These electron temperatures are substantially below those expected for equilibration of the electron and ion temperatures, assuming shock velocities inferred from radio and X-ray expansion measurements; the electron to mean temperature ratios are <~0.1-0.2, indicating that collisionless heating of the electrons at the shock is modest. The nonthermal contribution to these spectra may be important, but cannot be strongly constrained by these data. It could account for as much as half of the flux in the 4-6 keV energy range, based on an extrapolation of the hard X-ray spectrum above 10 keV.

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