Physikalisch-Metorologisches Observatorium Davos -- World Radiation Center pmod-wrc

Solar Physics at PMOD/WRC

Solar Physics at PMOD/WRC

The Solar Physics at PMOD is currently involved in the following research projects

  • Solar Irradiance Modeling

    • Modling the solar EUV spectrum

      • Our approach to model spectral irradiance variations is to calculate intensity spectra for different features on the solar disk. The features are identified from intensity images taken with the Precision Photometric Solar Telescope and the Extreme UV Imaging Telescope onboard the ESA/NASA satellite SOHO. Weighting the intensity spectra with the time-dependent relative area covered by the features yields the time-dependent spectral irradiance. For visible and UV wavelength ranges similar approaches have already been employed by Fontenla and Harder (2005), and Haberreiter et al. (2005).
      • For the photosphere, chromosphere, and TR we employ the latest semi-em\-pi\-rical atmospheric structures by Fontenla et al. (2009). These structures can be downloaded here. The notation follows the one presented by Fontenla et al. (2009), i.e. Model B 1001: intergranular cells, Model D 1002: quiet network, Model F 1003 active network. For these structures we solve the full NLTE radiative transfer for the most abundant elements from hydrogen to iron up to an ion charge of two. For the coronal structure the temperature gradient has been derived by semi-empirically adjusting temperature values from eclips observations by Singh et al. (1982). The density values are extended from the Transition Region to the corona based on the values given by Doschek (1997). Currently, the structures are purely semi-empirical, so hydrostatic equilibrium has not yet been validated. In a future version we will consider the radiative losses and also account see whether the hydrostatic equilibrium can be applied to the models. Details on the models will also continuously be updated on this webpage.
      • The model atmospheres for the lower atmosphere, i.e. the photosphere, chromosphere and transition region can be obtained from here
      • The model atmospheres for the corona can be obtained from here

      • Please send requests to

    • Modeling the solar UV spectrum

    • Modeling the solar spectrum from the UV to the visible and IR

  • Helioseismology

  • Impact of Solar Irradiance on the Earth atmosphere and climate

  • Please find a list of publications of the Solar Group here

Reponsible for this page is Margit Haberreiter ; last update: January 11, 2011

Dorfstrasse 33, CH-7260 Davos Dorf, Phone +41 58 467 51 11, Fax +41 58 467 51 00