University of Cambridge > Talks.cam > Institute of Astronomy Colloquia > Detecting and Characterising Giant Planets with Direct Imaging

Detecting and Characterising Giant Planets with Direct Imaging

Add to your list(s) Download to your calendar using vCal

If you have a question about this talk, please contact Simon Hodgkin.

Direct detection, and direct spectroscopy in particular, have great potential for advancing our understanding of extrasolar planets. In combinations with other methods of planet detection, direct imaging and spectroscopy will allow us to eventually: 1) fully map out the architecture of typical planetary systems and 2) study the physical properties of exoplanets (colors, temperatures, etc.) in depth. I will discuss in particular the constraints on the distributions of wide giant exoplanets placed by the current generation of direct imaging surveys. Variability attributed to cloud structure already appears to be a persistent feature for L and T type field brown dwarfs, potentially due to the breakup of thick silicate and iron condensate clouds during the L to T spectral type transition. Directly imaged planets occupy the same temperature regime as L and T type brown dwarfs and are likely to be equally variable. I will also discuss the prospects for detecting and characterising exoplanet weather patterns through monitoring the intrinsic photometric variability of these objects.

This talk is part of the Institute of Astronomy Colloquia series.

Tell a friend about this talk:

This talk is included in these lists:

Note that ex-directory lists are not shown.

 

© 2006-2024 Talks.cam, University of Cambridge. Contact Us | Help and Documentation | Privacy and Publicity