DISCOVERY OF ENHANCED RADIATIVE RECOMBINATION CONTINUA OF He-LIKE IRON AND CALCIUM FROM IC 443 AND ITS IMPLICATIONS

Ohnishi, Teruaki; Uchida, Hiroyuki; Tsuru, Takeshi Go; Koyama, K.; Masai, K.; Sawada, Makoto

doi:10.1088/0004-637x/784/1/74

Cited by 21 publications

(23 citation statements)

References 23 publications

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“…It implies that the 6.4 keV line emission does not originate from the thermal plasma. In fact, the IC 443's plasma is known to be in the recombining state [15,16], and it is impossible that the recombining plasma radiates a detectable 6.4 keV line. The 6.4 keV line intensity is associated with the MCs.…”

Section: Observation Resultsmentioning

confidence: 99%

Low-energy Cosmic Rays in Supernova Remnants Interacting with Molecular Clouds

Nobukawa¹

2020

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources - XIII — PoS(MULTIF2019)

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Information on low-energy cosmic rays (CRs) below the MeV band has been very limited due to difficulty of measurements in contrast to high-energy (GeV-TeV) CRs, which are observable via gamma-rays. Only ionization rate provides indirect information on low-energy CRs. The neutral iron line at 6.4 keV can be a new effective probe. Utilizing the Suzaku archive data, we searched supernova remnants (SNRs) for the particle-induced 6.4 keV line. Since accelerated CR particles can produce the 6.4 keV line when they interact with molecular clouds, we focused on SNRs interacting with molecular clouds. The 6.4 keV line probably induced by CR particles has been found from more than 10 SNRs. More than a half of the SNRs also show gamma-ray emission. We found that both the 6.4 keV line and gamma-ray emissions can be explained by a CR escaping scenario at least for W28, W44, and IC 443. It indicates that low-energy CRs producing the 6.4 keV line have been accelerated at the SNRs together with high-energy CRs.

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Section: Observation Resultsmentioning

confidence: 99%

Low-energy Cosmic Rays in Supernova Remnants Interacting with Molecular Clouds

Nobukawa¹

2020

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources - XIII — PoS(MULTIF2019)

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“…However we cannot exclude the more exotic case of RP, because many of MM SNRs that were previously known as a CIE plasma are now found to be RP (e.g. Yamaguchi et al 2009;Ozawa et al 2009;Ohnishi et al 2011;Uchida et al 2012;Sawada et al 2012;Yamauchi et al 2013;Ohnishi et al 2014;Yamauchi et al 2014).…”

Section: Sgr a Eastmentioning

confidence: 98%

ASTRO-H White Paper - Plasma Diagnostic and Dynamics of the Galactic Center Region

Koyama¹,

Kataoka²,

Nobukawa³

et al. 2014

Preprint

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The most characteristic high-energy phenomena in the Galactic center (GC) region is the presence of strong K-shell emission lines from highly ionized Si, S, Ar, Ca, Fe and Ni, which form the Galactic Center X-ray Emission (GCXE). These multiple lines suggest that the GCXE is composed of at least two plasmas with temperatures of ∼1 and∼7 keV. The GCXE also exhibits the K-shell lines from neutral Si, S, Ar, Ca, Fe and Ni atoms. A debatable issue is the origin of the GCXE plasma; whether it is a diffuse plasma or integrated emission of many unresolved point sources such as cataclysmic variables and active binaries. Detailed spectroscopy for these lines may provide a reliable picture of the GCXE plasma. The origin of the K-shell lines from neutral atoms is most likely the fluorescence by X-rays from a putative past flare of Sgr A * . Therefore ASTRO-H may provide unprecedented data for the past light curve of Sgr A * . All these lines may provide key information for the dynamics of the GCXE, using possible Doppler shift and/or line broadening. This paper overviews these line features and the previous interpretation of their origin. We propose extended or revised science with the ASTRO-H observations of some select objects in the GC region.

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“…This rapid cooling could arise from thermal conduction (Kawasaki et al 2002b), adiabatic expansion (Itoh & Masai 1989), or interaction with dense material (Dwarkadas 2005). To date, overionization has only been detected in mixed-morphology SNRs (e.g., W49B: Kawasaki et al 2005;Ozawa et al 2009;Miceli et al 2010;Lopez et al 2013b;IC443: Kawasaki et al 2002aYamaguchi et al 2009;Ohnishi et al 2014;Matsumura et al 2017), many of which have been classified as CC SNRs based on their elemental abundances, their morphologies, and the dense material in their environments. We find that the ejecta emission of 3C 397 is best described by an underionized plasma, where the temperature of the electrons is greater than the ionization temperature, contrary to an overionized plasma.…”

Section: Explosive Origin Constraints From Plasma Ionization State An...mentioning

confidence: 99%

Evidence of a Type Ia Progenitor for Supernova Remnant 3C 397

Martínez-Rodríguez,

Lopez,

Auchettl

et al. 2020

Preprint

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The explosive origin of the young supernova remnant (SNR) 3C 397 (G41.1−0.3) is debated. Its elongated morphology and proximity to a molecular cloud are suggestive of a core-collapse (CC) SN origin, yet recent X-ray studies of heavy metals show chemical yields and line centroid energies consistent with a Type Ia SN. In this paper, we analyze the full X-ray spectrum from 0.7−10 keV of 3C 397 observed with Suzaku and compare the line centroid energies, fluxes, and elemental abundances of intermediate-mass and heavy metals (Mg to Ni) to Type Ia and CC hydrodynamical model predictions. Based on the results, we conclude that 3C 397 likely arises from an energetic Type Ia explosion in a high-density ambient medium, and we show that the progenitor was a near Chandrasekhar mass white dwarf.

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DISCOVERY OF ENHANCED RADIATIVE RECOMBINATION CONTINUA OF He-LIKE IRON AND CALCIUM FROM IC 443 AND ITS IMPLICATIONS

Cited by 21 publications

References 23 publications

Low-energy Cosmic Rays in Supernova Remnants Interacting with Molecular Clouds

Low-energy Cosmic Rays in Supernova Remnants Interacting with Molecular Clouds

ASTRO-H White Paper - Plasma Diagnostic and Dynamics of the Galactic Center Region

Evidence of a Type Ia Progenitor for Supernova Remnant 3C 397

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