Magnetic fields in the Sun and Low-mass stars

Cool Stars 22 • June 24-28, 2024

Welcome to the CS22 splinter session webpage:
Magnetic fields in the Sun and Low-mass stars

Artist view of EV Lac - Credit: Casey Reed/NASA

Motivations

Magnetic fields play a crucial role in the birth, evolution and variability of stars. From atmospheric structure to flares, the presence of magnetic fields has a direct or indirect influence on recorded data and on the properties deduced from observations.

In the recent years, the new generation of high-resolution spectrometers and spectropolarimeters led to an increasing number of publications focused on measurements of magnetic fields of the Sun stars and low-mass stars. Those require innovative techniques and state of the art models, and raise fundamental questions regarding stellar magnetic fields: how are they generated? How do they evolve? How do large-scale and small-scale fields relate to one another? How do those magnetic fields affect the habitability and evolution of planetary systems?

In this session, we aim at addressing those questions by inviting experts on magnetic fields in the Sun and low-mass stars.

Program

The detailed program will be posted below as soon as it is available. We are looking forward to your contributions to complete the program.
To comply with the 90 minutes limit of the splinter session, we ask our contributing speakers to respect a 10 minute limit for their presentations including questions.

I - Magnetic fields from resolved to unresolved structures

Invited speaker:

S. Solanki [Max-Planck-Institut für Sonnensystemforschung]: The Sun as a resolved magnetic star

Contributed talks:

A. Finley [CEA Paris-Saclay]: How well does surface magnetism represent the dynamo action in cool stars?
F. Chiti [University of Hawaii]: Magnetic Activity and Stellar Spin-Down: Probing the Fully Convective Boundary using WD+MS Binary Systems

II - Techniques, models and results on stellar magnetic fields