Name: Stellar Convection: Modelling, Theory and Observations
Start: 2024-08-26T09:00:00+02:00
End: 2024-09-20T18:00:00+02:00
Location: Albano Building 3

Monday, 26 August 2024

09:00 Registration
Registration
09:00 - 11:00

11:00 Laurent Gizon: Probing the solar convection zone with inertial modes
Laurent Gizon: Probing the solar convection zone with inertial modes
11:00 - 11:45
The Sun supports a rich spectrum of global modes of oscillation in the inertial frequency range. Many of these modes can be identified by comparing their observed frequencies and horizontal velocity eigenfunctions at the surface to the linear eigenmodes of a set of adjustable rotating solar models. This provides sensitive diagnostics of the differential rotation and properties of the deep solar convection zone which are currently poorly constrained. These properties include the superadiabatic temperature gradient, the latitudinal entropy gradient, and the turbulent viscosity. In addition, nonlinear simulations indicate that the high-latitude inertial modes play a dynamical role and place a limit on the maximum allowed latitudinal differential rotation

11:45 Suprabha Mukhopadhyay: Numerical studies of inertial modes in the Sun using Dedalus
Suprabha Mukhopadhyay: Numerical studies of inertial modes in the Sun using Dedalus
11:45 - 12:10
The Sun undergoes various oscillations through which we can probe deep into its convective interior. Inertial modes are low-frequency oscillations restored by the Coriolis force and have recently been observed on the Sun (Gizon et al., 2021). There have been several attempts to model the inertial modes employing several simplifying assumptions. In this work, we use Dedalus (Burns et al., 2020), a flexible spectral code, to compute the eigenmodes in the inertial frequency range. This framework helps us to examine the sensitivity of the modes to different model setups, including incompressible, anelastic, and fully compressible ones. Furthermore, we extend the linear model to include a free-surface boundary condition, the coupling with the radiative interior, and the effects of the magnetic field. In this talk, we shall present two main findings: the assumption of incompressibility is unjustified, and the inertial modes weakly couple with the radiative interior.

12:10 Lunch
Lunch
12:10 - 13:30

13:30 Geoff Vasil: TBA
Geoff Vasil: TBA
13:30 - 14:15

14:15 Yuto Bekki: Effects of small-scale dynamo on rotating columnar convection in stellar convection zones
Yuto Bekki: Effects of small-scale dynamo on rotating columnar convection in stellar convection zones
14:15 - 14:40
In the equatorial region of the stellar convection zone, rotating convection tends to form vortical columns that propagate in a prograde direction. These convective columns are often called “banana cells” or “thermal Rossby waves.” In numerical simulations, they are commonly observed and found to play a significant role in transporting angular momentum, driving solar-like differential rotation. However, they have never been successfully observed in solar surface observations. Bridging this gap between numerical simulations and solar observations remains an open challenge. A physical ingredient likely missing in most numerical models is small-scale dynamo, which is believed to operate vigorously in the Sun and stars but is very costly to resolve numerically. In this talk, we report a series of high-resolution numerical simulations of rotating magneto-convection using a local f-plane box at the equator with varying Rossby numbers. We find that with the presence of small-scale dynamo, thermal Rossby waves have smaller amplitudes and higher longitudinal wavenumbers. We also find that the generation of mean zonal flow is significantly suppressed by the small-scale dynamo, as the Maxwell stresses counteract the Reynolds stresses. Finally, we will briefly discuss possible implications for the convective conundrum.

