Tentative program as of July 11, 2012.
Where the observations come from:
- Ground-based surveys and programs (OGLE, MACHO, WASP, HATNet, etc.)
- Spectrophotometric surveys
- Space observatories (MOST, Corot, Kepler)
What physical information on stars can be determined from high-precision photometry?
The state of solar and stellar models and their weaknesses and uncertainties.
Advanced tests of stellar structure from seismology:
- Measuring the depth of stellar convective envelopes
- Measuring the helium ionization discontinuity, which indicates the helium abundance
- Inferring internal rotation in stars
- Measuring the depth of composition discontinuities, such as the H/He layer in white dwarfs
- Inferring radial differential rotation
Stellar population studies enabled by seismology:
- Measuring mass, radius, and age from seismology
- The complementarity of seismology and conventional observations in setting fundamental parameters such as temperature and composition
- Using results from seismology to improve and calibrate empirical age properties such as rotation and activity
Going beyond the star as a perfect sphere:
- Understanding the origin and evolution of stellar magnetic fields and activity. Do magnetic fields influence stellar structure? Can we explain solar-like winds? How does activity affect habitability in the circumstellar environment?
- Rotation in all kinds of stars and angular momentum transport. Does rotation drive interior mixing? Does rapid rotation trigger supernovae?
- What are the origins of highly-magnetized stars?
- What determines the extent of convective regions, especially convective cores, in massive stars?
- What causes mass loss in massive stars? Is most of the mass lost during the main sequence, or in severe episodes after?
- What is the physics of mass loss in cool giants? Is most mass in first ascent giants lost at the helium flash or before?
- Interacting binaries are thought to generate many interesting classes of objects; do we have the story right? For example, do SN Ia arise from a single or double degenerate origin?
- Do we understand chemical evolution?
Pulsating stars in a new light from space and from the ground:
- δ Scuti stars
- β Cephei stars
- RoAp stars
- Slowly-pulsating B stars
Compact stars (e.g., white dwarfs) and their variability
Singular and unusual phenomena
Eruptive and flaring behavior in stars
The growth, evolution, and decay of spots on late-type stars
Binary stars as tests of stellar models, including eclipsing binaries
The future for precision tests:
- What's needed from models
- New projects and missions (e.g., SONG, WFIRST, LSST, Pan-Starrs)
Joint Discussion 13 is part of the scientific programme of the XXVIII General Assembly of the International Astronomical Union, which will take place in Beijing, China, August 27-31 2012. This website contains information directly relevant to the Special Session #13: High-Precision Tests of Stellar Physics from High-Precision Photometry. Please check the GA website for all other information, including accommodations, social program, Visa information, etc.