Astronomy and Astrophysics – Astrophysics
Scientific paper
2002-03-11
Mon.Not.Roy.Astron.Soc. 333 (2002) 241
Astronomy and Astrophysics
Astrophysics
8 pages, 8 figures, submitted to A&A
Scientific paper
10.1046/j.1365-8711.2002.05320.x
The X-ray emission from the young supernova remnant (SNR) N103B is measured and analysed using the high-resolution cameras and spectrometers on board XMMM and CHANDRA. The spectrum from the entire remnant is reproduced very well with three plasma components of kT=0.55, 0.65, and 3.5 keV, corresponding roughly to line emission by the O-K, Fe-L, and Fe-K species, respectively. Narrow band images reveal different morphologies for each component. The kT=0.65keV component, which dominates the emission measure (4.5E65m^{-3}), is in ionisation equilibrium. This provides a lower limit of 3000 yrs to the age of the remnant, which is considerably older than the previously assumed age of the remnant (1500 yrs). Based on the measured energy of the Fe-K feature at 6.5 keV, the hot (3.5 keV) component is found to be recently shocked (~200 yrs) and still ionising. The high elemental abundances of O and Ne and the low abundance of Fe could imply that SNR N103B originated from a type II supernova (SN) rather than a type Ia SN as previously thought.
Behar Ehud
Bleeker Johan A. M.
Kaastra Jelle S.
Kahn Steve M.
Mewe Rolf
No associations
LandOfFree
High-Resolution X-ray imaging and spectroscopy 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 High-Resolution X-ray imaging and spectroscopy of SNR N103B, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and High-Resolution X-ray imaging and spectroscopy of SNR N103B will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-619866