Simulations show high-speed solar wind streams evolve via interactions and 3D flows, making them non-parcel-preserving and location-dependent in their observed properties.
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The iτSBD magnetic braking model attributes the boost K to irradiation-driven winds and the disruption η to a spike in convective turnover time at the fully convective boundary, yielding CV tracks consistent with observations.
citing papers explorer
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MHD simulations on the large-scale propagation of high-speed solar wind streams
Simulations show high-speed solar wind streams evolve via interactions and 3D flows, making them non-parcel-preserving and location-dependent in their observed properties.
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Mechanisms for magnetic braking boost and disruption: the role of irradiation-driven winds and convective turnover time spike in cataclysmic variables
The iτSBD magnetic braking model attributes the boost K to irradiation-driven winds and the disruption η to a spike in convective turnover time at the fully convective boundary, yielding CV tracks consistent with observations.