The radial structure of supernova remnant N103b

Karen T. Lewis, David N. Burrows, John P. Hughes, Patrick O. Slane, Gordon P. Garmire, John A. Nousek

Research output: Contribution to journalArticle

42 Citations (Scopus)

Abstract

We report on the results from a Chandra ACIS observation of the young, compact, supernova remnant N103B. The unprecedented spatial resolution of Chandra reveals subarcsecond structure, in both the brightness and 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, nonequilibrium 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 (net > 1012 s cm-3) component containing Si, S, Ar, Ca, and Fe; and a low ionization timescale (n et ∼ 1011 s cm-3) O, Ne, and Mg component. To reproduce the strong Fe Kα line, it is necessary to include additional Fe in a hot (> 2 keV), low ionization timescale (net ∼ 10 10.8 s cm-3) component. This hot Fe might 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 la events.

Original languageEnglish (US)
Pages (from-to)770-782
Number of pages13
JournalAstrophysical Journal
Volume582
Issue number2 I
DOIs
StatePublished - Jan 10 2003

Fingerprint

supernova remnants
ionization
timescale
shell
radioactive decay
nonequilibrium ionization
ejecta
K lines
bubble
spatial resolution
clumps
temperature
spectroscopy
coolers
hydrogen
brightness
bubbles
prediction
radii
predictions

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Lewis, K. T., Burrows, D. N., Hughes, J. P., Slane, P. O., Garmire, G. P., & Nousek, J. A. (2003). The radial structure of supernova remnant N103b. Astrophysical Journal, 582(2 I), 770-782. https://doi.org/10.1086/344717
Lewis, Karen T. ; Burrows, David N. ; Hughes, John P. ; Slane, Patrick O. ; Garmire, Gordon P. ; Nousek, John A. / The radial structure of supernova remnant N103b. In: Astrophysical Journal. 2003 ; Vol. 582, No. 2 I. pp. 770-782.
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Lewis, KT, Burrows, DN, Hughes, JP, Slane, PO, Garmire, GP & Nousek, JA 2003, 'The radial structure of supernova remnant N103b', Astrophysical Journal, vol. 582, no. 2 I, pp. 770-782. https://doi.org/10.1086/344717

The radial structure of supernova remnant N103b. / Lewis, Karen T.; Burrows, David N.; Hughes, John P.; Slane, Patrick O.; Garmire, Gordon P.; Nousek, John A.

In: Astrophysical Journal, Vol. 582, No. 2 I, 10.01.2003, p. 770-782.

Research output: Contribution to journalArticle

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