2000/05/18 by F. Bocchino, J. Vink, Bocchino, F. +8
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0005369
13 pages, A&A in press
arxiv created 2000/05/18 · openalex publication_date 2000/05/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a spectral analysis of the Northern and Southwestern rim of the RCW86 X-ray shell, pointing out the remarkable differences between these two parts of the same object. In the North, a single temperature Non Equilibrium of Ionization emission model describes the data well, and the derived abundances of O, Ne, Mg, Si, S, Ar and Fe are in agreement with expected metal depletion behind a fast shock moving in the interstellar medium. If the initial explosion energy was ∼ 1051 erg, the derived distance and age are 1.18+0.17-0.16 kpc and 1630+440-360 yr, fully consistent with the association to the historical supernova SN185. The X-ray emission from the SW is described by a two-temperature emission model with kT\rm h=5.7 keV and kT\rm l=1.0 keV. There is evidence of overabundant metals in the high-temperature component, thus indicating the presence of ejecta. In this case, a Type Ia SN is to be preferred over a more energetic Type II event, which would imply a more distant and older remnant fully in its Sedov phase.