Search results for "Sun:corona"

showing 3 items of 3 documents

MHD modelling of plasma flowing in coronal magnetic channels

accretion accretion shockscorona [Sun]Sun:coronamagnetohydrodynamics (MHD)
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Connecting Solar Orbiter remote-sensing observations and Parker Solar Probe in situ measurements with a numerical MHD reconstruction of the Parker sp…

2022

As a key feature, NASA's Parker Solar Probe (PSP) and ESA-NASA's Solar Orbiter (SO) missions cooperate to trace solar wind and transients from their sources on the Sun to the inner interplanetary space. The goal of this work is to accurately reconstruct the interplanetary Parker spiral and the connection between coronal features observed remotely by the Metis coronagraph on-board SO and those detected in situ by PSP at the time of the first PSP-SO quadrature of January 2021. We use the Reverse In-situ and MHD Approach (RIMAP), a hybrid analytical-numerical method performing data-driven reconstructions of the Parker spiral. RIMAP solves the MHD equations on the equatorial plane with the PLUT…

Plasma Physics (physics.plasm-ph)Settore FIS/05 - Astronomia E AstrofisicaAstrophysics - Solar and Stellar AstrophysicsPhysics - Space PhysicsSpace and Planetary ScienceFOS: Physical sciencesAstronomy and Astrophysicsmagnetohydrodynamics (MHD) – methods: numerical – solar wind – Sun: heliosphere – Sun: coronamagnetohydrodynamics(MHD)methods:numericalsolar windSun:heliosphereSun:coronaPhysics - Plasma PhysicsSolar and Stellar Astrophysics (astro-ph.SR)Space Physics (physics.space-ph)
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Magnetic shuffling of coronal downdrafts

2017

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 …

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 PhysicsMagnetohydrodynamicsmagnetohydrodynamics
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