Prior to that, he was a Reader in the Astronomy Unit and School of Mathematical Sciences at Queen Mary University of London (formerly Queen Mary & Westfield College, University of London).
Michael was a long-term visiting scientist in 19, and an NCAR Affiliate Scientist from 2003 until his appointment as HAO Director.
Those simulations, and the seismological evidence with which they are being confronted, are reviewed elsewhere in this volume.
Our understanding of the global dynamics of the radiative interior of the Sun is in a much more primitive state.
Oscillation modes from each frequency range are sensitive to different layers in the solar sub-surface interior.
Thompson is NCAR Deputy Director and Chief Operating Officer, a position in which he has served since October 2013.
He concurrently served as interim UCAR President for thirteen months form 2015 to 2016.
From 2010 to 2014 he was Director of NCAR's High Altitude Observatory (HAO) and an NCAR Associate Director. Prior to his NCAR appointments, Michael was Head of the School of Mathematics and Statistics in the University of Sheffield, UK; and previously he was Professor of Physics and Deputy Head of the Space and Atmospheric Physics Group at Imperial College, London.
For a short overview of helioseismology, click here.Michael's scientific research activity is principally in helioseismology, asteroseismology, solar physics, and inverse problems.He has worked extensively over more than 25 years in developing and applying inverse techniques in helioseismology, and in particular measuring the stratification, rotation, and large-scale flows in the solar interior.Historically, great advances in our understanding of the solar interior have been due to helioseismology, the study of 5-minute solar internal oscillations (3).In the mid 1980s global-mode frequencies were used to measure the depth of the solar convective envelope at 0.71 solar radius, deeper than previous expectations based on underestimated opacities.