IAU Commission G5 Talks
Talk organized within IAU Commission G5 (Stellar and Planetary Atmospheres)
(This seminar is organized by the IAU G5 commission on stellar and planetary atmospheres)
Task-based computing is a method where computational problems are split
into a large number of semi-independent tasks (cf.
2018MNRAS.477..624N). The method is a general one, with application not
limited to traditional grid-based simulations; it can be applied with
advantages also to particle-based and hybrid simulations, which involve
both particles and fields. The main advantages emerge when doing
simulations of very complex and / or multi-scale systems, where the
cost of updating is very unevenly distributed in space, with perhaps
large volumes with very low update cost and small but important regions
with large update costs.
Possible applications in the context of stellar atmospheres include
modelling that covers large scales, such as whole active regions on the
Sun or even the entire Sun, while at the same time allows resolving
small-scale details in the photosphere, chromosphere, and corona. In
the context of planetary atmospheres, models of pebble-accreting hot
primordial atmospheres that cover all scales, from the surfaces of
Mars- and Earth-size embryos to the scale heights of the surrounding
protoplanetary disks, have already been computed (2018MNRAS.479.5136P,
2019MNRAS.482L.107P), and one can envision a number of applications
where the task-based computing advantage is leveraged, for example to
selectively do the detailed chemistry necessary to treat atmospheres
saturated with evaporated solids, or to do complex cloud chemistry
combined with 3-D radiative transfer.
In the talk I will give a quick overview of the principles behind
task-based computing, and then use both already published and still
on-going work to illustrate how this may be used in practice. I will
finish by discussing how these methods could be applied with great
advantage to problems such as non-equilibrium ionization, non-LTE
radiative transfer, and partial redistribution diagnostics of spectral
The ExoMol project (www.exomol.com) provides comprehensive spectroscopic data (line lists) for the study of atmospheres of exoplanets and other hot bodies. These line lists serve as input for models of radiative transport through hot atmospheres and are useful for a variety of terrestrial applications. The basic form of the database is extensive line lists; these are supplemented with partition functions, state lifetimes, cooling functions, Landé g-factors, temperature-dependent cross sections, opacities, k-coefficients and pressure broadening parameters. Currently containing 80 molecules and 190 isotopologues totaling over 700 billion transitions, the database covers infrared, visible and UV wavelengths. The field of the HR spectroscopy of exoplanets is growing extremely fast and urgently demands molecular data of high precision. Failure to detect molecules in atmospheres of exoplanets is often attributed to the lack of the underlying quality of
the line positions. These developments have led us to begin a systematic attempt to improve the accuracy of the line positions for the line lists contained in the database. Our new ExoMolHD project aims to provide comprehensive line lists to facilitate their use in characterization of exoplanets using high resolution Doppler shift spectroscopy. Progress on this objective will be presented.
The discoveries of thousands of extrasolar planets have revealed an astonishing diversity in their physical characteristics - orbital properties, masses, radii, temperatures, and host stars. Exoplanets known today range from super Jupiters to Earth-size rocky planets over a wide range of temperatures, including several in the habitable zones of their host stars. Recent advances in atmospheric spectroscopy of exoplanets are leading to unprecedented insights into their atmospheric properties. I will discuss some of these developments in atmospheric characterisation of exoplanets and their implications for understanding atmospheric processes, formation mechanisms, and habitability across a wide range of planetary bulk properties. A survey of theoretical and observational directions in the field will be presented along with some open questions on the horizon.
Meeting ID: 865 5820 3608
The new generation of spectrometers designed for extreme precision radial velocities enable correspondingly precise stellar spectroscopy. It is now fruitful to theoretically explore what the information content would be if stellar spectra could be studied with spectral resolutions of a million or more, and to deduce what signatures remain at lower resolutions. Hydrodynamic models of stellar photospheres predict how line profiles shapes, asymmetries, and convective wavelength shifts vary from disk center to limb. Corresponding high-resolution spectroscopy across spatially resolved stellar disks is now practical using differential observations during exoplanet transits, thus enabling the testing of such models. A most demanding task is to understand and to model spectral microvariability toward the radial-velocity detection of also low-mass planets in Earth-like orbits around solar-type stars. Observations of the Sun-as-a-star with extreme precision spectrometers now permit searches for spectral-line modulations on the level of a part in a thousand or less, feasible to test against hydrodynamic models of various solar features.
The field of Galactic archaeology has been very active in recent years, with a major influx of data from the Gaia satellite and large spectroscopic surveys. The major science questions in the field include Galactic structure and dynamics, the accretion history of the Milky Way, chemical tagging, and age-abundance relations. I will give an overview of GALAH as a large spectroscopic survey, and describe how it is complementary to other ongoing and future survey projects. I will also discuss recent science highlights from the GALAH team and compelling questions for future work.
Accurate non-LTE modelling of stellar spectra, and thus the derivation of accurate stellar properties such as chemical composition, temperature, and surface gravity, depends on reliable atomic data. While inelastic electron collisions are very important even in FGK stars, the relative importance of the more abundant yet less efficient hydrogen collisions has for a long time been a major source of uncertainty. Over the last decades, considerable progress has been made on the theoretical side, as well as with experiments for the important charge transfer processes involving hydrogen, both covering a significant number of astrophysically important atoms. I will review this progress, and discuss where further progress might be needed.
