Research Highlights

Sarah E. Gibson, et al. provide an expansive mosaic of observations spanning from the Sun, through interplanetary space, to the magnetospheric response and subsequent effects on the ionosphere-thermosphere-mesosphere (ITM) system. To accomplish this, a diverse set of observational datasets are utilized and focused on two long-lived coronal holes and their varying impact in sculpting the heliosphere and driving of the magnetospheric system.

Feng Chen, Mark C.M. Cheung, Matthias Rempel, and Georgios Chintzoglou present a method of conducting data-driven simulations of solar active regions and flux emergence with the MURaM radiative magnetohydrodynamics (MHD) code. This method helps to understand the evolution of magnetic field in a more realistic coronal environment and to link the magnetic structures to observable diagnostics.

Matthias Rempel, Tanayveer Bhatia, Luis Bellot Rubio, and Maarit J. Korpi-Lagg review small-scale dynamo processes that are responsible for magnetic field generation on scales comparable to and smaller than the energy carrying scales of turbulence. We provide a review of critical observation of quiet Sun magnetism, which have provided strong support for the operation of a small-scale dynamo in the solar photosphere and convection zone.

Feng Chen, Matthias Rempel, and Yuhong Fan present a radiative magnetohydrodynamic simulation that includes sufficiently realistic physics to allow for the synthesis of remote sensing observables that can be quantitatively compared with observations. The model helps to shed light on questions of where and when the a flux rope may form and how the magnetic structures in an eruption are related to observable emission properties.

Sarah E. Gibson, et. al. discuss the Whole Heliosphere and Planetary Interactions (WHPI,) an international initiative to study the most recent solar minimum and its impact on the interconnected solar-heliospheric-planetary system by facilitating and encouraging interdisciplinary activities, placing it into the context of prior initiatives and describing the overall evolution of the system between 2018–2020.

Astrid Maute, Jeffrey Forbes, Chihoko Cullens, and Thomas Immel use the thermosphere-ionosphere-electrodynamics general circulation model (TIEGCM) driven by observationally fitted tides via the Hough Mode Extension (HME) method to isolate the effect of the changing upward propagating tides on the dynamics, composition, and plasma distribution .

Sarah E. Gibson et. al. emphasize the need of understanding and predicting the major phenomena taking place in the solar corona, such as flares and Coronal Mass Ejections (CMEs), the heating and evolution of the solar atmosphere, and the acceleration of the solar wind, are fundamental challenges to predict our own star. These challenges are related to the solar magnetism and to the physical properties of solar plasma.

J. Sreelakshmi, Astrid Maute, Geeta Vichare, Arthur Richmond, Brian Harding, and Patrick Alken demonstate with modeling studies that the altitudinal gradient of the zonal wind is related to the strength of the dip currents. However, observational studies to validate these results have been missing to this date.

H.-L. Liu, W. Wang, J. D. Huba, P. H. Lauritzen, and F. Vitt analyze the Hunga Tonga-Hunga Ha'apai Volcano waves that have been recorded by ground and satellite instrumentation. This event provides a rare opportunity to study the strong and direct connection of the whole atmosphere system. The high-resolution Whole Atmosphere Community Climate Model with thermosphere/ionosphere extension (WACCM-X) can simulate the global propagation of the waves, and the model results compare favorably with observations from the surface to the thermosphere and ionosphere.