Discovery of a jet-like structure with overionized plasma in the SNR IC 443

Greco, E.; Miceli, M.; Orlando, S.; Peres, G.; Troja, E.; Bocchino, F.

doi:10.1051/0004-6361/201832733

Cited by 23 publications

(49 citation statements)

References 26 publications

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“…On the other hand, alternative cooling processes suggest that the overionization of the ejecta is due to their rapid free expansion following their early heating in the case of an interaction with dense clouds Article published by EDP Sciences A14, page 1 of 14 A&A 649, A14 (2021) (e.g. Miceli et al 2010;Zhou et al 2011;Yamaguchi et al 2018;Greco et al 2018). It is, therefore, important to carefully model the evolution of MM SNRs by describing in detail their interaction with the complex environment.…”

Section: Introductionmentioning

confidence: 99%

“…Several works have investigated the physical and chemical properties of IC 443 via radio (Leahy 2004;Lee et al 2008Lee et al , 2012, infrared (Rho et al 2001;Su et al 2014), X-ray (Troja et al 2006(Troja et al , 2008Greco et al 2018) and γ-ray (Tavani et al 2010;Abdo et al 2010) observations. IC 443 is interacting with a molecular cloud in the northwestern (NW) and southeastern (SE) areas and with an atomic cloud in the northeast (NE).…”

Section: Introductionmentioning

confidence: 99%

“…The remnant shows a great diversity and superposition of shocks which may be a natural result of the shock-cloud interactions in a clumpy interstellar medium (Snell et al 2005;Shinn et al 2011). Indications for the presence of overionized plasma have also been found (Yamaguchi et al 2009;Matsumura et al 2017;Greco et al 2018), with their origin still under debate.…”

Section: Introductionmentioning

confidence: 99%

“…The plerion nebula, discovered by Chandra (Olbert et al 2001) and previously studied by several authors (e.g., Bocchino et al 2001;Gaensler et al 2006;Swartz et al 2015), is situated in the southern part of the remnant, but its association with IC 443 is still debated considering its offcenter position. Recently, Greco et al (2018) detected a Mg-rich jet-like structure in the NW area of IC 443 close to the molecular cloud. Interestingly, the jet emission is mainly due to overionized plasma and its projection towards the remnant interior crosses the position of the neutron star at the time of the explosion of the progenitor star.…”

Section: Introductionmentioning

confidence: 99%

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Modeling the mixed-morphology supernova remnant IC 443

Ustamujic

Orlando

Greco

et al. 2021

A&A

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Context. The morphology and the distribution of material observed in supernova remnants (SNRs) reflect the interaction of the supernova (SN) blast wave with the ambient environment, the physical processes associated with the SN explosion, and the internal structure of the progenitor star. IC 443 is a mixed-morphology (MM) SNR located in a quite complex environment: it interacts with a molecular cloud in the northwestern and southeastern areas and with an atomic cloud in the northeast. Aims. In this work, we aim to investigate the origin of the complex morphology and multi-thermal X-ray emission observed in SNR IC 443 through the study of the effect of the inhomogeneous ambient medium in shaping its observed structure and an exploration of the main parameters characterizing the remnant. Methods. We developed a 3D hydrodynamic (HD) model for IC 443, which describes the interaction of the SNR with the environment, parametrized in agreement with the results of the multi-wavelength data analysis. We performed an ample exploration of the parameter space describing the initial blast wave and the environment, including the mass of the ejecta, the energy and position of the explosion, as well as the density, structure, and geometry of the surrounding clouds. From the simulations, we synthesized the X-ray emission maps and spectra and compared them with actual X-ray data collected by XMM-Newton. Results. Our model explains the origin of the complex X-ray morphology of SNR IC 443 in a natural way, with the ability to reproduce, for the first time, most of the observed features, including the centrally-peaked X-ray morphology (characteristic of MM SNRs) when considering the origin of the explosion at the position where the pulsar wind nebula CXOU J061705.3+222127 was at the time of the explosion. In the model that best reproduces the observations, the mass of the ejecta and the energy of the explosion are ~7 M⊙ and ~1 × 1051 erg, respectively. From the exploration of the parameter space, we find that the density of the clouds is n > 300 cm−3 and that the age of SNR IC 443 is ~8000 yr. Conclusions. The observed inhomogeneous ambient medium is the main property responsible for the complex structure and the X-ray morphology of SNR IC 443, resulting in a very asymmetric distribution of the ejecta due to the off-centered location of the explosion inside the cavity formed by the clouds. It can be argued that the centrally peaked morphology (typical of MM SNRs) is a natural consequence of the interaction with the complex environment. A combination of high resolution X-ray observations and accurate 3D HD modeling is needed to confirm whether this scenario is applicable to other MM SNRs.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Modeling the mixed-morphology supernova remnant IC 443

Ustamujic

Orlando

Greco

et al. 2021

A&A

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“…Their studies in X‐rays convey prime information on the energy output from the supernovae, stellar wind of massive stars, properties of the interstellar medium, or on the activity of the galactic center massive black hole Sgr A* (Decourchelle et al , and references therein). Recent progress in the field in terms of observations and modeling has been presented during this conference by An , Ferrand , Greco ; Matsumara , Yamaguchi , and Zhou .…”

Section: Breakthroughs Expected From Athena On the Astrophysics Of Exmentioning

confidence: 99%

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

et al. 2020

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The properties (temperature, density, chemical composition, velocity) of hot astrophysical plasma and the physical processes affecting them (heating/cooling, turbulence, shocks, acceleration) can be probed by high‐resolution X‐ray spectroscopy, to be complemented by high‐spatial‐resolution imaging. The paper presents the status of the European Space Agency's Advanced Telescope for High Energy Astrophysics (Athena) mission, particularly focusing on the science performance of its two focal‐plane instruments for studies of extended X‐ray sources: the wide‐field imager and the X‐ray integral field unit. This paper then provides a brief summary of the breakthroughs expected with Athena on the astrophysics of hot plasma, building on the vast heritage of the discoveries and revolutionary results obtained by Chandra and XMM‐Newton in this field. As of November 12, 2019, Athena successfully concluded its feasibility study, and has since then moved into the definition phase, with a launch date scheduled in the early 2030s.

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