Six Years of Chandra Observations of Supernova Remnants

Weisskopf, Martin C.; Hughes, John P.

doi:10.1007/3-540-30313-8_3

Cited by 15 publications

(11 citation statements)

References 189 publications

(250 reference statements)

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“…The telescope's superb spatial resolution has revealed newly processed metals in the interiors of most LMC SNRs and at least one new pulsar wind nebula (see Weisskopf & Hughes 2006 and reference therein). Studying the full sample of LMC SNRs is essential to gaining a more complete understanding of the evolution of metal-rich ejecta, from its synthesis in stars and SNe to its integration into the interstellar medium.…”

Section: Introductionmentioning

confidence: 98%

The Chandra View of the Supernova Remnant 0506-68.0 in the Large Magellanic Cloud

Hughes

Rafelski

Warren

et al. 2006

ApJ

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A new Chandra observation of SNR 0506Ϫ68.0 (also called N23) reveals a complex, highly structured morphology in the low-energy X-ray band and an isolated compact central object in the high-energy band. Spectral analysis indicates that the X-ray emission overall is dominated by thermal gas whose composition is consistent with swept-up ambient material. There is a strong gradient in ambient density across the diameter of the remnant. Toward the southeast, near a prominent star cluster, the emitting density is 10-23 cm Ϫ3 , while toward the northwest it has dropped to a value of only 1 cm Ϫ3 . The total extent of the X-ray remnant is ( pc for 100 # 120 24 # 29 a distance of 50 kpc), somewhat larger than previously known. The remnant's age is estimated to be ∼4600 yr.One part of the remnant shows evidence for enhanced O, Ne, and perhaps Mg abundances, which is interpreted as evidence for ejecta from a massive star core collapse supernova. The compact central object has a luminosity of a few times 10 33 ergs s Ϫ1 and no obvious radio or optical counterpart. It does not show an extended nebula or pulsed emission as expected from a young energetic pulsar, but resembles the compact central objects seen in other core collapse SNe, such as Cas A. Subject headings: ISM: individual (LHA 120-N 23, SNR 0506Ϫ68.0) -shock wavessupernova remnants -X-rays: individual (CXOU J050552.3Ϫ680141) -X-rays: ISM

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Section: Introductionmentioning

confidence: 98%

The Chandra View of the Supernova Remnant 0506-68.0 in the Large Magellanic Cloud

Hughes

Rafelski

Warren

et al. 2006

ApJ

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“…As computer processing power has advanced, astronomers have been able to include additional physics into their 3D models, such as precollapse perturbations (Couch & Ott 2013;Couch et al 2015;Müller & Janka 2015;Müller et al 2016Müller et al , 2017aMüller 2016), rotation (Kuroda et al 2014;Nakamura et al 2015;Takiwaki et al 2016;Summa et al 2018), Supernova remnants (SNRs) are a useful sample for comparison to simulation predictions. The heavy elements synthesized in the explosions as well as NSs are observable in young SNRs of ages 10 4 years (see reviews by Weisskopf &Vink 2012). As the ejecta expands into the interstellar medium (ISM), the reverse shock heats the ejecta to ∼ 10 7 K temperatures, producing X-rays that can be detected with modern X-ray facilities, such as the Chandra X-ray Observatory.…”

Section: Introductionmentioning

confidence: 99%

Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

Holland-Ashford

Lopez

Auchettl

2020

ApJ

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Supernova remnants (SNRs) offer the means to study supernovae (SNe) long after the original explosion and can provide a unique insight into the mechanism that governs these energetic events. In this work, we examine the X-ray morphologies of different elements from oxygen to iron found in the youngest known core-collapse (CC) SNR in the Milky Way, Cassiopeia A. The heaviest elements exhibit the highest levels of asymmetry, which we relate to the burning process that created the elements and their proximity to the center of explosion. Our findings support recent model predictions that the material closest to the source of explosion will reflect the asymmetries inherent to the SN mechanism. Additionally, we find that the heaviest elements are moving more directly opposed to the neutron star (NS) than the lighter elements. This result is consistent with NS kicks arising from ejecta asymmetries.

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“…The physical properties of these filaments were reviewed by Vink & Laming (2003), Vink (2004), Weisskopf & Hughes (2006), Ballet (2006), Parizot et al (2006), Bamba et al (2006), and Berezhko (2008). These filaments are believed to be produced by synchrotron radiation emitted by TeV electrons.…”

Section: Introductionmentioning

confidence: 99%

Postshock turbulence and diffusive shock acceleration in young supernova remnants

Marcowith¹,

Casse²

2010

A&A

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Context. Thin X-ray filaments are observed in the vicinity of young supernova remnants (SNR) blast waves. Identifying the process that creates these filaments would provide direct insight into the particle acceleration occurring within SNR and in particular the cosmic ray yield. Aims. We investigate magnetic amplification in the upstream medium of a SNR blast wave through both resonant and non-resonant regimes of the streaming instability. We attempt to understand more clearly of the diffusive shock acceleration (DSA) efficiency by considering various relaxation processes of the magnetic fluctuations in the downstream medium. Multiwavelength radiative signatures originating in the SNR shock wave are used to test various downstream turbulence relaxation models. Methods. Analytical and numerical calculations that couple stochastic differential equation schemes with 1D spherical magnetohydrodynamics simulations are used to investigate, in the context of test particles, turbulence evolution in both the forshock and post-shock regions. Stochastic second-order Fermi acceleration induced by resonant modes, magnetic field relaxation and amplification, and turbulence compression at the shock front are considered to model the multiwavelength filaments produced in SNRs. The γ-ray emission is also considered in terms of inverse Compton mechanism. Results. We confirm the result of Parizot and collaborators that the maximum CR energies should not go well beyond PeV energies in young SNRs where X-ray filaments are observed. To reproduce observational data, we derive an upper limit to the magnetic field amplitude and so ensure that stochastic particle reacceleration remains inefficient. Considering various magnetic relaxation processes, we then infer two necessary conditions to achieve efficient acceleration and X-ray filaments in SNRs: (1) the turbulence must fulfil the inequality 2 − β − δ d ≥ 0; where β is the turbulence spectral index and δ d is the relaxation length energy power-law index; (2) the typical relaxation length must be of the order the X-ray rim size. We find that Alvénic/fast magnetosonic mode damping fulfils all conditions; while non-linear Kolmogorov damping does not. By confronting previous relaxation processes with observational data, we deducte that among our SNR sample, data for the older ones (SN1006 and G347.3-0.5) does not comply with all conditions, which means that their X-ray filaments are probably controlled by radiative losses. The younger SNRs, Cassiopeia A, Tycho, and Kepler pass all tests and we infer that the downstream magnetic field amplitude is in the range of 200−300 μGauss.

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Six Years of Chandra Observations of Supernova Remnants

Cited by 15 publications

References 189 publications

The Chandra View of the Supernova Remnant 0506-68.0 in the Large Magellanic Cloud

The Chandra View of the Supernova Remnant 0506-68.0 in the Large Magellanic Cloud

Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

Postshock turbulence and diffusive shock acceleration in young supernova remnants

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