Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
@doi [ ] 10.1093/mnras/stac1808, https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.4229P 515
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Diffusive spreading of dynamo fields into turbulent exteriors reverses the usual decay ordering, allowing quadrupole toroidal components to decay slower than dipoles and confining fields within a magnetosphere whose synchrotron signatures are potentially observable.
Fornax cluster magnetic field follows a power-law spectrum of slope ~2.7 with central strength ~5 μG scaling as n^1.6, consistent with recent central re-amplification and trends across 17 clusters.
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.
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Revisiting radio synchrotron diagnostics in star-forming galaxies
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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Magnetic field spreading from stellar and galactic dynamos into the exterior
Diffusive spreading of dynamo fields into turbulent exteriors reverses the usual decay ordering, allowing quadrupole toroidal components to decay slower than dipoles and confining fields within a magnetosphere whose synchrotron signatures are potentially observable.
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The MeerKAT Fornax Survey VII. Characterisation of the Fornax cluster's magnetic field and new insights on magnetisation in large scale systems
Fornax cluster magnetic field follows a power-law spectrum of slope ~2.7 with central strength ~5 μG scaling as n^1.6, consistent with recent central re-amplification and trends across 17 clusters.
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Steady-State or Not? The Evolution of Cosmic Ray Electron Spectra in Galaxies
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.