16:30 Reception (TBA)
Reception (TBA)
16:30 - 18:30
Tuesday, 27 August 2024

09:30 Dominic Bowman: An asteroseismic view of convective boundary mixing in massive stars
Dominic Bowman: An asteroseismic view of convective boundary mixing in massive stars
09:30 - 10:15
During the main sequence the convective cores of massive stars act as engines that drive their evolution, but direct inference of core masses is challenging. Moreover, estimates are subject to unconstrained convective boundary mixing (CBM) processes owing to largely uncalibrated prescriptions in 1D stellar evolution models. The uncertain chemical and angular momentum transport mechanisms can lead to unwieldy interior mixing and rotation profiles, thus making it difficult to predict a massive star's evolutionary fate. However, thanks to ongoing space missions and our development of modern asteroseismic modelling techniques for massive stars, we are now able to deduce precise convective core masses and robustly measure (non-rigid) radial rotation profiles in main-sequence stars that span a wide range in mass and age within the HR diagram. In this talk, I will provide an introduction to asteroseismology of massive stars for the non-expert and highlight recent modern advances in forward asteroseismic modelling of such stars. The combination of space photometry, high-resolution spectroscopy, and Gaia astrometry for massive stars allows precise measurements of masses, core masses, and ages to better than 10-20% precision. Asteroseismic modelling of gravity-mode period spacing patterns and rotational multiplets also allow CBM, as well as the near-core and envelope rotation profiles to be inferred, thus providing important anchor points for calibrating angular momentum transport processes. Finally, the inclusion of magnetic fields in forward asteroseismic modelling also allows the strength and geometry of such fields and their impact on CBM to be probed through magneto-asteroseismology.

10:15 Markus Roth: Probing Large-scale flows with eigenfunction perturbation analysis
Markus Roth: Probing Large-scale flows with eigenfunction perturbation analysis
10:15 - 10:40
Large-scale flows and magnetic field components inside the Sun or solar-like stars affect the resonant oscillations by perturbing the oscillation eigenfunctions. By eigenfunction perturbation analysis, conclusions can be drawn on these physical quantities.

10:40 Coffee
Coffee
10:40 - 11:10

11:10 Catherine Blume: Inertial Oscillations in the Convection Zone
Catherine Blume: Inertial Oscillations in the Convection Zone
11:10 - 11:35
Recent observations of Rossby waves and other more exotic forms of inertial oscillations in the Sun’s convection zone have kindled the hope that such waves might be used as a seismic probe of the Sun’s interior. Here, we present a 3D numerical simulation in spherical geometry that models the Sun’s convection zone and upper radiative interior. This model features a wide variety of inertial oscillations, including both sectoral and tesseral Rossby waves, retrograde mixed inertial modes, prograde thermal Rossby waves, the recently observed high-frequency retrograde (HFR) vorticity modes, and what may be latitudinal overtones of these HFR modes. We suggest that many of the retrograde inertial waves that appear in the convection zone, including the HFR modes, are in fact all related, being latitudinal overtones that are mixed modes with the prograde thermal Rossby waves. This unifying picture greatly reduces the many different observed and modeled waves in the convection zone into two categories: equatorial Rossby waves and this new collection of mixed modes

11:35 Whitney Powers: Searching for signatures of oscillation in turbulent, low Prandtl number convection
Whitney Powers: Searching for signatures of oscillation in turbulent, low Prandtl number convection
11:35 - 12:00
In a rotating system with low Prandtl numbers (Pr < 0.7) the onset of convection occurs as oscillations rather than the stationary onset observed in non-rotating Rayleigh-Bénard convection. As we raise the Rayleigh number above onset, standard stationary convection will occur, however the oscillatory branch persists, and at low wavenumbers the system is unstable to oscillations but not to stationary convection. Studies of solar super-granulation such as Beck and Duvall (2001) show that the auto-correlation function for super-granulation becomes anti-correlated after approximately 40 hours. This behavior is reminiscent of the oscillatory branch of low Prandtl number rotating convection. We present simulations of low-Prandtl number rotating convection to determine if oscillatory signatures persist above convective onset, and if this mechanism could explain the anti-correlation of solar super-granulation.

12:00 Lunch
Lunch
12:00 - 13:30

13:30 Lisa Bugnet: TBA
Lisa Bugnet: TBA
13:30 - 14:15

14:15 Dhruba Mitra: Towards magnetoseismology : surface signature of sub-surface magentic fields
Dhruba Mitra: Towards magnetoseismology : surface signature of sub-surface magentic fields
14:15 - 14:40
We solve for waves in a stratified medium with a spatially varying background magnetic field that points along a horizontal (x) direction, and with gravity that is directed along the vertical (z) direction. Static force balance determines the magnitude of the background magnetic field. We consider both an isothermal and a more realistic polytropic atmosphere. In both cases we calculate how the presence of the sub-surface magnetic field changes the the dispersion relations for the surface waves. Applications of our result are in magnetoseismology and nonlinear asteroseismology.

