Infrared colour-magnitude diagrams (K vs. J-K) have been obtained for eight intermediate age (˜0.1-1 Gyr) Large Magellanic Cloud (LMC) clusters and one Small Magellanic Cloud (SMC) cluster (NGC 419). The data have been obtained from infrared array camera images taken at the CTIO 1.5m telescope and reduced using the software package ROMAFOT. We believe that we have observed the onset of the extended red giant branch, i.e. the discontinuous change in the infrared colour and in the number of infrared bright stars per unit optical cluster luminosity. The most luminous stars (K = 10-12.5) must be on the asymptotic giant branch; some of them are very red (J - K > 1.5) and must be carbon stars.

We present a preliminary map of the 30-Doradus region at 22 GHz with a HPBW of 4'.6 arc. The results are compared with those from maps at lower frequencies and at similar resolution. Three supernova remnants were detected: N157b, MC 78 and MC 89.

The Large Magellanic Cloud (LMC) HII region N159A is shown to be a group of ionized regions, some of which overlap, rather than a single HII region. There are at least 11 stars earlier than B2 in this region

The ellipticities of the most populous MC star clusters (87) have been derived for studying a) ellipticity variations within individual clusters, b) variations of ellipticity distributions for various galaxies, and c) variations of ellipticity of star clusters relative to their dynamical parameters.

From the studied clusters it is found that radial ellipticity variations within individual clusters seem to be a common phenomenon for the MC clusters where the inner parts are more elliptical than the outer. The SMC clusters are more elliptical than LMC clusters where ellipticities are measured at rh.

The dynamical masses of the clusters seem to correlate with ellipticities where the most massive are the most elliptical.

New observations give more details and some confirmation about the chemical evolution of the Clouds. From more numerous data, information is beginning to emerge about the importance of mixing in the Clouds.

Cepheid variables provide a key to understanding the structure and distance of the Magellanic Clouds, as well as providing accurate reddenings there. Recent major observing programs have continually expanded the data base of photometry and velocities. It is important to try to reconcile the plethora of Cepheid data into a consonant picture of the three-dimensional spatial structure of the Clouds and to compare in a consistent manner the bulk Cloud distance moduli found by several photometric methods.

Until recently, surveys for variable stars in the Magellanic Clouds were carried out in blue and visual passbands, but these passbands are not ideal for finding very cool stars such as long-period variables (LPVs). Consequently, the early surveys generally found only the brightest LPVs in the Magellanic Clouds. The most extensive surveys were the Harvard surveys whose results are summarized by Payne-Gaposhkin and Gaposhkin 1966 (SMC) and Payne-Gaposhkin 1971 (LMC), with some supplementary data in Hodge and Wright (1969) and Wright and Hodge (1971). LPVs were also found during other smaller surveys such as those of Dessy (1959), Butler (1972, 1978) and Lloyd Evans (1971, see also Glass and Lloyd Evans 1981, Lloyd Evans 1978,1985 and Lloyd Evans et al. 1988).

The main characteristics of the luminous blue variables (LBVs) in the MCs with S Dor-type outbursts are reviewed. At quiescence they are luminous OB supergiants occupying an inclined instability strip in the HRD. The most luminous LBVs are the hottest ones. During outburst, dense envelopes are expelled of equivalent spectral-type middle A to early F. LBVs occupy at maximum a vertical strip in the HRD at a temperature of about 8000K. The observed amplitudes in the visual range increase from 1 mag (e.g. R71; T=14500K at quiescence) to 2.5 mag (e.g. R127; T=33000K at quiescence). The existence of an amplitude-luminosity relation is suggested which can be used to derive extragalactic distances, if calibrated with the LBVs of the LMC. Whereas four LBVs are known to be members of the LMC, none is known in the SMC. This could be a consequence of the lower metal abundance in this galaxy.

The most striking feature of the Wolf-Rayet stars in the Magellanic Clouds is their subtype distribution. The range of WC subtypes found in the Large and Small Cloud agrees with evolutionary model predictions at the corresponding metallicities. It follows that the WR subtype distribution in any external galaxy is a clear indicator of the metallicity in that galaxy.

The fluxes in the emission lines of WC stars appear to be consistent within the LMC. This can be used (with some precautions) in the Milky Way and other galaxies to determine reddening, distance and the numbers of WR stars in compact regions.

