¹ Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH41 1LD. UK
² Landessternwarte Königstuhl, D-69117 Heidelberg, Germany

Recent results on classical Be stars are reviewed and links to general astrophysics are presented. Classical Be stars are B type stars close to the main sequence which exhibit line emission over the photospheric spectrum. The excess is attributed to a circumstellar gaseous component which is commonly accepted to be in the form of an equatorial disc. Since 1988, when the last such review was published, major progress has been made. The geometry and kinematics of the circumstellar environment can be best explained by a rotationally supported relatively thin disc with very little outflow, consistent with interferometric observations. The presence of short-term periodic variability is restricted to the earlier type Be stars. This variation for at least some of these objects have been shown to be due to nonradial pulsation. For at least one star, evidence for a magnetic field has been observed. The mechanisms responsible for the production and dynamics of the circumstellar gas are still not constrained. Observations of nonradial pulsation beating phenomena connected to outbursts point towards a relevance of pulsation, but this mechanism cannot be generalized. Either the evidence that Be stars do not form a homogeneous group with respect to disc formation is growing, or the short-term periodic variability is less important than previously thought. The statistics of Be stars investigated in open clusters of the Milky Way and the Magellanic Clouds have re-opened the question of the evolutionary status of Be stars. The central B star is a fast rotator, although theoretical developments have revived the question of how high rotational rates are, so that the commonly quoted mean value of about 70 to 80% of the critical velocity may just be a lower limit. Be stars are in an unique position to make contributions to several important branches of stellar physics e.g. asymmetric mass-loss processes, stellar angular momentum distribution evolution, astroseismology, and magnetic field evolution.

Review in PASP October 2003 issue (Vol. 115, No. 812, Page 1153)
Available on the web at http://www.journals.uchicago.edu/cgi-bin/resolve?PASP203118