Get Involved!

We welcome correspondence concerning the possibility that data from the UVCS/SOHO instrument might be useful in your research program. Please request any information that might help you identify a use for UVCS data in your research. UVCS is a complex spectroscopic instrument and there are subtle techniques involved in analyzing the data. Therefore, we enourage you to enter into collaborations with the scientists already involved in UVCS operations and data analysis.

In general, UVCS is a spectroscopic instrument that observes the extended solar corona from about 1.3 to 11.8 solar radii with a spatial resolution of about 15 arcsec. Often, the spatial resolution is degraded to improve statistical accuracy. Coronal holes are observable up to about 4 solar radii and streamers up to at least 8 solar radii. UVCS can also observe stars, comets, interplanetary H I, and planets at projected heliocentric heights up to 11.8 solar radii, and it can observe from disk center to 1.3 solar radii, although we try not to do that often because of concerns about detector aging and optics contamination (polymerization).

UVCS provides ultraviolet diagnostic techniques to determine velocity distributions for protons, electrons and minor ions; outflow velocities for protons, O5+ and other ions, particle densities, and elemental abundances. We have observed about 31 spectral lines in the extended solar corona for H I and ions of C, N, O, Mg, Al, Si, S, and Fe.

A Statement of Data Policy is available.

If you would like to get more involved in UVCS, please contact Leonard Strachan (lstrachan 'at' cfa 'dot' harvard 'dot' edu) or any other UVCS team member

Created by Raid Suleiman
Last Modified on 10/17/13