6533b873fe1ef96bd12d5841
RESEARCH PRODUCT
Magnetic shuffling of coronal downdrafts
Salvatore OrlandoA. PetraliaA. PetraliaFabio RealeFabio Realesubject
010504 meteorology & atmospheric sciencesField lineAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesAstrophysicsSun:corona01 natural sciencesAlfvén waveSettore FIS/05 - Astronomia E AstrofisicaPhysics::Plasma Physics0103 physical sciencesAstrophysics::Solar and Stellar Astrophysics010303 astronomy & astrophysicsSolar and Stellar Astrophysics (astro-ph.SR)0105 earth and related environmental sciencesPhysicsSolar flareAstronomy and AstrophysicsSun:activityPlasmaMagnetic fluxAccretion (astrophysics)Magnetic fieldAstrophysics - Solar and Stellar AstrophysicsSpace and Planetary SciencePhysics::Space PhysicsMagnetohydrodynamicsmagnetohydrodynamicsdescription
Channelled fragmented downflows are ubiquitous in magnetized atmospheres, and have been recently addressed from an observation after a solar eruption. We study the possible back-effect of the magnetic field on the propagation of confined flows. We compare two 3D MHD simulations of dense supersonic plasma blobs downfalling along a coronal magnetic flux tube. In one, the blobs move strictly along the field lines; in the other, the initial velocity of the blobs is not perfectly aligned to the magnetic field and the field is weaker. The aligned blobs remain compact while flowing along the tube, with the generated shocks. The misaligned blobs are disrupted and merged by the chaotic shuffling of the field lines, and structured into thinner filaments; Alfven wave fronts are generated together with shocks ahead of the dense moving front. Downflowing plasma fragments can be chaotically and efficiently mixed if their motion is misaligned to field lines, with broad implications, e.g., disk accretion in protostars, coronal eruptions and rain.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2017-01-20 |