High-cadence synoptic program of the
Extreme-ultraviolet Imaging Telescope

Solar Physics Department
of the Royal Observatory of Belgium

Contact: Dr. Frédéric Clette


Contents
  • Guidelines and rules
  • Procedure definitions and options
  • First campaigns evaluation
  • Data pre-processing


    • Past campaigns
    # Cmp # Date EIT TRACE ROB lead
    1 test 19 Nov 2000 304 1600/WL Frédéric Clette
    2 6724 19 Apr 2001 195 171 Frédéric Clette
    3 6776 11 Jul 2001 304 171 Erwin Verwichte
    4 6816 13 Oct 2001 195 171 Erwin Verwichte
    5 6843 17 Jan 2002 304 171 Jean-Francois Hochedez
    6 6852 27 Mar 2002 195 171 Frédéric Clette
    7 6880 27 Aug 2002 304 171 Claire Foullon
    8 6899 13 Oct 2002 195 171 Jean-Francois Hochedez
    9 6916 8 Jan 2003 304 171 Erwin Verwichte
    10 6928 27 Mar 2003 and
    2 Apr 2003    		 195 171 David Berghmans


    Future campaigns
    # Cmp # Date EIT TRACE ROB lead
    11 TBD 24 Jun 2003 and
    28 Jun 2003    		 304 171 Jean-Francois Hochedez
    12 TBD 9-10 Sep 2003 and
    17 Sep 2003    		 195 171 David Berghmans


    EIT Homepage at GSFC

    		Scientific Aim

    The scientific aim of the EIT high-cadence synoptic program is to monitor long-term changes in the small-scale dynamics of all kinds of solar structures (Active Regions, Quiet Sun, Coronal Holes, etc.), using high-cadence sequences made by the Extreme-ultraviolet Imaging Telescope (EIT). The program is thus planned on the long term (need for regular time intervals of 1 to 3 months), and should eventually last for years until EIT or SOHO dies.

    Program Characteristics

    We need a wide field of view to include as many (preferably all) kinds of solar regions as possible, including the solar limb. Our basic field of view is thus essentially a quarter-disk (see Figure) : one corner is near disk center and the outer edges are just beyond the limb at the pole and equator.

    With such a field of view and using the shutterless mode of EIT, we can achieve a 68s cadence with an effective exposure quite larger than the standard synoptic exposures (best for CH and QS).

    Based on instrument safety concerns (radiation induced aging), the compromise for the baseline duration was set to 2 hours.

    As we want to monitor the Transition Region as well as the corona, we run the sequences alternately in 2 bandpasses: 304Å and 195Å (with occasionally a third one: 171Å). We started with a 304Å sequence in December 2000.