MC
Member Since 1998
Marco C M Velli
Professor, University of California Los Angeles
AGU Research
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The Evolution of the 1/f Range Within a Single Fast-Solar-Wind Stream Between 17.4 and 45.7 Solar Radii
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE IV POSTER
spa-solar and heliospheric physics | 15 december 2023
Nooshin Davis, Benjamin D. Chandran, Trevor Bowen...
MHD turbulence accounts for many of the temporal and spatial variations in the fluid variables observed in the solar wind and other plasmas. The turbu...
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Evolution of MHD turbulence in the expanding solar wind: residual energy and intermittency
MAGNETIC STRUCTURES AND WAVES IN SOLAR WIND TURBULENCE II ORAL
spa-solar and heliospheric physics | 15 december 2023
Chen Shi, Nikos Sioulas, Zesen Huang, Marco C. Vel...
We conduct 3D MHD simulations of decaying turbulence in the solar wind context. To account for the spherical expansion of the solar wind, we implement...
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Investigating the Structure and Dynamics of the Heliospheric Current Sheet
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE IV POSTER
spa-solar and heliospheric physics | 15 december 2023
Lizet Casillas, Marco C. Velli
The heliospheric current sheet (HCS) is the boundary between open magnetic field lines of opposite polarity in the solar wind that are also rooted in ...
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Natural Contextualization of Solar Wind Time Series with Jensen-Shannon Scalogram
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE III POSTER
spa-solar and heliospheric physics | 14 december 2023
Zesen Huang, Chen Shi, Marco C. Velli, Nikos Sioul...
Contextualization of the in situ solar wind time series is crucial for understanding the structure and dynamics of the sun's coronal magnetic field. I...
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A Predictive and Validated Theory for the Formation of Magnetic SwitchbacksObserved by Parker Solar Probe
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE III POSTER
spa-solar and heliospheric physics | 14 december 2023
Gabor Toth, Marco C. Velli, Bart van der Holst
Magnetic switchbacks are rapid high amplitude reversals of the radialmagnetic field in the solar wind that do not involve a heliosphericcurrent sheet ...
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Sources of Slow Solar Wind Streams
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE III POSTER
spa-solar and heliospheric physics | 14 december 2023
Marco C. Velli, Olga Panasenco, Victor Réville, Co...
Solar wind streams are characterized by different plasma properties, from overall speed, to temperature and temperature anisotropies, composition, as ...
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Looking Through Solar Coronal Holes
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE III POSTER
spa-solar and heliospheric physics | 14 december 2023
Olga Panasenco, Marco C. Velli, Shadia R. Habbal
The solar dynamo and plasma convection produce three main observed structures extending from the solar surface into the corona: active regions, solar ...
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Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
FUNDAMENTAL PHYSICS OF THE SOLAR CORONA AND INNER HELIOSPHERE III POSTER
spa-solar and heliospheric physics | 14 december 2023
Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi...
In this work we report observations of magnetic switchback (SB) features near 1 au using data from the Wind spacecraft. These features appear to be st...
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