Suzaku observation of the Galactic supernova remnant CTB 37A (G348.5+0.1)

Sezer, Aytap; Gök, Fatma; Hüdaverdi, Murat; Ercan, E. N.

doi:10.1111/j.1365-2966.2011.19357.x

Cited by 19 publications

(29 citation statements)

References 37 publications

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“…The age of the SNR shell is estimated around 1300 yr , which is consistent with the age between 750 and 2100 yr estimated by Kumar et al (2014). Kes 73 has been also observed by ROSAT (Helfand et al 1994), ASCA , Chandra (Lopez et al 2011) and Suzaku (Sezer et al 2010).…”

Section: Kes 73supporting

confidence: 86%

Comparing supernova remnants around strongly magnetized and canonical pulsars

Martín

Rea

Torres³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The origin of the strong magnetic fields measured in magnetars is one of the main uncertainties in the neutron star field. On the other hand, the recent discovery of a large number of such strongly magnetized neutron stars, is calling for more investigation on their formation. The first proposed model for the formation of such strong magnetic fields in magnetars was through alpha-dynamo effects on the rapidly rotating core of a massive star. Other scenarios involve highly magnetic massive progenitors that conserve their strong magnetic moment into the core after the explosion, or a common envelope phase of a massive binary system. In this work, we do a complete re-analysis of the archival X-ray emission of the Supernova Remnants (SNR) surrounding magnetars, and compare our results with all other bright X-ray emitting SNRs, which are associated with Compact Central Objects (CCOs; which are proposed to have magnetar-like B-fields buried in the crust by strong accretion soon after their formation), high-B pulsars and normal pulsars. We find that emission lines in SNRs hosting highly magnetic neutron stars do not differ significantly in elements or ionization state from those observed in other SNRs, neither averaging on the whole remnants, nor studying different parts of their total spatial extent. Furthermore, we find no significant evidence that the total X-ray luminosities of SNRs hosting magnetars, are on average larger than that of typical young X-ray SNRs. Although biased by a small number of objects, we found that for a similar age, there is the same percentage of magnetars showing a detectable SNR than for the normal pulsar population.

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Section: Kes 73supporting

confidence: 86%

Comparing supernova remnants around strongly magnetized and canonical pulsars

Martín

Rea

Torres³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Using Chandra and XMM-Newton observations, Aharonian et al (2008a) found diffusive thermal X-ray emission from the east part of the remnant and derived a flux upper limit of -3.5 10 13 erg cm −2 s −1 for nonthermal emission in the 1-10 keV range. Sezer et al (2011) suggested that the diffuse thermal X-ray emission of CTB 37A is produced by shocked interstellar/circumstellar medium and estimated an ambient gas density of~-f 1 1 2 cm −3 and an age of~´f 3 10 4 1 2 years, where f is the volume filling factor of the emitting plasma. Assuming a distance of 11.3 kpc, Pannuti et al (2014) obtained similar results with an electron density n e =0.77 cm −3 and an age of3.2 4.2 10 4 ( -) years by analyzing the X-ray spectrum.…”

Section: Ctb 37amentioning

confidence: 99%

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

Zeng

Xin

Liu

et al. 2017

ApJ

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Multi-wavelength observations of mature supernova remnants (SNRs), especially with recent advances in γ-ray astronomy, make it possible to constrain energy distribution of energetic particles within these remnants. In consideration of the SNR origin of Galactic cosmic rays and physics related to particle acceleration and radiative processes, we use a simple one-zone model to fit the nonthermal emission spectra of three shell-type SNRs located within 2°on the sky: RX J1713.7−3946, CTB 37B, and CTB 37A. Although radio images of these three sources all show a shell (or half-shell) structure, their radio, X-ray, and γ-ray spectra are quite different, offering an ideal case to explore evolution of energetic particle distribution in SNRs. Our spectral fitting shows that (1) the particle distribution becomes harder with aging of these SNRs, implying a continuous acceleration process, and the particle distributions of CTB 37A and CTB 37B in the GeV range are harder than the hardest distribution that can be produced at a shock via the linear diffusive shock particle acceleration process, so spatial transport may play a role; (2) the energy loss timescale of electrons at the high-energy cutoff due to synchrotron radiation appears to be always a bit (within a factor of a few) shorter than the age of the corresponding remnant, which also requires continuous particle acceleration; (3) double power-law distributions are needed to fit the spectra of CTB 37B and CTB 37A, which may be attributed to shock interaction with molecular clouds.

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“… References. (1) Paper I; (2) Velázquez et al (2002); (3) Green (2009); (4) Tian et al (2007); (5) Abdo et al (2010a); (6) Seta et al (1998); (7) Brogan & Troland (2001); (8) Koo et al (2005); (9) Koo & Moon (1997a); (10) Green (1990); (11) Blair, Sankrit & Raymond (2005); (12) Miyata et al (1994); (13) Sezer et al (2011); (14) Reynoso & Mangum (2000); (15) Slane et al (2002). …”

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

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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.

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Suzaku observation of the Galactic supernova remnant CTB 37A (G348.5+0.1)

Cited by 19 publications

References 37 publications

Comparing supernova remnants around strongly magnetized and canonical pulsars

Comparing supernova remnants around strongly magnetized and canonical pulsars

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

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

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