14:40 Kishore Gopalakrishnan: Magnetic effects on helioseismic modes in simulations of convection
Kishore Gopalakrishnan: Magnetic effects on helioseismic modes in simulations of convection
14:40 - 15:05
Observationally, localized strengthening of the f mode is known to precede the emergence of solar active regions by up to 48 hours. Similar effects have been found in simplified numerical models. For the first time, we have been able to demonstrate such effects in a 3D simulation of convection. While a magnetic field near the top of the convection zone (CZ) strengthens the f mode, a magnetic field of equal strength near the bottom of the CZ produces a much weaker effect. I will also talk about how unresolved small-scale magnetic fields can be probed using local helioseismology. If time permits, I will also demonstrate the effect of internal reflection on the number of radial nodes of the p mode. This resolves a long-standing disagreement between simulations, where it has been reported that the lowest p mode has zero radial nodes, and observations, where the lowest p mode is thought to have one radial node.

15:05 Coffee
Coffee
15:05 - 15:35

15:35 Bradley Hindman: The Implications of the Sun's Differential Rotation on the Transport of Heat and Angular Momentum
Bradley Hindman: The Implications of the Sun's Differential Rotation on the Transport of Heat and Angular Momentum
15:35 - 16:20
We have known since the observations of Galileo that the Sun rotates differentially, with its equator rotating faster than its poles. More recently, helioseismology has demonstrated that this latitudinal variation in the rotation rate only occurs within the Sun's convection zone, while the underlying radiative interior rotates like a solid body. For obvious reasons, the sense of differential rotation with a rapidly rotating equator is called solar-like and the converse (rapidly rotating poles) is called antisolar. Through a variety of observational techniques we now know that the Sun is not alone; most if not all main sequence stars for which differential rotation can be measured possess solar-like differential rotation, whereas a handful of more evolved stars have been demonstrated to be antisolar. The Sun's observed rotation profile is a rich source of information about fluid transport properties within the solar interior, in particular, the transport of angular momentum and heat. In this review talk, I will present two fundamental puzzles that quickly arise when one considers the torque balance required to achieve the observed rotation profile: (1) why does the Sun's convection zone rotate with a fast equator? and (2) why does the radiative interior rotate like a solid body? The first of these puzzles emerges from the belief that turbulence should mix and homogenize angular momentum, which should therefore lead to antisolar differential rotation. The second emerges from the well-known tendency of latitudinal shear to "burrow" into neighboring stable layers on a short time-scale compared to the solar age. In other words, since the Sun's convection zone rotates differentially, why hasn't the radiative interior been dragged into a similar shearing state? I will present the current theoretical paradigm of angular momentum transport within a Sun-like star and discuss unresolved problems and weaknesses in this paradigm. Further, I will summarize recent work by several different authors that suggest that magnetism plays a crucial role in the Sun's torque balance and may provide an answer to the two puzzles

16:20 Yoshiki Hatta: Inversion for inferring solar meridional circulation: the case with constraints on angular momentum transport inside the Sun
Yoshiki Hatta: Inversion for inferring solar meridional circulation: the case with constraints on angular momentum transport inside the Sun
16:20 - 16:45
Meridional Circulation (MC) in the Sun is an essential component in the solar dynamo mechanism. There have thus been a number of attempts to infer the solar internal MC profile via, e.g., time-distance helioseismology. We have however not reached an agreement even about the large-scale morphology of the internal MC profile. For example, whether the MC profile is overall single-cell or double-cell is not evident. This is partly due to the difficulty in inverting measured travel times in which the signal of the solar MC is small. In this talk, we present inversion results obtained with an additional constraint that the angular momentum (AM) transport by MC should be equatorward. Putting this physical constraint is motivated by a recent numerical result (Hotta and Kusano 2021, Nature Astronomy) where the solar equator-fast rotation is successfully reproduced without any tweaking. Inversion of the travel times measured by Gizon et al. (2020, Science) with this constraint results in a double-cell MC profile. Our result is compatible with a theoretical argument that the AM transport by single-cell MC is always poleward when we assume the mass conservation in the convective zone. However, we have also confirmed that the averaging kernels targeting around the deep convective zone are not well localized enough for us to conclude that the solar MC profile is double-cell. Although we have thus not reached a definitive conclusion on the large-scale morphology of the solar MC profile yet, our attempts highlight the relevance of investigating the solar MC profile from both theoretical and observational perspectives.
Wednesday, 28 August 2024

