We describe several aspects of the variability of bright pulsating red giant (PRG) stars, with emphasis on the determination of pulsation modes and pulsation masses by using observed multiperiodicity and pulsation constants (Q- values). Our studies of bright PRGs provide a model for the analysis and interpretation of the thousands of PRGs being discovered in surveys of Local Group galaxies.

We have (1) accumulated long-term (up to 15 years) photoelectric photometry of 76 bright pulsating red giants (PRGs) and related stars, with V amplitudes of 0.04 to ≥ 1 magnitude; (2) used a variety of techniques, including autocorrelation, to determine both “short” radial pulsation periods, and long secondary periods; (3) determined pulsation modes using the Q-value method; the modes range from fundamental to second overtone, independent of temperature; (4) tested wavelet analysis on small-amplitude PRGs; (5) made a special study of PRGs with amplitudes less than 0.1 magnitude; and (6) called further attention to the problem of the long secondary periods of these stars. Our studies provide a “model” for the analysis and interpretation of larger, fainter surveys such as MACHO and OGLE.

The analysis of high S/N spectra and photometric data of 60 Cyg shows that: (1) Pronounced long-term variations in spectra are accompanied with light variations. (2) The medium-term variations of RV could indicate that 60 Cyg is a spectroscopic binary. (3) Two independent structures dominate the rapid variability of both spectrum and light of the star.

Let us begin by defining “amateur astronomer”. According to a dictionary, an amateur astronomer is “someone who loves astronomy, and cultivates it as a hobby”. At IAU colloquium 98 (The Contributions of Amateurs to Astronomy), Williams (1988) discussed this issue at length. He proposed that, to be an amateur astronomer, one must be an astronomer - able to do astronomy with some degree of skill; he then defined an amateur astronomer as “someone who carries out astronomy with a high degree of skill, but not for pay”.

We briefly discuss the methods of observing stellar evolution in real time, and of interpreting these observations. Then we discuss recent results on RR Lyrae stars, Population I and II Cepheids, RV Tauri stars, and related objects.

The B type star 53 Persei was discovered in 1977 by Smith (1977) as the prototype of a separate group of B-type variables showing light and line profile variability. The physical cause of the variability was thought to be nonradial pulsation (NRP) (see, e.g. Smith et al. 1984). However, the NRP model for this star has been questioned by Balona (1986) who suggested the rotational modulation (RM) model to explain the variability. In order to resolve the long lasting debate about 53 Persei, a campaign was initiated to organize coordinated optical photometry and spectroscopy from the ground, and Far-UV photometry from Voyager in 1991 January. This paper presents the results of period analysis on the groundbased UBV data. In another paper, Smith & Huang (1994) report the new identification of pulsation modes using Voyager Far-UV photometry combined with the results from optical observations. Some preliminary results from APT uvby observations taken at a single site are also cited for comparison.

The President is happy to report that a considerable increase of interest in astronomy teaching problems seems to have taken place in many countries during the period 1985-1987. Some countries organized local teachers courses and meetinge, other - national conferences devoted to establishing modern school programmes and training teachers methods including astronomical notions. An international workshop for physics teachers showing possibilities of practical introducing astronomy when teaching physics / GIREP 1986/ brought into contact astronomers and physicists. And, last but not least, teaching problems have been also introduced during the IAU Colloquium No.98, “The Contribution of Amateur Astronomers to Astronomy”, in 1987, while the first IAU meeting dedicated to teaching probleme - the IAU Colloquium No.105 “The Teaching of Astronomy” -is planned for 1988 in Williams town /USA/. Let us hope that in the near future all astronomers will be well aware of their own responsibility in helping astronomical education all over the world.

Basic information about the star o and (HR 8762, HD 217675-6) is a bright (V=3.55m, B-V=-0.11m U-B=-0.50m) B6 III-Ve star. Its emission-line and shell spectrum is known to come and go on a time scale of years. In fact, the presence of a strong shell spectrum misled the authors of the HD catalogue to assign the star two HD numbers.

o and is a prototype of Be rapid light variables in the sense that it has the longest record of photoelectric monitoring which goes back to 1915! The long history of attempts to understand the variations of this star has recently been summarized by Harmanec (1983). Collecting and analyzing all historical photoelectric observations, Harmanec (1984) concluded that the light variations of o And can be understood as a superposition of a long-term cyclic (8.5y) variation with an amplitude over 0.1m (the star being faintest at the recorded shell maxima) and a rapid periodic variation with a period of 1.571272 days.