Kinematics of the Molecular Hydrogen Associated with the Supernova Remnant IC 443

Rosado, M.; Arias, L.; Ambrocio-Cruz, P.

doi:10.1086/509505

Cited by 22 publications

(21 citation statements)

References 31 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In the case of IC 443, these conditions can be accommodated for the solutions in Table 1, except perhaps for the very massive cloud located close to the SNR at d snr = 2 pc, for which would imply a cloud average density higher than usually found, although even this might also be possible given the small‐scale clumps found therein (e.g. see Rosado, Arias & Ambrocio‐Cruz 2007).…”

Section: The Cosmic Ray Diffusion Modelmentioning

confidence: 86%

The GeV to TeV connection in the environment of SNR IC 443

Torres¹,

Marrero²,

Pozo³

2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We have recently interpreted the source MAGIC J0616+225 as a result of delayed TeV emission of cosmic-rays diffusing from IC 443 and interacting with a cloud in the foreground of the remnant. This model was used to make predictions for future observations, especially those to be made with the Fermi satellite. Just recently, AGILE, Fermi, and VERITAS have released new results of their observations of IC 443. In this work, we compare them with the predictions of our model, exploring the GeV to TeV connection in this region of space. We use Fermi data to consider the possibility of constraining the cosmic-ray diffusion features of the environment. We analyze the cosmic-ray distributions, their interactions, and a possible detection of the SNR environment in the neutrino channel.Comment: Accepted for publication in MNRAS. 20 pages, 10 figures, 1 tabl

show abstract

Section: The Cosmic Ray Diffusion Modelmentioning

confidence: 86%

The GeV to TeV connection in the environment of SNR IC 443

Torres¹,

Marrero²,

Pozo³

2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…IC 443 is one of the most thoroughly studied interacting SNRs, with rich evidence including OH masers from the central and southeast regions (Hewitt et al 2006),CO line ratio (Seta et al 1998), molecular line broadening (Dickman et al 1992) and near‐infrared shocked H 2 emission (Rosado, Arias & Ambrocio‐Cruz 2007).…”

Section: Application To Individual Snrsmentioning

confidence: 99%

γ-rays from molecular clouds illuminated by accumulated diffusive protons - II. Interacting supernova remnants

Li¹,

Chen²

2012

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Recent observations reveal that spectral breaks at ∼GeV are commonly present in Galactic γ‐ray supernova remnants (SNRs) interacting with molecular clouds and that most of them have a spectral (E2dF/dE) ‘platform’ extending from the break to lower energies. In Paper I, we developed an accumulative diffusion model by considering an accumulation of the diffusive protons escaping from the shock front throughout the history of the SNR expansion. In this paper, we improve the model by incorporating the finite volume of molecular clouds, demonstrate the model dependence on particle diffusion parameters and cloud size, and apply it to nine interacting SNRs (W28, W41, W44, W49B, W51C, Cygnus Loop, IC443, CTB 37A and G349.7+0.2). This refined model naturally explains the GeV spectral breaks and, in particular, the ‘platforms’, together with available TeV data. We find that the index of the diffusion coefficient δ is in the range 0.5–0.7, similar to the Galactic averaged value, and the diffusion coefficient for cosmic rays around the SNRs is essentially two orders of magnitude lower than the Galactic average (χ∼ 0.01), which is a good indication for the suppression of cosmic‐ray diffusion near SNRs.

show abstract

“…Recent X-ray studies include those of Troja et al (2008), Bykov et al (2008), and Troja et al (2006), while infrared and radio studies include Noriega-Crespo et al (2008), Bykov et al (2008), Lee et al (2008), Rosado et al (2007), Leahy (2004), and references therein. The remnant was classified as mixed-morphology by Rho & Petre (1998), based on observations with the ROSAT satellite.…”

Section: Ic 443mentioning

confidence: 99%

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

Bocchino

Miceli

Troja

2009

A&A

View full text Add to dashboard Cite

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.

show abstract

Kinematics of the Molecular Hydrogen Associated with the Supernova Remnant IC 443

Cited by 22 publications

References 31 publications

The GeV to TeV connection in the environment of SNR IC 443

The GeV to TeV connection in the environment of SNR IC 443

γ-rays from molecular clouds illuminated by accumulated diffusive protons - II. Interacting supernova remnants

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

Contact Info

Product

Resources

About