A reddening of E(B-V) = 0.12 ± 0.02 has been determined for NGC 330 in the Small Magellanic Cloud (SMC) from spectrophotometry of B stars in the cluster. This high reddening helps explain many of the anomalous low metallicity estimates for the cluster. Preliminary analysis of Coudé spectra of K giants in the cluster indicates a high value of 3.5 to 4.5 km s−1 for the micro-turbulence, and a metallicity near −0.7 dex with respect to the sun.

The Magellanic Clouds provide a unique laboratory in which to study the metallicity dependence of stellar winds. If proved by observations, such a dependence would have important consequences for stellar evolution, nucleosynthesis, energy balance of the ISM, star formation and so on. In addition, the diagnostics of emitting gaseous nebulae in metal-poor galaxies would be affected, since the photospheric ionizing radiation of massive hot stars is modified by metal absorption in the surrounding stellar winds (see recent review by Kudritzki et al. 1990). Moreover, the method of using mass-loss rates M and terminal velocities vi, to determine stellar distances, radii and masses (Kudritzki & Hummer 1990) would need further modification.

We report new results on the X-ray binaries in the LMC since IAU Symposium 108 (see review by Hutchings 1984). These include an update of the point source identifications after further optical observations and a reprocessing of the Einstein database. We report major new results on several specific systems. Among low-mass systems (LMXB), we report periods and orbital determinations for LMC X-2 (long period), CAL 83, and CAL 87 (eclipsing black-hole binary). For the high-mass X-ray binaries (MXRB), we announce an ˜ 99 day (precession?) period in LMC X-3 and discuss orbital determinations for LMC X-1 and 0538–66.

The enhanced nitrogen abundances in planetary nebulae (PN) show the effects of CN-cycle processing at the time of the first dredge-up, while their very enhanced carbon abundances show the effects of the third dredge-up. The efficiency of both the first and third dredge-ups increases with decreasing initial metallicity. ON-cycle depletion of oxygen via the second dredge-up does not appear to have been significant in LMC Type I planetary nebulae (those with N/O > 0.5) – these nebulae have experienced the third dredge-up and envelope-burning, giving enhanced C+N abundances. The LMC Type I PN show enhanced Ne/O ratios. Enrichment rates in nitrogen and carbon by PN are estimated for the ISM s of the Magellanic Clouds.

We present a simple two-wind model for the evolution of the Magellanic Cloud planetary nebulae (PN) which reproduces the observed density / radius / ionised mass relationships, and serves to define the geometrical relationship between the ionised nebula and the star. From self-consistent photoionisation modelling of 78 Magellanic Cloud PN, we have constructed the H-R Diagram for the central stars, and have derived both the chemical abundances and the nebular parameters. We find that the central stars have masses generally between 0.55 and 0.7 M⊙. Type I PN have more massive precursors, and show clear evidence for the Third dredge-up episode and for the dredge-up of ON processed material. The expansion velocity of the nebula is closely correlated with the position of the central star on the H-R Diagram, proving that the nebula undergoes continuous acceleration. Excluding Type I PN, the mean abundances derived for the LMC and the SMC agree with those derived from H II regions and evolved, radiative SNR.

RR Lyrae variables are a component of the oldest stellar populations. In the Magellanic Clouds they occur in a few clusters and in the general field. Recent observations have concentrated on obtaining accurate photometry for the cluster variables and the evolved stars of their parent clusters; these data have been used to determine abundances, distances and ages. Results from this work are reviewed.

In the Magellanic Clouds about 60 confirmed supernova remnants (SNRs) or candidates are known. They have been detected by a combination of X-ray, optical and radio observations. Various statistical aspects of these SNRs will be considered including the implied supernova rate, the spatial distribution, the implications of the radio luminosity/diameter distribution for SNR evolution, and the relation to the extended non-thermal emission.

A brief review is presented of results obtained at ESO on dust formation, evolution of line profiles and luminosities, and chemical abundances including the radioactive species. The most recent evolution of the bolometric light curve is discussed.

The Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) have been searched for radio pulsars using the 64-m Parkes radiotelescope. The search has resulted in the discovery of four pulsars. Observed dispersion measures to each suggest that three lie in the Clouds (two in the LMC, one in the SMC) and that the fourth, which was found in the direction of the LMC, is a foreground object belonging to the galactic pulsar population.

Observations of the LMC SNR 0540-693 using the Australia Telescope Compact Array at a wavelength of 6cm show that the remnant consists of a central core coincident with the associated pulsar and a partial ring of about 65 arcsec diameter.