The Radial Structure of SNR N103B

Details The Radial Structure of SNR N103B The Radial Structure of SNR N103B

2002-09-13

arxiv.org/abs/astro-ph/0209280v1

Astrophys.J. 582 (2003) 770-782

Astronomy and Astrophysics

Astrophysics

34 pages, including 7 tables and 7 figures, Accepted by ApJ

Scientific paper

10.1086/344717

We report on the results from a Chandra ACIS observation of the young, compact, supernova remnant N103B. The unprecedented spatial resolution of Chandra reveals sub-arcsecond structure, both in the brightness and in spectral variations. Underlying these small-scale variations is a surprisingly simple radial structure in the equivalent widths of the strong Si and S emission lines. We investigate these radial variations through spatially resolved spectroscopy using a plane-parallel, non-equilibrium ionization model with multiple components. The majority of the emission arises from components with a temperature of 1 keV: a fully ionized hydrogen component; a high ionization timescale (n_e*t > 10^12 s cm^-3) component containing Si, S, Ar, Ca, and Fe; and a low ionization timescale (n_e*t ~ 10^{11} s cm^-3) O, Ne, and Mg component. To reproduce the strong Fe Kalpha line, it is necessary to include additional Fe in a hot (> 2 keV), low ionization (n_e*t ~ 10^10.8 s cm^-3) component. This hot Fe may be in the form of hot Fe bubbles, formed in the radioactive decay of clumps of 56Ni. We find no radial variation in the ionization timescales or temperatures of the various components. Rather, the Si and S equivalent widths increase at large radii because these lines, as well as those of Ar and Ca, are formed in a shell occupying the outer half of the remnant. A shell of hot Fe is located interior to this, but there is a large region of overlap between these two shells. In the inner 30% of the remnant, there is a core of cooler, 1 keV Fe. We find that the distribution of the ejecta and the yields of the intermediate mass species are consistent with model prediction for Type Ia events.

Affiliated with

Also associated with

No associations

Rating

The Radial Structure of SNR N103B does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The Radial Structure of SNR N103B, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Radial Structure of SNR N103B will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-356184