activity
20052023
most citedPLUTO: a Numerical Code for Computational Astrophysics

1.6k citations · 5k across the 73 of their papers we have counts for

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Showing astro-ph.SRShow all

10 papers · 1 filter

astro-ph.SR2021★ 9 cited

Acceleration of Solar Energetic Particles by the shock of Interplanetary Coronal Mass Ejection

Shanwlee Sow Mondal, Aveek Sarkar, Bhargav Vaidya +1

Interplanetary Coronal Mass Ejection (ICME) shocks are known to accelerate particles and contribute significantly to Solar Energetic Particle (SEP) events. We have performed Magnet…

astro-ph.SR2021★ 30 cited

3D MHD astrospheres: applications to IRC-10414 and Betelgeuse

D. M. -A. Meyer, A. Mignone, M. Petrov +3

A significative fraction of all massive stars in the Milky Way move supersonically through their local interstellar medium (ISM), producing bow shock nebulae by wind-ISM interactio…

astro-ph.SR2021★ 1 cited

SWELTO -- Space WEather Laboratory in Turin Observatory

A. Bemporad, L. Abbo, D. Barghini +20

SWELTO -- Space WEather Laboratory in Turin Observatory is a conceptual framework where new ideas for the analysis of space-based and ground-based data are developed and tested. Th…

astro-ph.SR2020★ 30 cited

Laboratory disruption of scaled astrophysical outflows by a misaligned magnetic field

G. Revet, B. Khiar, E. Filippov +20

The shaping of astrophysical outflows into bright, dense and collimated jets due to magnetic pressure is here investigated using laboratory experiments. We notably look at the impa…

astro-ph.SR2017★ 12 cited

Numerical Simulations of Torsional Alfvén Waves in Axisymmetric Solar Magnetic Flux Tubes

D. Wójcik, K. Murawski, Z. E. Musielak +2

We investigate numerically Alfvén waves propagating along an axisymmetric and non-isothermal solar flux tube embedded in the solar atmosphere. The tube magnetic field is current-fr…

astro-ph.SR2016★ 49 cited

3D MHD modeling of twisted coronal loops

F. Reale, S. Orlando, M. Guarrasi +4

We perform MHD modeling of a single bright coronal loop to include the interaction with a non-uniform magnetic field. The field is stressed by random footpoint rotation in the cent…