2008/04/01 by Andrea P. Buccino, A. P. Buccino, P. J. D. Mauas +1 · 1 citation
Physics and Astronomy · Social Sciences · #Astronomical spectroscopy #Astronomy and Astrophysical Research #Educational Leadership and Practices #Emission spectrum #Line (geometry) #Main sequence #Spectral line #Stars #Stellar atmosphere #Stellar, planetary, and galactic studies #Ultraviolet #Ultraviolet astronomy #astro-ph
paper · pdf · doi:10.1051/0004-6361:20078925
10 pages, accepted for publication in Astronomy and Astrophysics
openalex publication_date 2008/04/01 · arxiv created 2008/04/07 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. The largest dataset of stellar activity measurements available at present is the one obtained at the Mount Wilson Observatory, where high-precision H+K fluxes have been measured from 1966 for about 2200 stars. Since the h and k lines at λ2800 Å are formed in a similar way to the H+K emission lines, they are also good indicators of chromospheric structure. The International Ultraviolet Explorer (IUE) provides a large database of UV spectra in the band 1150-3350 Å from 1978 to 1995, which can also be used to study stellar activity.