Philip S. Muirhead
Department of Astronomy, Boston University
M dwarf stars present many advantages for the detection and characterization of rocky and temperate exoplanets; however, the stars themselves present many challenges to observers trying to measure fundamental properties such as mass, radius and metallicity. At BU, we recently began a comprehensive program to characterize M dwarf properties using multi-wavelength observations of eclipsing binary stars, high-resolution near-infrared spectroscopy, and state-of-the-art atmosphere simulations. I will present results from our research group that suggest many eclipsing binary M dwarfs in the literature have erroneous mass and radius determinations. I will also present results that suggest the carbon-to-oxygen ratio in M dwarf stars regulates metallicity indicators in M dwarf spectra, rather than the overall metallicity itself. The results have significant implications for detailed studies of M dwarf planets in the Gaia, TESS, and JWST era.
2016 March 10, 13:30
Centro de Astrofísica da Universidade do Porto (Auditorium)
Rua das Estrelas, 4150-762 Porto