Coordinated Observations of Strllar Flares

Details Coordinated Observations of Strllar Flares Coordinated Observations of Strllar Flares

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1821h&link_type=abstract

IUE Proposal ID #FSGBH

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Scientific paper

We are proposing to observe four UV Ceti-type flare stars to obtain discrete, time resolved spectra of stellar flares. The following coordinated ground-based observations were arranged in collaboration with the Catania group (M. Rodono) and the Armagh group during the previous year: optical photometry and spectrophotometry, and radio monitoring using the VLA, Arecibo, CSIRO and other radio telescopes. Similar arrangements will be made again; ESA and NASA IUE programs will be coordinated; X-ray observations will be requested in separate proposals to be submitted to the EXOSAT guest investigator program and via possible collaboration with ASTRO-B scientists. We propose to address the following: (1) Can flare line emission be explained by any flare loop models of the sort being developed to interpret SMM solar flares? (2) Can any close empirical analogs be found in SMM observations? (3) How do UV lines evolve during flares? (We have temporal resolution by repositioning the target during a given exposure.) (4) What is the nature of the UV continuum observed previously by IUE during flares? (5) What is the strength of the chromospheric (Mg II) flare? (6) How does the coronal-sensitive He II 1640 A line compare to other UV lines during a flare? How does it evolve? (7) What if; the overall energy balance and budget during a flare? primarily cooled by radiative losses? by conduction of energy to the chromosphere?

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