The Youngest Galactic Supernova Remnant: G1.9+0.3

Reynolds, Stephen P.; Borkowski, Kazimierz J.; Green, David A.; Hwang, U.; Harrus, I.; Petre, Robert

doi:10.1086/589570

Cited by 176 publications

(221 citation statements)

References 24 publications

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“…Thus, the magnetic energy increase and the X-ray variability might have a time-scale (1 yr) much lower than the SNR hydrodynamic time-scale and might occur in middle-aged SNRs, not necessarily young SNRs (RXJ1713.7 − 3946 age is estimated as 1, 600 yr (Stephenson & Green 2002)). The high shock speed C r ∼ 15, 000 km/s in Fig.2 is comparable to observations of the youngest SNR in our galaxy, i.e., 100 years old G1.9 + 0.3 (Reynolds et al 2008). Thus, a rapid field saturation even up to B ∼ 10 mG is predicted at SNR shocks within a few months.…”

Section: Field Growthsupporting

confidence: 87%

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Fraschetti

2013

ApJ

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We derive analytically the vorticity generated downstream of a two-dimensional rippled hydromagnetic shock neglecting fluid viscosity and resistivity. The growth of the turbulent component of the downstream magnetic field is driven by the vortical eddies motion. We determine an analytic time-evolution of the magnetic field amplification at shocks, so far described only numerically, until saturation occurs due to seed-field reaction to field lines whirling. The explicit expression of the amplification growth rate and of the non-linear field back-reaction in terms of the parameters of shock and interstellar density fluctuations is derived from MHD jump conditions at rippled shocks. A magnetic field saturation up to the order of milligauss and a short-time variability in the X-ray observations of supernova remnants can be obtained by using reasonable parameters for the interstellar turbulence.

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Section: Field Growthsupporting

confidence: 87%

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Fraschetti

2013

ApJ

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“…The diameter increased by 16 % ±3% in 22 years between radio (1985) and X-ray (2007) measurements, as confirmed by recent radio and X-ray reobservations (Reynolds et al 2008a;Borkowski et al 2010). Using an SNR diameter expansion from 84 to 97.5 arc seconds gives the FS velocity shown in Table 1 Kepler (SN 1604, G4.5+6.8) Hughes (1999) used Einstein and ROSAT data to measure an average expansion rate of the Kepler X-ray images of 0.239 % yr −1 , giving an expansion parameter value of m ≈ 0.93 with an error of order ±0.10.…”

Section: G19+03supporting

confidence: 52%

Kinematics of Supernova Remnants: Status of X-Ray Observations

Dewey¹

2010

High-Resolution X-Ray Spectroscopy

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A supernova (SN) explosion drives stellar debris into the circumstellar material (CSM) filling a region on a scale of parsecs with X-ray emitting plasma. The velocities involved in supernova remnants (SNRs), thousands of km s −1 , can be directly measured with medium and high-resolution X-ray spectrometers and add an important dimension to our understanding of the last stages of the progenitor, the explosion mechanism, and the physics of strong shocks. After touching on the ingredients of SNR kinematics, I present a summary of the still-growing measurement results from SNR X-ray observations. Given the advances in 2D/3D hydrodynamics, data analysis techniques, and especially X-ray instrumentation, it is clear that our view of SNRs will continue to deepen in the decades ahead.Keywords supernova remnants · supernovae · X-ray spectroscopy · X-ray instrumentation

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“…Cassiopeia A (Cas A) is the second youngest known supernova remnant (SNR) in our galaxy, with only the recently discovered G1.9+0.3 being younger (Reynolds et al 2008). Extensive observations in the radio, infrared, optical, and X-ray give an estimated explosion date of around 1680 AD (Thorstensen et al 2001;Fesen et al 2006).…”

Section: Introductionmentioning

confidence: 99%

The Three-Dimensional Structure of Interior Ejecta in Cassiopeia a at High Spectral Resolution

Isensee

Rudnick

DeLaney

et al. 2010

ApJ

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We used the Spitzer Space Telescope's Infrared Spectrograph to create a high-resolution spectral map of the central region of the Cassiopeia A (Cas A) supernova remnant, allowing us to make a Doppler reconstruction of its threedimensional structure. The ejecta responsible for this emission have not yet encountered the remnant's reverse shock or the circumstellar medium, making it an ideal laboratory for exploring the dynamics of the supernova explosion itself. We observe that the O, Si, and S ejecta can form both sheet-like structures and filaments. Si and O, which come from different nucleosynthetic layers of the star, are observed to be coincident in velocity space in some regions, and separated by 500 km s −1 or more in others. Ejecta traveling toward us are, on average, ∼900 km s −1 slower than the material traveling away from us. We compare our observations to recent supernova explosion models and find that no single model can simultaneously reproduce all the observed features. However, models of different supernova explosions can collectively produce the observed geometries and structures of the interior emission. We use the results from the models to address the conditions during the supernova explosion, concentrating on asymmetries in the shock structure. We also predict that the back surface of Cas A will begin brightening in ∼30 years, and the front surface in ∼100 years.

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The Youngest Galactic Supernova Remnant: G1.9+0.3

Cited by 176 publications

References 24 publications

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Kinematics of Supernova Remnants: Status of X-Ray Observations

The Three-Dimensional Structure of Interior Ejecta in Cassiopeia a at High Spectral Resolution

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