09:30 Meridith Joyce: A Review of One-Dimensional Parameterizations of Convection and Their Applications
Meridith Joyce: A Review of One-Dimensional Parameterizations of Convection and Their Applications
09:30 - 10:15
The treatment of convection in one dimension is a drastic simplification of an inherently three-dimensional process based on the bulk motion of fluids. However, one-dimensional parameterizations of convection remain necessary and useful in a number of applications, including the construction of stellar tracks, isochrones, and population synthesis models, and they perform reasonably well in these contexts. In this review, I will discuss the applications of one-dimensional treatments of convection, especially the Mixing Length Theory, in stellar interiors and stellar evolution. I will summarize the history of MLT and discuss its interactions with other modeling physics, including demonstrating the impact of variations in the convective mixing length on stellar models. I will review the successes and shortcomings of this formalism, as well as attempts to improve and extend it, including the Full Spectrum Turbulence model. I will discuss situations in which the use of time-dependent convection is worthwhile and the ways in which three-dimensional convective simulations might inform and improve one-dimensional treatments of convection in the future.

10:15 Felix Ahlborn: Hydrodynamic simulations as a test bed for turbulent convection models
Felix Ahlborn: Hydrodynamic simulations as a test bed for turbulent convection models
10:15 - 10:40
To date, the mixing length theory (MLT) is still the most common way to model convection in stars. However, MLT is neglecting important aspects of stellar turbulence. As an alternative, we implemented the turbulent convection theory by Kuhfuss (1987), in the stellar evolution code GARSTEC, which provides a more accurate description of the turbulent flow field in one spatial dimension. Using the GARSTEC models with Kuhfuss convection, we modelled a convectively burning main-sequence star. Subsequently, we set up three-dimensional hydrodynamic simulations based on the stellar models to compare with the results of the turbulent convection theory. These simulations were performed at the nominal luminosity of the star using the SLH (Seven-League-Hydro) code, which specialises in low Mach number flows. The hydrodynamic simulations confirm that the Kuhfuss theory accurately predicts the most relevant quantities for stellar structure and evolution, e.g. the turbulent kinetic energy profile or the morphology of the thermal stratification. We conclude that the Kuhfuss theory is an appropriate description of turbulent convection for stellar models.

10:40 Coffee
Coffee
10:40 - 11:10

11:10 Nobumitsu Yokoi: Non-equilibrium turbulence effects in stellar convection
Nobumitsu Yokoi: Non-equilibrium turbulence effects in stellar convection
11:10 - 11:35
Plumes are considered to play an important role in the transport in stellar convection. The non-equilibrium effect associated with plumes is linked to the variations of turbulence properties along the plume motions. With the response-function formulation of the renormalised perturbation theory, the non-equilibrium properties of turbulence can be incorporated into the analytical expressions of the turbulent fluxes such as the turbulent mass flux, the Reynolds and turbulent Maxwell stresses, and the turbulent heat/energy flux. A turbulence model with this non-equilibrium effect incorporated is proposed. This non-equilibrium turbulence model is applied to a two convection configurations: the locally or entropy-gradient driven convection and the non-locally or surface-cooling driven convection. The validation of the non-equilibrium turbulence model is sought in these two cases by comparing the results of turbulence model with those of direct numerical simulations (DNSs). The statistical and mean properties of turbulence in the two convection configurations are discussed, including the analysis of the probability distribution function and the turbulent energy flux.

