We will be happy to receive your abstracts and questions once the new dates are defined
Thanks to those who already submitted, and please remain in contact for 2021!
Cool stars are formed by accretion processes, starting in the Class 0/I phase and lasting well into the Pre-Main Sequence (PMS). Magnetically controlled accretion connects the matter and angular momentum flow in the disk with the central star and affects the disk structure and the formation and migration of planets. Besides being the connection between stellar properties and planets, accretion is a key to understand cool stars.
The last years have seen advances in stellar magnetic fields, accretion rate and disk mass and size estimates, observations of systems with variable accretion, and even the first hints of accretion onto planets, answering some questions but revealing many new ones. How does accretion evolve between the Class 0/Class I and PMS phases? How does the accretion mechanism vary for stars with different masses and ages? And for planets? What is the interplay between accretion and photoevaporation or disk winds? How does accretion proceed in disks with low metallicity, or with low viscosity? Are our measurements of accretion rates biased? In this splinter session, we will address these topics and related issues, bringing together a community of experts in accretion, stars, disks, and planets and aiming to develop future collaborations between accretion-related fields that will continue beyond the meeting.
For this purpose, we are not only collecting abstracts, but also open questions to lead the discussion.
The deadline for the submission of
both is April 17th, and we will notify succesful applicants before May 8th.
The links on the left side will bring you to the form where you can submit your contribution.
The session will be organized as a led open discussion with very brief presentations/notes from selected speakers from among the participants. The aim of the presentations is not to discuss a particular result or object, but rather to focus on the open problems and how these can be tackled from various points of view, including observations and theory.
In order to focus the discussion, we are collecting open questions from among the participants.
Please let us know your own key questions to add them to our list below:
Accretion through the age of the star and through the age of the galaxy: How does accretion vary in time and what effect does it have on the star and forming planets? What happens for disks with different viscosities or metallicities, including low-metallicity stars?
Observational techniques: measuring accretion rates and disks masses, with their limitations and open problems, including measuring accretion in very embedded Class 0/I phases.
The disk mass vs accretion time problem: Are new observations and models (of disks, of accretion variability over time) adding anything new to it? How relevant is disk dissipation through accretion during the optically visible PMS phase compared to other processes such as photoevaporation, winds, planet formation? Is the relative importance of these different processes dependent on the stellar mass, stellar structure (which influences the stellar magnetic field topology and likely the magnetospheric accretion process), or age of the system?
Accretion vs planet migration: How does accretion affect the formation and migration of planets? How does accretion onto the star compare to accretion through the disk? How does accretion variability modify the planet formation regions?
Aurora Sicilia-Aguilar, Justyn Campbell-White, Soko Matsumura, Scott Gregory (University of Dundee)
Ignacio Mendigutía (Centro de Astrobiología, Spain)
Min Fang (Caltech, USA)
Carlo Felice Manara, Gaitee Hussain (ESO, Germany)
Veronica Roccatagliata (University of Pisa, Italy)
Ágnes Kóspál, Peter Ábrahám, Fernando Cruz-Saenz de Miera (Konkoly Observatory, Hungary)
Giovanni Rosotti (Leiden Observatory, The Netherlands)
Created and maintained by A.Sicilia-Aguilar and J. Campbell-White, last update Jan 31, 2020