2010A&A...519A..11K


Query : 2010A&A...519A..11K

2010A&A...519A..11K - Astronomy and Astrophysics, volume 519, A11-11 (2010/9-1)

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0. An XMM-Newton and Chandra study.

KOSENKO D., HELDER E.A. and VINK J.

Abstract (from CDS):

We present a detailed analysis of the XMM-Newton and Chandra X-ray data of the young type Ia supernova remnant SNR 0519-69.0, which is situated in the Large Magellanic Cloud. We used data from both the Chandra ACIS and XMM-Newton EPIC MOS instruments, and high resolution X-ray spectra obtained with the XMM-Newton reflection grating spectrometer (RGS). Our analysis of the spatial distribution of X-ray line emission using the Chandra data shows that there is a radial stratification of oxygen, intermediate mass elements (IME) and iron, with the emission from more massive elements peaking more toward the center. Using a deprojection technique we measure a forward shock radius of 4.0±0.3pc and a reverse shock radius of 2.7±0.4pc. We took the observed stratification of the shocked ejecta into account in the modeling of the X-ray spectra, for which we used multi-component non-equilibrium ionization models, with the components corresponding to layers dominated by one or two elements. An additional component was added in order to represent the shocked interstellar medium, which mostly contributed to the continuum emission. This multicomponent model fits the data adequately, and was also employed to characterize the spectra of distinct regions extracted from the Chandra data. From our spectral analysis we find that the approximate fractional masses of shocked ejecta for the most abundant elements are: MO≃32%, MSi/S≃7%/5%, MAr+Ca≃1% and MFe≃55%. From the continuum component we derive a circumstellar density of nH=2.4±0.2cm–3. This density, together with the measurements of the forward and reverse shock radii suggest an age of 0519-69.0 of 450±200yr, somewhat lower than, but consistent with the age estimate based on the extent of the light echo (600±200yr). Finally, from the high resolution RGS spectra we measured a Doppler broadening of σ=1873±50km/s, from which we derive a forward shock velocity of vFS=2770±500km/s. We discuss our results in the context of single degenerate explosion models, using semi-analytical and numerical modeling, and compare the characteristics of 0519-69.0 with those of other type Ia supernova remnants.

Abstract Copyright:

Journal keyword(s): X-rays: individual: SNR0519-69.0 - ISM: supernova remnants

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1146 1
2 SNR J050854-684447 SNR 05 08 58.7 -68 43 46           ~ 151 2
3 SNR B0509-67.5 SNR 05 09 31 -67 31.3           ~ 211 0
4 SNR B0519-69.0 SNR 05 19 35.14 -69 02 00.5           ~ 148 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16407 1
6 SN 2002bo SN* 10 18 06.51 +21 49 41.7   13.95       SNIa 297 1
7 SN 1991T SN* 12 34 10.20 +02 39 56.4   11.70 11.51     SNIapec 748 1
8 SN 1996X SN* 13 18 01.13 -26 50 45.3   12.99 13.00     SNIa 185 1
9 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1288 1
10 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 766 4
11 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2646 1

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2022.12.03-14:26:12

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