11:35 Catherine Lovekin: Updates to SPHERLS: Radial stellar pulsation and convection
Catherine Lovekin: Updates to SPHERLS: Radial stellar pulsation and convection
11:35 - 12:00
We present a newly updated version of SPHERLS, which can be used for modelling the interaction of convection and pulsation in radial pulsators. We present preliminary calculations to verify performance for RR Lyrae stars, as well as extensions to Cepheids. SPHERLS will be made publicly available, and is expected to have applications to a number of outstanding problems in understanding RR Lyrae and classical Cepheids.

12:00 Lunch
Lunch
12:00 - 13:30

13:30 Friedrich Kupka: Fully turbulent RHD simulations and Reynolds stress models as tools for studying convective overshooting in stars
Friedrich Kupka: Fully turbulent RHD simulations and Reynolds stress models as tools for studying convective overshooting in stars
13:30 - 14:15

14:15 Manfred Küker: Simulations of convection in cool stars
Manfred Küker: Simulations of convection in cool stars
14:15 - 14:40
We present numerical simulations of convection and magnetic field generation in stars with outer convection zones. We study the convection pattern, the generation of small-scale and large-scale magnetic fields, differential rotation, and meridional flows for different rotation rates and geometries

14:40 Coffee
Coffee
14:40 - 15:10

15:10 Åke Nordlund: The Volleyball Sun Experiment
Åke Nordlund: The Volleyball Sun Experiment
15:10 - 15:55
The Volleyball Sun experiment is based on the DISPATCH code framework, and is the first simulation of the Sun that covers the whole convection zone using no modifications of the physics (fully compressible MHD, realistic equation of state, with no modification of phase speeds). The convection zone is covered by a large number (up to more than 5 million) of small Cartesian "patches" (3D data cubes), with overlapping guard zones. The patches are arranged in a “volleyball geometry”, with 6 identical “faces”, in which patches are lined up in the (locally) longitudinal direction, with constant latitudinal offsets. The patches generated on the first face are duplicated, via permutation and reflection operations, to the remaining 5 faces. Each patch is exactly Cartesian (unigrid, with optional adaptive mesh refinement), with one axis exactly vertical, and the spherical geometry only enters via the guard zone interpolation mechanisms, which also handle the transformation of vector variable between the slightly tilted neighbors of each patch. The HD and MHD solvers can in principle be chosen freely, but to avoid problems in handling the very nearly adiabatic internal layers, we choose to use Riemann solvers with entropy per unit volume as the energy-related conserved variable. We use the FreeEOS equation of state, represented by a fast tabular lookup procedure. The calculations are carried out at the LUMI supercomputing center, under an Extreme Scale Access grant from EuropHPC. I will present first results, and additional details about the experiment, including methods to utilize GPU off-loading to handle radiative energy transfer and charged particle acceleration in the surface layers. On the basis of this first experiment, we plan to continue with a number of “zoom in” simulations, which use the larger scale results as initial and boundary conditions, while extending the computational domain locally into the chromosphere and corona, offering the opportunity to model, for the first time ab initio, the dynamics controlling solar “active regions”.

15:55 Tao Cai: Vortices in turbulent rotating convection: a new challenge in stellar convection theories
Tao Cai: Vortices in turbulent rotating convection: a new challenge in stellar convection theories
15:55 - 16:20
The influence of rotation on stellar convection remains a complex and not fully understood phenomenon. We use numerical simulations on f-planes to study the impact of rotation on stellar convection. Our findings indicate that large-scale vortices can be naturally generated as the rotational effect intensifies. Initially, with the increase in the rotational effect, the emergence of a large-scale cyclone is noted. As the rotational effect continues to amplify, we observe the appearance of both large-scale cyclones and anticyclones. This phenomenon is not limited to a specific latitude, as it has also been observed in the simulations of f-planes conducted at lower latitudes. When we incorporated the geometric effect into our study, we made an intriguing observation - the formation of vortex crystals in the polar regions. We notice that energy and vorticity transfers can be significantly different when large-scale vorticites appear, which brings a new challenge in stellar convective theories.

