The X-Ray Expansion of the Supernova Remnant Cassiopeia A

Koralesky, Barron; Rudnick, Lawrence; Gotthelf, E. V.; Keohane, J. W.

doi:10.1086/311604

Cited by 44 publications

(44 citation statements)

References 23 publications

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“…These knot measurements confirmed that the X-ray Doppler expansion rate agrees with the X-ray proper motion rate, ∼ 0.2 % yr −1 on average (Koralesky et al 1998;Vink, et al 1998;DeLaney et al 2004). Perhaps somewhat surprisingly, the expansion rate of the FS is about the same as the X-ray ejecta (DeLaney & Rudnick 2003;Patnaude & Fesen 2009).…”

Section: Core-collapse X-ray Observationssupporting

confidence: 72%

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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Section: Core-collapse X-ray Observationssupporting

confidence: 72%

Kinematics of Supernova Remnants: Status of X-Ray Observations

Dewey¹

2010

High-Resolution X-Ray Spectroscopy

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“…This provides further insight into the well-known large-scale asymmetries in Cas A's expansion (Tuffs 1986;Reed et al 1995;Koralesky et al 1998). The reverse shock is found to be offset to the northwest by ∼0Ј .22 (∼15% of the ring radius) from the center of the forward shock.…”

Section: Cas A's Dynamical Statementioning

confidence: 57%

[ITAL]Chandra[/ITAL] Detection of the Forward and Reverse Shocks in Cassiopeia A

Gotthelf

Koralesky

Rudnick

et al. 2001

The Astrophysical Journal

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227

272

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We report the localization of the forward and reverse shock fronts in the young supernova remnant Cassiopeia A using X-ray data obtained with the Chandra X-Ray Observatory. High-resolution X-ray maps resolve a previously unseen X-ray feature encompassing the extremity of the remnant. This feature consists of thin, tangential wisps of emission bordering the outer edge of the thermal X-ray and radio remnant, forming a circular rim, ∼2Ј .7 in radius. Radio images show a sharp rise in brightness at this X-ray rim along with a large jump in the synchrotron polarization angle. These characteristics suggest that these wisps are the previously unresolved signature of the forward, or outer, shock. Similarly, we identify the sharp rise in emissivity of the bright shell for both the radio and X-ray line emission associated with the reverse shock. The derived ratio of the averaged forward and reverse shock radii of ∼3 : 2 constrains the remnant to have swept up roughly the same amount of mass as was ejected; this suggests that Cas A is just entering the Sedov phase. Comparison of the X-ray spectra from the two shock regions shows that the equivalent widths of prominent emission lines are significantly lower exterior to the bright shell, as expected if they are respectively identified with the shocked circumstellar material and shocked ejecta. Furthermore, the spectrum of the outer rim itself is dominated by power-law emission, likely the counterpart of the nonthermal component previously seen at energies above ∼10 keV.

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“…Our data are within two dashed lines. Other data shown as stars are responsible for the Cas A SNR at 350 yr (Koralesky et al, 1998;Vink et al, 1998), the Kepler's SNR at 400 yr (Katsuda et al, 2008;Vink, 2008), the Tycho's SNR at 430 (Hughes, 2000), SN1006 at 1000 yr (Moffett et al, 1993), and the Cygnus Loop at 10,000 yr (Blair et al, 2005). The solid line is the bestfit Power-law function representing the data points of five other SNRs.…”

Section: Discussionmentioning

confidence: 96%