The temperature dependence of luminescence from a-Si: H/a-Si<sub>3</sub>N<sub>4</sub>: H superlattices

Yamaguchi, Masatoshi; Morigaki, Kazuo

doi:10.1080/13642818908228821

Cited by 23 publications

(36 citation statements)

References 12 publications

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“…4) within the confidence range. However, considering the large error bars due to low statistics, we could also make a similar statement for the Fe abundance value and an unattained reverse shock, as is reported in many Type Ia SNRs like SN1006 (Yamaguchi et al 2008a), Tycho (Tamagawa et al 2009) and G337.2-0.7 (Rakowski et al 2001), the Fe abundance being less than the expected value produced in a Type Ia SN. Considering all these cases, we can predict that the remnant may originate from a Type Ia SN explosion.…”

Section: Relative Abundances In the Ejectasupporting

confidence: 82%

“…From the equation t = τ /n e , the age of G346.6−0.2 is calculated to be ∼1.1 × 10 4 yr. Thus, this remnant is likely to be the oldest known ejecta-dominated shell-like SNR (compared with SN1006, RCW86, G337.2-0.7 and G309.2-0.6 at ∼1000 (Yamaguchi et al 2008a), ∼1800 (Yamaguchi et al 2008b), 2000-4500 and 700-4000 yr (Rakowski, Hughes & Slane 2001), respectively).…”

Section: Thermal Emissionmentioning

confidence: 93%

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Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

Sezer

Gök

Hüdaverdi

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present here the results of an X‐ray analysis of Galactic supernova remnant G346.6−0.2 observed with Suzaku. K‐shell emission lines of Mg, Si, S, Ca and Fe are detected clearly for the first time. Strong emission lines of Si and S imply that the X‐ray emission nature of G346.6−0.2 is ejecta‐dominated. The ejecta‐dominated emission is well fitted by a combined model consisting of a thermal plasma in non‐equilibrium ionization and a non‐thermal component, which can be regarded as synchrotron emission with a photon index of Γ∼ 0.6. An absorbing column density of NH∼ 2.1 × 1022 cm−2 is obtained from the best fit, implying a high‐density medium, high electron temperature of kTe∼ 1.2 keV and ionization time‐scale of net∼ 2.9 × 1011 cm−3 s, indicating that this remnant may be far from full ionization equilibrium. The relative abundances from the ejecta show that the remnant originates from a Type Ia supernova explosion.

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Section: Relative Abundances In the Ejectasupporting

confidence: 82%

Section: Thermal Emissionmentioning

confidence: 93%

Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

Sezer

Gök

Hüdaverdi

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…We then derive the elapsed time since the dense molecular clouds was heated t = 4.0 × 10 10 f 0.5 s < 1300 yr This value is much less than the maximum age of 5000 yr, and hence the high temperature plasma likely has been heated recently. This situation is very similar to the Magellanic SNR N49 and Galactic SNR RCW 86 (Park et al 2003;Yamaguchi et al 2008). To confirm the scenario, we need more detailed studies of spatially resolved X-ray spectroscopy for the whole remnant.…”

Section: Shocked Molecular Cloudsmentioning

confidence: 59%

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

Sano

Matsumura

Nagaya

et al. 2019

ApJ

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We carried out new 12 CO(J = 1-0, 3-2) observations of a N63A supernova remnant (SNR) from the LMC using ALMA and ASTE. We find three giant molecular clouds toward the northeast, east, and near the center of the SNR. Using the ALMA data, we spatially resolved clumpy molecular clouds embedded within the optical nebulae in both the shock-ionized and photoionized lobes discovered by previous Hα and [S ii] observations. The total mass of the molecular clouds is ∼800 M ⊙ for the shockionized region and ∼1700 M ⊙ for the photoionized region. Spatially resolved X-ray spectroscopy reveals that the absorbing column densities toward the molecular clouds are ∼1.5-6.0 × 10 21 cm −2 , which are ∼1.5-15 times less than the averaged interstellar proton column densities for each region. This means that the X-rays are produced not only behind the molecular clouds, but also in front of them. We conclude that the dense molecular clouds have been completely engulfed by the shock waves, but have still survived erosion owing to their high-density and short interacting time. The X-ray spectrum toward the gas clumps is well explained by an absorbed power-law or high-temperature plasma models in addition to the thermal plasma components, implying that the shock-cloud interaction is efficiently working for both the cases through the shock ionization and magnetic field amplification. If the hadronic gamma-ray is dominant in the GeV band, the total energy of cosmic-ray protons is calculated to be ∼0.3-1.4 × 10 49 erg with the estimated ISM proton density of ∼190 ± 90 cm −3 , containing both the shock-ionized gas and neutral atomic hydrogen.

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“…These spectra have been corrected for NXB, using the spectra generated by xisnxbgen (Tawa et al 2008). Yamaguchi et al (2008Yamaguchi et al ( , 2011 showed that the emission in RCW 86 can be well reproduced by two temperature plasma and power-law component model, and taking into account Galactic absorption. The low-temperature component corresponds to the shock-heated ISM, and is modeled with the vpshock model.…”

Section: Integrated Spectra In Each Fovmentioning

confidence: 99%

A Systematic Study of the Thermal and Nonthermal Emission in the Supernova Remnant RCW 86 With Suzaku

Tsubone

Sawada

Bamba

et al. 2017

ApJ

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Diffusive shock acceleration by the shockwaves in supernova remnants (SNRs) is widely accepted as the dominant source for Galactic cosmic rays. However, it is unknown what determines the maximum energy of accelerated particles. The surrounding environment could be one of the key parameters. The SNR RCW 86 shows both thermal and non-thermal X-ray emission with different spatial morphologies. These emission originate from the shock-heated plasma and accelerated electrons respectively, and their intensities reflect their density distributions. Thus, the remnant provides a suitable laboratory to test possible association between the acceleration efficiency and the environment. In this paper, we present results of spatially resolved spectroscopy of the entire remnant with Suzaku. The spacially-resolved spectra are well reproduced with a combination of a power-law for synchrotron emission and a two-component optically thin thermal plasma, corresponding to the shocked interstellar medium (ISM) with kT of 0.3-0.6 keV and Fe-dominated ejecta. It is discovered that the photon index of the nonthermal component becomes smaller with decreasing the emission measure of the shocked ISM, where the shock speed has remained high. This result implies that the maximum energy of accelerated electrons in RCW 86 is higher in the low-density and higher shock speed regions.

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The temperature dependence of luminescence from a-Si: H/a-Si₃N₄: H superlattices

Cited by 23 publications

References 12 publications

Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

A Systematic Study of the Thermal and Nonthermal Emission in the Supernova Remnant RCW 86 With Suzaku

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The temperature dependence of luminescence from a-Si: H/a-Si3N4: H superlattices

Cited by 23 publications

References 12 publications

Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

Suzaku observations of ejecta-dominated Galactic supernova remnant G346.6−0.2

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

A Systematic Study of the Thermal and Nonthermal Emission in the Supernova Remnant RCW 86 With Suzaku

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The temperature dependence of luminescence from a-Si: H/a-Si₃N₄: H superlattices