High-Resolution X-ray imaging and spectroscopy of N 103B

摘要: The X-ray emission from the young supernova remnant (SNR) N 103B is measured and analysed using high-resolution cameras spectrometers on board XMM-Newton  and Chandra . spectrum entire is reproduced very well with three plasma components of $kT_{\rm e} = 0.55$, 0.65, and 3.5 keV, corresponding roughly to line by O–K, Fe–L, Fe–K species, respectively. Narrow band images reveal different morphologies for each component. 0.65$ keV component, which dominates measure ($4.5\times10^{65}$ m -3 ), in ionisation equilibrium. This provides a lower limit 1200 yrs age remnant, agreement previously assumed remnant (1500 yrs). Based energy feature at 6.5 keV, hot (3.5 keV) component found be recently shocked (~200 yrs) still ionising. high elemental abundances of O and Ne low abundance Fe could imply that N 103B originated type II (SN) rather than type Ia SN as thought.