Accelerating Computational Modeling via Neural Networks: Application to Exoplanet Atmospheric Retrieval
IIn physics and astronomy, computationally expensive forward models are often an integral part of preparing experiments/observations, analyzing data, and/or planning future instrumentation/telescopes. In many of these cases, machine learning (ML) models, such as neural networks (NNs), can offer a significant reduction in compute time with minimal loss in accuracy. We demonstrate this approach on the problem of exoplanet atmospheric retrieval, which involves on the order of 10^5 -- 10^6 radiative transfer (RT) model evaluations. We find that the ML RT approach yields the same scientific conclusions as the traditional method, while requiring ~1000x less compute cost for typical setups. We present our open-source software packages that implement this technique, and we discuss broader applications of this NN surrogate modeling approach.
The first magnetic Helium-sdOs: which mergers are magnetic?
Magnetic fields play an important role throughout stellar evolution, and among white dwarfs, the end stage of 95% of all stars, the fraction of strongly magnetic systems is larger than 20%. The origins of magnetic white dwarfs are still under discussion, but it is likely that a significant fraction of them are formed by stellar mergers.
Several types of merger remnants are thought to ignite helium fusion, such as the merger of a helium-WD (He-WD) with a second He-WD, a He/C/O hybrid WD, or a low-mass main sequence star, thus forming a hot subdwarf star. The majority of hot subdwarf stars are helium burning stars with very thin or no hydrogen envelopes. In particular, most of the hot and helium-poor He-sdO stars are thought to be formed by mergers. However, out of hundreds of hot subdwarfs studied over several decades, none showed detectable magnetic fields.
This changed recently, when four almost identical magnetic He-sdO stars were discovered, with mean field strengths between 300 and 500kG.
Why are these stars magnetic while vast majority of other He-sdOs are non-magnetic? This question is still open. In this talk I will give a short introduction to He-sdO stars and their formation and then try to highlight the differences between the four magnetic stars and their non-magnetic cousins.
We present a sample of 734 ultracool dwarfs using LAMOST DR7 spectra, i.e., those having a spectral type of or later than M6, including an L0. All of these red or brown dwarfs are within 360 pc, with a Gaia G magnitude brighter than 19.2 mag, a BP-RP color redder than 2.5 mag and an absolute G magnitude fainter than 9 mag. Their stellar parameters (Teff, log g, and [M/H]) are consistent with being the Galactic thin-disk population, which is further supported by their kinematics using LAMOST radial velocity plus Gaia proper motion and parallax. A total of 77 are detected with the lithium absorption line at 6708 A, signifying youth and substellar nature. We report on their kinematic ages estimated by the velocity dispersion. Thirty five close pairs are identified, of which the binarity of six is discovered for the first time.
Massive stars (at least eight times as massive as the Sun) possess strong stellar winds driven by radiation. With the advent of the so called MiMeS collaboration, an increasing number of these massive stars have been confirmed to have global magnetic fields. Such magnetic fields can have significant influence on the dynamics of these stellar winds which are strongly ionized. Such interaction of the wind and magnetic field can generate copious amount of X-rays, they can spin the star down, they can also help form large scale disk-like structures. In this presentation I will discuss the nature of such radiatively-driven winds and how they interact with magnetic fields.
Unlike the giant planets in the solar system, "hot Jupiter" giant exoplanets are subject to intense stellar irradiation, which drives their atmospheres from ~100 K (in the solar system) to ~1000 to 3000 K. In this talk I will review several aspects of their atmospheric physics and chemistry, with a particular emphasis on the cooler "warm Jupiters" below 1000 K where we expect to see some interesting transitions in atmospheric chemistry and clouds with JWST. I will discuss new JWST spectra and modeling work on 1100 K exoplanet WASP-39b, which will be published in Nature in a few days time, as part of the JWST Early Release Science (ERS) program. The spectra show some expected things but also some very interesting surprises!
Meeting ID: 820 7223 6238
Spectroscopic analyses of stellar chemical compositions are model-dependent, and shortcomings in the models often limit the accuracy of the final results. For late-type stars like our Sun, two of the main problems in present-day methods are that they assume the stellar atmosphere is a) one-dimensional (1D) and hydrostatic, and b) satisfies local thermodynamic equilibrium (LTE). We can relax these assumptions simultaneously by performing detailed 3D non-LTE radiative transfer post-processing of 3D radiative-hydrodynamic model stellar atmospheres. I shall give a brief overview of this approach, and illustrate its impact on carbon, oxygen, and iron abundances in late-type stars.
- Ultra-Diffuse Galaxies (UDGs) and the Stellar Mass – Halo Mass Relationship Dr. Jonah GannonTuesday June 6, 2023 - 12:30 GMT+1 (Aula)
- The complex Milky Way historyDr. Cristina ChiappiniThursday June 8, 2023 - 10:30 GMT+1 (Aula)