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Parallel sessions
Sessions
id
date time
2022-03-08 11:44:00
3D Hydrodynamics and Magnetohydrodynamics: Stars and their Environment
Stellar4
In the last two decades, realistic three-dimensional hydrodynamical simulations have become essential to understand modern observations of stars and their environment, ranging from Solar flares to spectral lines in cool stars, the imaging of circumstellar discs and transients resulting from stellar mergers. This session aims at discussing new results and current challenges related to 3D hydrodynamical simulations and sharing ideas between diverse research areas regarding their applications to observations, with a focus on the training of junior researchers. (i) Stellar astrophysics: The surface layers of cool stars, giants and white dwarfs are governed by convection, which requires an understanding of the complex interplay between compressible hydrodynamical flows, radiative cooling (RHD) and magnetic fields (MHD). Realistic numerical simulations of the atmospheres of convective stars are now within reach, but there is still extensive work needed to fully understand line formation, convective overshoot and interaction with pulsations. Hydrodynamical simulations of interiors stellar convection are also critical to understand stellar evolution, chemical mixing and nuclear burning rates. (ii) Exoplanet characterisation and atmospheres: Stellar atmospheric convection and magnetic activity can impact the interpretation of planet detections from radial velocities or transits, as well as the interpretation of exoplanet atmospheres observed via transmission and emission spectroscopy. In addition, hydrodynamics models of planet atmospheres can inform on global heat transport and circulation, chemistry, and infrared spectra. (iii) Solar physics: The generation of magnetic fields by a large-scale dynamo is linked to the significant activity of the Sun, including the emergence and disappearance of active regions, as well as flare events and mass ejections. High resolution spatial and time cadence MHD simulations are essential to understand the physical processes underlying the highly dynamical plasma and magnetic field evolution through the atmosphere, chromosphere and corona. (iv) Circumstellar disks: Hydrodynamical simulations are key to understand circumstellar discs ranging from protoplanetary discs to those that form from disrupted rocky planetesimals around old white dwarfs. Important questions including dust growth and fragmentation in self-gravitating discs, and the modelling of gap and ring features that are common in planet-forming discs. (v) Transients: With the discovery of the first gravitational wave events, there has been renewed interest in hydrodynamical simulations of stellar mergers including compact neutron stars and white dwarfs. Furthermore, 3D hydro simulations of core-collapse and type Ia supernovae have matured significantly in recent years, helping to understand a vast range of transients and their underlying stellar populations.
Tony Arber, Matteo Brogi, Heather Cegla, Elena Cukanovaite, Tim Cunningham, Viktor Fedun, Tom Goffrey, Raphael Hirschi, Joseph Lyman, Rebecca Nealon, Sahl Rowther, Pier-Emmanuel Tremblay
Thur. 09:00-10:30 / Thur. 14:30-16:00
09:00-09:05 Pier-Emmanuel Tremblay Welcome
09:06-09:17 Yurina Nakazato: The formation of gas-rich structure though baryon-dark matter streaming motion
09:18-09:30 Hila Glanz: Simulations of common envelope evolution in triple systems and their outcomes
09:36-09:48 Rebecca Nealon: Rocking shadows in protoplanetary discs
09:49-10:01 Dr Loren E Held: MRI dynamo in accretion discs at large magnetic Prandtl numbers
10:02-10:14 Sahl Rowther: Planet-Disc Interactions Versus Gravitational Instability
10:15-10:30 Discussion with Nealon, Held and Rowther.
14:30-14:42 Junho Park: Hydrodynamic instabilities and turbulence in radiation zone of rotating stars
14:43-14:55 Federico Rizzuti: Entrainment in 3D hydrodynamics simulations of neon burning
14:56-15:08 Adrien Morison: Hydrodynamics of convective cores of massive stars
15:09-15:21 Dimitar G Vlaykov: Convective non-locality — the impact on convective overshooting and internal gravity waves in global hydrodynamic simulations of solar type stars
15:22-15:34 Bannawit Pimpanuwat: ALMA observations and 3D modelling of mm-wavelength SiO masers towards oxygen-rich evolved stars
15:35-15:47 Daye Lim: Slow Magnetoacoustic Oscillations in Stellar Coronal Loops