IAU Symposium 365 was devoted to observational and theoretical aspects of solar and stellar hydrodynamics and magnetohydrodynamics. It brought together specialists in the physics of convection zones and atmospheres, to stimulate the emergence of new ideas and to develop new techniques in this dynamic field of active research.
Impressive events of magnetic energy release, such as solar and stellar flares and coronal mass ejections, take place in the atmospheric layers above a star's photosphere. These magnetic-activity events are closely related to the dynamics of subsurface convection zones inside the star. IAU Symposium 365 was devoted to observational and theoretical aspects of solar and stellar hydrodynamics and magnetohydrodynamics, both global and local, including numerical studies. The last few decades have been marked by substantial progress in our understanding of the physics of internal and external processes in the Sun and solar-type stars, but the scientific communities making this progress have not traditionally worked closely together. This symposium, delayed due to the COVID pandemic, brought together specialists in the physics of convection zones and atmospheres, to stimulate the emergence of new ideas and to develop new techniques in this dynamic field of active research.
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IAU S365 was devoted to observational and theoretical aspects of solar and stellar hydrodynamics and magnetohydrodynamics.
Section
1. Solar and Stellar Convection: Effects of rotation and surface
forcing on deep stellar convection zones P. J. Käpylä; Analyzing magnetic
network and its variations over Solar Cycles 23, 24 and 25 based on magnetic
power spectra Y. Luo, J. Jiang and R. Wang; Imaging stellar surface features
with optical interferometry X. Haubois; Section
2. Differential Rotation and
Meridional Circulation: Differential rotation of the solar chromosphere using
multidecadal Ca II K spectroheliograms D. K. Mishra et al.; A
frequency-dependent method for measuring the Sun's interior meridional
circulation R. Chen and J. Zhao; Probing the Sun's near surface shear layer
using HMI spherical harmonic coefficients S. C. Tripathy, K. Jain, S.
Kholikov and R. Komm; Rotational shear in the low photosphere of the Sun T.
Corbard, M. Faurobert et al.; Near-surface shear layer of solar rotation:
origin and significance L. Kitchatinov; The near-surface shear layer (NSSL)
of the Sun: a theoretical model A. R. Choudhuri and B. K. Jha; Differential
rotation of stars from spot transit mapping: dependence on rotation period
and effective temperature A. Araújo and A. Valio; Short and long term spot
evolution on EI Eri L. Kriskovics et al.; Magnetic activity under tidal
influences in the 2+2 hierarchical quadruple system V815 Herculis Zs. Kvári
et al.; Section
3. Global dynamo. Solar and Stellar Activity Cycles: Recent
developments in the BabcockLeighton solar dynamo theory B. B. Karak;
Nonlinear and stochastic mechanisms of the solar cycle and their implications
for the cycle prediction J. Jiang; A new generation of solar dynamo model and
its application to explore the stellar magnetic cycle Z. Zhang; Resonance and
stellar dynamos D. Sokoloff, E. Yushkov and A. Serenkova; The role of
nonlinear toroidal flux loss due to flux emergence in the long-term evolution
of the solar cycle A. Biswas; Dominating active regions in the minima of
solar activity R. A. Suleymanova and V. I. Abramenko; Solar cycle variability
induced by stochastic fluctuations of BMR properties and at different amounts
of dynamo supercriticality Pawan Kumar; Exploring the predictability of the
solar cycle from the polar field rise rate: Results from observations and
simulations A. Biswas; The NorthSouth asymmetry of the number and magnetic
fluxes of active regions of different magneto-morphological types in cycles
23 and 24 A. Zhukova; Prognostic opportunity of the shifted correlation
Between Wolf numbers and their time derivatives S. V. Starchenko and S. V.
Yakovleva; Chromosphere activity: relations with solar cycles S. Koutchmy and
E. Tavabi; Modelling the rotation dependence of cycle variability in sun-like
stars: Answering why only slowly rotating stars produce grand minima V.
Vashishth; On origin of active/inactive branches on moderate rotating solar
analogs V. V. Pipin; Section
4. Helioseismology and Asteroseismology: Recent
progress in timedistance helioseismology: meridional circulation, far-side
imaging, and sunquakes R. Chen and J. Zhao; Convection, rotation, and
magnetic activity of solar-like stars from asteroseismology S. Mathur; Solar
inertial modes L. Gizon et al.; A 2D model for the excitation of the linearly
stable inertial modes of the Sun by turbulent convection J. Philidet and L.
Gizon; Temporal variation of solar equatorial Rossby modes with azimuthal
orders 6 <= m <= 10 B. Lekshmi et al.; Observational study of Reynolds
stresses associated with solar inertial modes Y. Mandowara et al.; Probing
the superadiabaticity of the solar convection zone with inertial modes P. Dey
et al.; Effects of small-scale magnetic fields in the photosphere on surface
effects for solar-like stars G. Lin, Y. Li, T. Wu and S. Jie; The effect of
Coulomb interactions on acoustic oscillations in the outer layers of low-mass
stars A. Brito and I. Lopes; Section
5. Local Processes of Ma
