July 29 - Aug 3 2018, Boston / Cambridge, USA

The "Cambridge Workshops of Cool Stars, Stellar Systems and the Sun" are held biennially and have evolved to be the premier conference series for cool star research.

Program

The meeting will cover the following five science themes:

Galactic Cartography in the Gaia Era

Starting with our own solar neighborhood and moving to greater distances using luminous stars, what have we learned from the current programs and what will be accomplished in the future? Do these surveys provide quality information needed for modelers and theoreticians to address many problems in stellar evolution, star formation, cluster formation, disk/halo/bulge formation and evolution?

Fundamental Properties of Cool Stars

From asteroseismology of stellar interiors to construction of stellar atmospheres, the physical parameters of cool stars remain fundamental quantities of astrophysics. Our understanding is being refined by new capabilities. Measurement of masses, radii, abundances, rotation are required for stars in the field and in clusters. Understanding of stellar evolution, interpretation of complex color­magnitude diagrams, and characteristics of exoplanet hosts are among the topics that benefit from improvement of these quantities.

Solar/Stellar Environments

Our Sun and stars interact with their surroundings through radiation and plasma. Stellar winds span almost 10 orders of magnitude in flux. Transient events - violent coronal mass ejections and flares - produce both enhanced radiation and particles surrounding a star. The environment can interact with stars as well via the process of accretion. Can we quantify the characteristics of these events and define how these processes change as a star is formed and evolves?

Solar/Stellar Magnetic Fields and Surface Structure

Magnetic fields remain fundamental to the evolution of stars and to their atmospheric structures. A magnetic dynamo drives stellar cycles which in turn affects magnetic field configurations and the angular momentum evolution of a star. How do surface phenomena – such as star spots and flares – change with stellar mass and evolutionary stage? How can we prepare for the arrival of the innovative solar telescope DKIST, which will offer unprecedented spatial resolution of the surface of the Sun?

Very Low Mass (VLM) Objects

Low mass stars and brown dwarfs present one extreme of stellar physics that becomes more prominent as exoplanet hosts. These objects can harbor very cool and puzzling atmospheric structures and behavior. What do we know about their magnetic structures and flaring activity? What are their fundamental parameters such as mass, abundances, atmospheric structures?