Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ap%26ss.273..225s&link_type=abstract
Astrophysics and Space Science, v. 273, Issue 1/4, p. 225-232 (2000).
Astronomy and Astrophysics
Astrophysics
Scientific paper
Active hot stars (Be stars) have been observed and studied for more than two decades. They exhibit hydrogen emission lines in the visible domain and often some emission lines of singly ionized metals. These emissions originate in a circumstellar envelope produced by a strong radiative stellar wind. Since the discovery of the prototype star of this class (γ Cas) by Father A. Secchi in 1866, the basic physical properties of these objects are still poorly known. These stars are also very bright (most of them can be found in the Bright Star Catalogue) which make them good targets for small telescopes studies. In the following I will focus on some studies that can be done using a 40 cm telescope class. Then I will explain how small telescopes can be combined in an interferometric network in order to reach one milliarcsecond (mas) angular resolution even if each telescope's aperture can be smaller than ten centimeters. With this technics it becomes possible to measure very small and faint structures on the stellar surface of stars other than our sun.
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