Spectroscopic and Photometric Observations of a Five-Magnitude Flare Event on UV Ceti
Abstract
Flare stars are late-type emission-line main sequence stars which exhibit random and rapid increases in luminosity. All dwarf M stars thus far observed in the blue-visible and near ultraviolet emit Ca II H and K and Mg II h and k arising from their low to midchromospheres, respectively. However, only those with enhanced chromospheric and transition region densities emit Ha (Distinguishing dMe from dM) as well as a host of other optical and ultraviolet emission lines. There are several classes of stars that exhibit flaring behavior and related phenomena similar to solar magnetic activity. UV Ceti is the classic prototype of the flare star. These flare stars are isolated systems characterized by a wide range of flaring properties that include, for example, the frequency of flaring and the total flare energy.
Document Details
- Document Type
- Technical Report
- Publication Date
- May 12, 1992
- Accession Number
- ADA275165
Entities
People
- E. K. Hege
- Erik L. Eason
- M. S. Giampapa
- R. R. Radick
- S. P. Worden
Organizations
- Phillips Laboratory