Hinode EIS Initial Science Plan

The EIS Science Working Group (SWG) was formed at the April 01 Science meeting at MSSL,
and consists of Louise Harra, Ken Dere, George Doschek, Hirohisa Hara, Helen Mason,
Peter Young, Viggo Hansteen and Peter Cargill. The aim is to prioritise the observing plan
for the first few months of observations. We also put forward recommendations for long
term use the EIS Core Science Programme and Synoptic Studies.

We will aim for the following science targets which are addressed in the "Main Science Goals of Hinode" :

Core line list:

We will include 3 lines in ALL studies for a consistent dataset during the mission.
The core line list is:

  1. He II 256
  2. Fe XII 195
  3. Ca XVII 192.8
These are based on line strength, cleanliness and temperature range.

Flare trigger/dynamics
- spatial determination of evaporation and turbulence in flares.

Active region heating
- spatial determination of the velocity field in active region loops over a range of temperatures.

Quiet Sun and Coronal Hole Boundaries
- determination of the relationship between the various categories of quiet Sun brightenings
(e.g explosive events and blinkers) both in the quiet Sun and coronal holes. EIS has
the spatial and velocity resolution to solve this mystery.

The observing time will be split evenly between the topics. If there is an active region we will track it,
otherwise we will observe quiet Sun and coronal holes for long periods of time (at least 12 hours).

When there is an active region, we will track it, and if there is a highly sheared magnetic field then we
will go into flare trigger mode to respond to XRT's trigger.

If there are no active regions but there is a quiet prominence, we concentrate on this.

The initial plan was last updated May 2005.

Last Revised: Monday, 24-Jul-2006

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