On the metal abundances inside mixed-morphology supernova remnants: the case of IC 443 and G166.0+4.3

被引:24
作者
Bocchino, F. [1 ]
Miceli, M. [2 ]
Troja, E. [3 ,4 ]
机构
[1] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy
[2] Consorzio COMETA, I-95123 Catania, Italy
[3] Univ Palermo, Sez Astron, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy
[4] Sez Palermo, Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy
关键词
ISM: supernova remnants; ISM:; dust; extinction; X-rays: ISM; X-rays: individuals: IC 443; X-rays: individuals: G166.0+4.3; ISM; XMM-NEWTON OBSERVATIONS; FORMED DENSE SHELL; X-RAY-EMISSION; THERMAL CONDUCTION; MODELING W44; HOT INTERIOR; EJECTA; IC-443; EXPLOSION; EVOLUTION;
D O I
10.1051/0004-6361/200810742
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. Recent developments in the study of mixed morphology supernova remnants (MMSNRs) have revealed the presence of metal-rich X-ray emitting plasma inside a fraction of these remnants, a feature not properly addressed by traditional models for these objects. Aims. Radial profiles of thermodynamical and chemical parameters are needed for a fruitful comparison of data and model of MMSNRs, but these are available only in a few cases. Methods. We analyzed XMM-Newton data of two MMSNRs, namely IC 443 and G166.0+4.3, previously known to have solar metal abundances, and performed a spatially resolved spectral analysis of the X-ray emission. Results. We detected enhanced abundances of Ne, Mg and Si in the hard X-ray bright peak in the north of IC 443, and of sulphur in the outer regions of G166.0+4.3. The metal abundances are not distributed uniformly in both remnants. The evaporating clouds model and the radiative SNR model fail to reproduce consistently all the observational results. Conclusions. We suggest that further deep X-ray observations of MMSNRs may reveal more metal-rich objects. More detailed models including ISM-ejecta mixing are needed to explain the nature of this growing subclass of MMSNRs.
引用
收藏
页码:139 / 145
页数:7
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