Spectroscopic mode identification of non-radially pulsating stars (Karen Pollard; University of Canterbury)

From December 07, 2017 13:35 until December 07, 2017 13:55

At Instituto de Astrofísica, Pontificia Universidad Católica, Vicuña Mackenna 4860, Santiago, Chile

Categories: Seminarios

Asteroseismology has developed into a tool of tremendous power thanks to the availability of high-cadence, long-term, high-precision photometry from space missions such as MOST, CoRoT, Kepler and BRITE. Ground-based spectroscopic measurements of stellar oscillations provide additional and complementary information to the intensity variations provided by space telescopes. Spectroscopic observations provide a way to physically map the pulsational variations across the stellar disk and are capable of detecting higher degree modes to which photometric methods are insensitive.

In this talk I will describe our program to carry out long-term high-resolution spectroscopic observations of various non-radially pulsating stars at the University of Canterbury Mt John Observatory (Lat: –44.0°, Long: 170.5°E). Of special asteroseismic interest are the ? Dor stars, which are slightly hotter and more massive than the Sun. These stars display gravity modes that propagate deep inside the stars, providing information about interior layers as deep as the core.