Turbulence and Particle Acceleration in Radiative Shock Waves in the Cygnus Loop II: Development of Postshock Turbulence

Abstract

Radiative shock waves in the Cygnus Loop and other supernova remnants show different morphologies in [O III] and Hα 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.

arXiv comment40 pages, 22 Figures. Accepted for publication in ApJ

References in corpus (25)

• Simulations of Ion Acceleration at Non-relativistic Shocks. I. Acceleration Efficiency
• CHIANTI - An atomic database for Emission Lines. Version 8
• A Unified Model for Galactic Discs: Star Formation, Turbulence Driving, and Mass Transport
• Magnetically Aligned HI Fibers and the Rolling Hough Transform
• Is Turbulence in the Interstellar Medium Driven by Feedback or Gravity? An Observational Test
• Characterizing Magnetohydrodynamic Turbulence in the Small Magellanic Cloud
• Destruction of Interstellar Dust in Evolving Supernova Remnant Shock Waves
• The Star Formation Rate in the Gravoturbulent Interstellar Medium
• Binospec: A Wide-field Imaging Spectrograph for the MMT
• On the Amplification of Magnetic Field by a Supernova Blast Shock Wave in a Turbulent Medium
• The Distance to the Cygnus Loop from Hubble Space Telescope Imaging of the Primary Shock Front
• The Turbulence Velocity Power Spectrum of Neutral Hydrogen in the Small Magellanic Cloud
• Turbulent amplification of magnetic field driven by dynamo effect at rippled shocks
• Far Ultraviolet Spectra of a Non-Radiative Shock Wave in the Cygnus Loop
• The Cygnus Loop's Distance, Properties, and Environment Driven Morphology
• Shock Speed, Cosmic Ray Pressure, and Gas Temperature in the Cygnus Loop
• The Multi-phase Turbulence Density Power Spectra in the Perseus Molecular Cloud
• An Isolated, Recently Shocked ISM Cloud in the Cygnus Loop SNR
• Trapping of cosmic rays in MHD turbulence
• A cosmic-ray precursor model for a Balmer-dominated shock in Tycho's supernova remnant
• Turbulence and Energetic Particles in Radiative Shock Waves in the Cygnus Loop I: Shock Properties
• HST-STIS Observations of the Cygnus Loop: Spatial Structure of a Non-radiative Shock
• Localized enhancements of energetic particles at oblique collisionless shocks
• Fast Particle Acceleration at Perpendicular Shocks with Uniform Upstream Magnetic Field and Strong Downstream Turbulence
• Particle acceleration in a shock wave propagating to an inhomogeneous medium

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• Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures
• The Origin of the Cluster of Local Interstellar Clouds
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• Shocks in the warm neutral medium I -- Theoretical model
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• On the Determination of the Evolutionary Status of Supernova Remnants from Radio Observation Data