MHD Turbulence as a Foreground for CMB Studies
arXiv:astro-ph/0205284 · doi:10.1086/342722
Abstract
Measurements of intensity and polarization of diffuse Galactic synchrotron emission as well as starlight polarization reveal power law spectra of fluctuations. We show that these fluctuations can arise from magnetohydrodynamic (MHD) turbulence in the Galactic disk and halo. To do so we take into account the converging geometry of lines of sight for the observations when the observer is within the turbulent volume. Assuming that the intensity of turbulence changes along the line of sight, we get a reasonable fit to the observed synchrotron data. As for the spectra of polarized starlight we get a good fit to the observations taking into account the fact that the observational sample is biased toward nearby stars.
10 pages, 6 figures, Astrophyscal J., submitted
References in corpus (9)
- Simulations of MHD Turbulence in a Strongly Magnetized Medium
- Compressible Sub-Alfvenic MHD turbulence in Low-beta Plasmas
- Compressible MHD Turbulence in Interstellar Plasmas
- Velocity and density spectra of the Small Magellanic Cloud
- Statistical Properties of Galactic Starlight Polarization
- Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: a re-analysis of the Parkes data
- The angular power spectrum of radio emission at 2.3 GHz
- The power-law behaviours of angular spectra of polarized Galactic synchrotron
- Polarized Microwave Emission from Dust
Cited by in corpus (32)
- Interstellar Turbulence I: Observations and Processes
- Compressible Magnetohydrodynamic Turbulence: mode coupling, scaling relations, anisotropy, new regime and astrophysical implications
- Tracing Magnetic Fields with Aligned Grains
- Compressible Turbulence in Galaxy Clusters: Physics and Stochastic Particle Re-acceleration
- Fundamental Physics with the Square Kilometre Array
- Planck 2018 results. XI. Polarized dust foregrounds
- Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio halos to gamma rays
- Velocity Modification of Power Spectrum from Absorbing Medium
- Magnetic Fields via Polarimetry: Progress of Grain Alignment Theory
- Obtaining Spectra of Turbulent Velocity from Observations
- Studying Galactic interstellar turbulence through fluctuations in synchrotron emission: First LOFAR Galactic foreground detection
- Characteristic Lengths of Magnetic Field in Magnetohydrodynamic Turbulence
- Diffusion of cosmic rays in MHD turbulence with magnetic mirrors
- Plasma turbulence in the interstellar medium
- The impact of Galactic synchrotron emission on CMB anisotropy measurements. I. Angular power spectrum analysis of total intensity all-sky surveys
- Deflections of cosmic rays in a random component of the Galactic magnetic field
- Modelling and simulation of large-scale polarized dust emission over the southern Galactic cap using the GASS HI data
- The Multi-phase Turbulence Density Power Spectra in the Perseus Molecular Cloud
- Loops and spurs: The angular power spectrum of the Galactic synchrotron background
- Polarimetric studies of magnetic turbulence with interferometer
- Supernova-regulated ISM -- V. Space- and time-correlations
- Galactic foregrounds: Spatial fluctuations and a procedure of removal
- Microwave Emission from Aligned Dust
- Magnetohydrodynamic turbulence in supernova remnants
- A Technique for Foreground Subtraction in Redshifted 21 cm Observations
- Radio polarimetry signatures of strong magnetic turbulence in Supernova Remnants
- Diffusion of large-scale magnetic fields by reconnection in MHD turbulence
- Turbulent power distribution in the local interstellar medium
- Basic Properties of Compressible MHD Turbulence: Implications for Molecular Clouds
- Angular Spectra of Polarized Galactic Foregrounds
- Galactic turbulence and paleoclimate variability
- B-mode polarization forecasts for GreenPol