Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.6004l&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #60.04; Bulletin of the American Astronomical Society, Vol. 24, p.825
Astronomy and Astrophysics
Astronomy
Scientific paper
The study of stellar radio emission provides information on the physical processes occuring in, and the physical properties of, stellar coronae. This knowledge helps us to better understand the nature of solar-like activity and the coronal structure of active stars, and their dependence on physical properties such as mass, angular velocity, and age. I present from my thesis observations of young solar-like stars using, for the first time, the newly commissioned Australia Telescope Compact Array. Some of the highlights of these observations are: (i) the discovery of rotational modulation of stellar radio emission, observed on the young ( ~ 50 million yrs) and rapidly-rotating ( ~ 12.4 hrs) K1 dwarf star AB Doradus. This observation provides the first evidence that the radio emission of late-type dwarf stars, like that of the Sun, originates from regions of strong coronal magnetic fields which are associated with starspots; (ii) the discovery of remarkably intense quiescent and flaring radio emission from the young ( ~ 50 million yrs) and rapidly-rotating (<= 9 hrs) dM4e star Rositter 137B. This observation suggests that the radio emission of pre-main-sequence flare stars is much more luminous that that of older solar-neighbourhood flare stars; (iii) the first high-sensitivity radio observation of the dM5e flare star Proxima Centauri, the closest star to the Sun. The result of this observation is in conflict with the currently popular picture that the entire surface of highly-active flare stars is covered by strong (a few kG) coronal magnetic fields containing hot X-ray emitting plasma.
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