19:00 Conference dinner (TBA)
Conference dinner (TBA)
19:00 - 21:00
Thursday, 29 August 2024

09:30 Oleg Kochukhov: Convection and magnetic fields across the Hertzsprung-Russell diagram
Oleg Kochukhov: Convection and magnetic fields across the Hertzsprung-Russell diagram
09:30 - 10:15
Depending on the stellar mass, evolutionary phase, and interior structure, convection can be the source of stellar magnetism or be mutually exclusive with the presence of strong magnetic fields. In this talk, I will present an observational perspective on this highly nuanced relationship between stellar convection and magnetism. I will review observational evidence for the existence of magnetic fields on stellar surfaces and relate it to the convective behaviour of several interesting groups of main sequence stars.

10:15 Quentin Noraz: Magnetochronology of solar-type stars dynamos
Quentin Noraz: Magnetochronology of solar-type stars dynamos
10:15 - 10:40
The magnetism and rotation of cool stars evolve in an intertwined manner over secular times. However, recent observations have questioned this link, in particular as solar-type stars older than the Sun possibly exhibit stronger magnetic proxies and rotate faster than predicted. To assess how the combination of rotation and convection via the Rossby number influences the type of rotation and magnetism established, we analyse a set of 15 global MHD models of solar-type stars dynamo, and confront it to current observations. These models harbor different rotation and dynamo regimes as a function of the Rossby number Ro and show an overall agreement with observational trends, making us able to propose a physics-based ‘Sun in Time’ scenario : While aging and reaching intermediate Ro values, the dynamo nature changes and cycle periods increase to decadal ranges. In addition, we find that the magnetic field amplitude reaches a minimum around Ro~1, suggesting that a stalling of cool stars’ spin-down could originate from a minimum of their magnetism. Then, they may undergo a transition towards anti-solar DR and lose cycles, while building back a stronger large-scale field, and possibly revive their spin-down. We first discuss the numerical evidence of such a scenario, and further present an observational study of the Kepler field, seeking to identify high-Rossby stellar targets in order to constrain the Ro~1 limit. To this end, we developed an new observational formula for Ro, that could also be applied to future missions, such as PLATO.

10:40 Coffee
Coffee
10:40 - 11:10

11:10 Igor Rogachevskii: Convection and magnetic fields of low-mass main sequences stars: Non-linear dynamo theory and mean-field numerical simulations
Igor Rogachevskii: Convection and magnetic fields of low-mass main sequences stars: Non-linear dynamo theory and mean-field numerical simulations
11:10 - 11:35
Our theoretical and numerical analysis of convection and magnetic fields for low-mass main sequences stars (of the spectral classes from M5 to G0) rotating much faster than the Sun, have suggested that the generated large-scale magnetic field is caused by the mean-field $\alpha^2\Omega$ dynamo, whereby the $\alpha^2$ dynamo is modified by a weak differential rotation. Even for a weak differential rotation, the behaviour of the magnetic activity is changed drastically from aperiodic regime to non-linear oscillations and appearance of a chaotic behaviour with increase of the differential rotation. Periods of the magnetic cycles decrease with increase of the differential rotation, and they vary from tens to thousand years. This long-term behaviour of the magnetic cycles may be related to the characteristic time of the evolution of the magnetic helicity density of the small-scale field. The performed analysis is based on the mean-field simulations (MFS) of the $\alpha^2\Omega$ and $\alpha^2$ dynamos and a developed non-linear theory of convection and dynamos.

