Turbulence and Energetic Particles in Radiative Shock Waves in the Cygnus Loop. II. Development of Postshock Turbulence

Radiative shock waves in the Cygnus Loop and other supernova remnants show different morphologies in [O iii] and H emission. We use HST spectra and narrowband images to study the development of turbulence in the cooling region behind a shock on the west limb of the Cygnus Loop. We refine our earlier...

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Bibliographic Details
Published in:The Astrophysical journal 2020-11, Vol.903 (1), p.2
Main Authors: Raymond, John C., Slavin, Jonathan D., Blair, William P., Chilingarian, Igor V., Burkhart, Blakesley, Sankrit, Ravi
Format: Article
Language:English
Subjects:
Astrophysics
Emission analysis
Emission lines
Emission spectra
Energetic particles
Field strength
H alpha line
Hough transformation
Interplanetary turbulence
Interstellar magnetic fields
Magnetic fields
Morphology
Narrowband
Parameter estimation
Plasma astrophysics
Power spectra
Ram pressure
Shell stability
Shock waves
Shocks
Stability analysis
Supernova
Supernova remnants
Thermal instability
Thin walled shells
Turbulence
Upstream
Vorticity
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Summary:Radiative shock waves in the Cygnus Loop and other supernova remnants show different morphologies in [O iii] and H emission. We use HST spectra and narrowband images to study the development of turbulence in the cooling region behind a shock on the west limb of the Cygnus Loop. We refine our earlier estimates of shock parameters that were based upon ground-based spectra, including ram pressure, vorticity, and magnetic field strength. We apply several techniques, including Fourier power spectra and the Rolling Hough Transform, to quantify the shape of the rippled shock front as viewed in different emission lines. We assess the relative importance of thermal instabilities, the thin shell instability, upstream density variations, and upstream magnetic field variations in producing the observed structure.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abb821