11:35 Loren Matilsky: Dynamo Confinement of the Solar Tachocline
Loren Matilsky: Dynamo Confinement of the Solar Tachocline
11:35 - 12:00
The solar tachocline is a narrow shear layer (no thicker than ~5% the solar radius), in which strong differential rotation in the convection zone (CZ) transitions to solid-body rotation in the adjacent radiative zone (RZ). How the tachocline can remain so thin at the current age of the Sun, despite the effect of 'radiative spread' (where latitudinal entropy gradients in the CZ spread inward via radiative diffusion and carry along a meridional circulation and differential rotation) remains a long-standing unresolved issue of stellar astrophysics. In the parameter regimes most accessible to global simulations, the simulated tachocline usually spreads viscously instead of radiatively (i.e. the CZ drags the RZ into differential rotation via a higher-than-realistic viscosity). In 2022, we explored a 3-D MHD simulation of a CZ-RZ system in which a dynamo was self-excited in the CZ, spread into the RZ, and confined a tachocline against viscous spread via magnetic torque. As a whole, this result was reminiscent of the 1-D 'fast magnetic confinement scenario', in which a poloidal dynamo-generated field (cycling with a period of 22 years) penetrates below the CZ to a magnetic skin depth, determined by the single cycle frequency. We have recently shown more carefully that the skin effect indeed well describes the amplitude of poloidal field strength in the RZ for several CZ-RZ dynamo simulations at different magnetic Prandtl numbers, even when the cycle is aperiodic (i.e. composed of many distinct frequencies). Overall, these results suggest a much wider range of operation for a general 'dynamo confinement scenario.' To assess if this scenario is realistic for the Sun, we also discuss our latest dynamo simulations for a tachocline in the radiative spreading regime.

12:00 Lunch
Lunch
12:00 - 13:30

13:30 Ansgar Reiners: Empirical constraints on convection: Stellar magnetic fields and solar convective blueshift
Ansgar Reiners: Empirical constraints on convection: Stellar magnetic fields and solar convective blueshift
13:30 - 14:15
Two projects from solar and stellar spectroscopy relevant for stellar convection will be presented: 1) the CARMENES survey for exoplanets around M dwarfs observed 300 stars for more than five years. The entire data set was used to produce high-S/N spectra of the stars from which average surface magnetic fields were measured. The stars cover a large parameter range showing scaling relations relevant for convection and stellar dynamos. 2) In Göttingen, we are operating a 50cm solar telescope with a broadband high-resolution spectrometer that we use for developing spectral calibration techniques. The spectrometer provides unprecedented frequency accuracy with which we can determine line-by-line absolute Doppler shifts. We measured the depth-dependent convective blueshift across the solar surface (at different limb positions) providing useful constraints for solar convection and detailed empirical information about line profiles from the solar atmosphere seen under different projection angles.

14:15 Nishant Singh: On active latitudes and magnetic flux concentrations in convection simulations
Nishant Singh: On active latitudes and magnetic flux concentrations in convection simulations
14:15 - 14:40
Traces of cyclic large-scale magnetic fields are seen at some preferred latitudes in some recent simulations. These seem intimately related to the appearance of large-scale vortices that are in turn affected by the growing magnetic field. Analysis of these simulations reveals that there is no large-scale dynamo, and unlike most previous studies, a small-scale dynamo operates and coexists with the large-scale flows. Spontaneous formation of localized magnetic structures, resembling active regions (ARs) or sunspots, has proved to be more challenging in simulations of turbulent magneto-convection. We will discuss some developments on these topics based on numerical and observational studies.

14:40 Coffee
Coffee
14:40 - 15:10

15:10 Sacha Brun: Powering solar-type stars magnetism: How are magnetic cycles established and driven?
Sacha Brun: Powering solar-type stars magnetism: How are magnetic cycles established and driven?
15:10 - 15:55
We present an extensive study on the dynamo origin of solar-type star's magnetism, based on a series of 32 3D MHD global numerical simulations of rotating magnetised convection. We quantify how the combination of rotation and convection via the Rossby number influences the type of magnetism established (short or long cycles, statistically steady activity) and their expected differential rotation (solar-like, anti-solar, cylindrical or almost solid). This large survey allows us to propose a possible solution to why the Sun possesses a long decadal cycle and a conical differential rotation. The solar conical differential rotation and decadal cycle are recovered in a specific range of Rossby numbers, which opens up the possibility to use this dimensional parameter to define a path in parameter space towards more and more turbulent models while retaining key force balances thought to operate in the Sun. We further assess the amount of energy needed to maintain such angular velocity profiles and magnetic activity. We find that between 0.1 and 3% of the stellar luminosity can be converted into magnetic energy, giving plenty of energy for surface eruptive events to occur. We also compute the magnetic energy spectra and show how the dipole and quadrupole magnetic fields evolve as the Sun ages and compare the trend found with observations finding a good overall agreement. In particular interesting regimes at low and high Rossby number are identified.

15:55 Andrius Popovas: Towards realistic simulations of solar dynamics
Andrius Popovas: Towards realistic simulations of solar dynamics
15:55 - 16:20
Due largely to computational resource limitations, solar research evolved as distinct “internal-” and “surface-” related research fields, preventing an integrated global view of the Sun's complex plasma dynamics. However, the Sun encompasses large-scale hierarchical structures, extending from its deep core to its outer atmosphere. Magnetic flux, pivotal for many phenomena, such as sunspots and solar flares, may be generated through both local and large-scale dynamo actions within the solar interior, interacting with motions in the convection zone that are ultimately driven by cooling at the very surface. The current advancements in high performance computing (HPC) infrastructure finally allows us to address the burgeoning need for an integrated understanding of the solar dynamics from the core to the photosphere and beyond. In this talk I will present the current state of our ongoing work – the global compressible MHD simulations covering the entire convection zone of the Sun.
Friday, 30 August 2024

09:30 Robert Andrassy: Convective boundary mixing: Theory and numerical simulations
Robert Andrassy: Convective boundary mixing: Theory and numerical simulations
09:30 - 10:15
Convection has traditionally been described by the mixing-length theory (MLT) in one-dimensional numerical models of stellar evolution. The MLT, due to its local nature, does not provide any information about mass exchange between a convective layer and a neighbouring stably-stratified layer. Theoretical arguments, laboratory experiments, as well as decades of astronomical observations suggest that convective boundary mixing (CBM) is a real phenomenon playing a vital role in our understanding of stellar physics and evolution. However, the physical processes involved in CBM depend on the type of convection zone in question and the mixing rate is difficult to quantify in most cases relevant to stars. I will provide an overview of our current understanding of CBM along with some historical developments leading to it. I will argue that the growth of convective layers can already be simulated with confidence in late stages of massive star evolution and that simplified hydrodynamic simulations combined with analytical theory are beginning to provide predictive models of CBM even for stars on the main sequence.

10:15 Axel Brandenburg: Entropy rain
Axel Brandenburg: Entropy rain
10:15 - 10:40
The flux from a radiating surface depends significantly on the opacity and its functional dependence on temperature. This is why the correct depth of the convection zone was only known since the discovery of the H-minus opacity by Wildt (1938). This leads to the concept of convection driven by cooling from above rather than heating from below, which is sometimes also called entropy rain. An important feature is that the enthalpy flux cannot be modeled solely by the superadiabatic gradient, but there is also the Deardorff term that carries enthalpy outward. This contribution can also lead to weakly subadiabatic convection and may be responsible for convection on length scales smaller than the local scale height

10:40 Coffee
Coffee
10:40 - 11:10

11:10 Petri Käpylä: Effects of rotation on convective scale and subadibatic Deardorff layers
Petri Käpylä: Effects of rotation on convective scale and subadibatic Deardorff layers
11:10 - 11:35

11:35 Felipe Navarrete: Internal magnetic fields in close binary stars
Felipe Navarrete: Internal magnetic fields in close binary stars
11:35 - 12:00
A long standing problem in proving our theories of convection and stellar dynamos is that observations of stars other than the Sun are difficult to achieve, specially when it comes to inferring what happens inside the convection zone. A special class of close binaries might offer us information about the interior of stars, particularly about the state of the non-axisymmetric magnetic field of low-mass main-sequence stars. In this talk, I will introduce the observations and theory behind this idea, and our current efforts that attempt to address the characterization of such magnetic fields.

12:00 TBA: Closing remarks
TBA: Closing remarks
12:00 - 12:30
Saturday, 31 August 2024
Sunday, 1 September 2024

Monday, 2 September 2024
Tuesday, 3 September 2024
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