March 10 to 15, 2002
The International Astronomical Observatories in Chile Workshop
Galactic Star Formation Across the Stellar Mass Spectrum
Venue: La Serena, Chile
Contact: James De Buizer
Address: AURA/CTIO, Casilla 603, La Serena, Chile
E-mail: workshop2002@ctio.noao.edu
Phone: +56 52 205 210
Fax: +56 52 205 212
URL: http://www.ctio.noao.edu/workshop2002/

From the meeting abstract:
Until recently, observation and theory of star formation was focused on low-mass stars. However, there has been increased interest and work in the areas of intermediate and high mass star formation in the recent decade. This work has progressed to the point where we can now begin to create a coherent understanding of star formation across the entire mass spectrum.

Topics to be addressed include:

• Structure and Initial Conditions of the ISM and Molecular Clouds
• Initial Mass Function, Star Formation Rate, and Star Formation Efficiency
• Star Formation Theory and Supporting Observations
  General Star Formation
  Low Mass Star Formation (Turbulence vs. Gravity)
  Intermediate Mass Star Formation
  High Mass Star Formation (Mergers vs. Accretion)
• Disks and Planet Formation around Stars of Increasing Mass
• Energetics (Jets, Winds, Outflows, Infall, Ionizing Radiation)
• Multiplicity of Formation
  Binaries, Multiple Systems, Clusters, and Dynamical Interactions
  Effect of High Mass Stars on Low Mass Star Formation (Proplyds, Eggs, Radiative Implosion)
  
• Future Star Formation Studies at the International Observatories in Chile

June 24 to 28, 2002
Padua Meeting in Honor of Ivan King
New Horizons in Globular Cluster Astronomy
Venue: Padua, Italy
Contact: Giampaolo Piotto
Address: Dipartimento di Astronomia, Universita di Padova, Vicolo dell 'Osservatorio, 2 Padova, Italy, I-35122
Phone: +39-049-827-8223
Fax: +39-049-827-8212
E-mail: piotto@pd.astro.it
URL: http://menhir.pd.astro.it/newhorizons

From the meeting abstract:
The purpose of this meeting is to bring together experts from the full variety of fields of research spanning globular clusters and their stars, to summarize the great developments in both theory and observations which have taken place during the last decade, and to pose and define clearly the new questions and ideas for the decade ahead. Some of the major new data sets would be presented for the first time, along with their interpretation and implications for the future work to be done. The conference is intended to stimulate active discussion and intellectual cross-fertilisation among the different branches of globular cluster research, and to develop or refine scientific strategies for the major ongoing and forthcoming facilities, missions, and surveys, both from the ground (VLT, Gemini, Keck, etc.) and space (HST, SIM, GAIA, etc.).

June 24 to 28, 2002
IAU Symposium 212
A Massive Star Odyssey From Main Sequence to Supernova
Venue: Costa Teguise, Lanzarote, Canary Islands, Spain
Contact: Cesar Esteban
Address: Instituto de Astrofisica de Canarias, La Laguna, Tenerife 38200, Spain
Phone: +34 922 605 261
Fax: +34 922 605 210
E-mail: iau212@ll.iac.es
URL: http://www.iac.es/project/iau212/

From the meeting abstract:
The physics of massive stars has major highlights. During their evolution from the main sequence to the pre-supernova phase they dominate the interstellar radiation field and the enrichment of the interstellar medium with heavy elements. They are progenitors of supernovae, sources of cosmic rays, and provide nucleosynthesis tests. In the last decade the major role of massive starbursts in the evolution of the universe has become evident. Recent years have seen avalanches of new observational results in the field of massive stars and massive starbursts from ground-based, airborne and space observatories, from the Galactic Center to Local Group galaxies and high-z galaxies. Due to their luminosity and spectroscopic features, the consecutive phases of massive stars and starbursts can be observed out to huge distances, and thus be studied at great variety. While rapid observational developments are taking place on both the stellar and extragalactic fronts, also at the theoretical and modelling sides are continuing important developments in stellar atmosphere modelling techniques, galaxy/starburst spectral synthesing and stellar interior modelling. This all calls for a symposium, that will cover the evolutionary phases of massive stars (M > 20 solar masses) from the main sequence to the supernova phase. The key astrophysical themes of the symposium are:

• Atmospheres of massive stars
• Interiors of massive stars
• Location and distribution of massive stars
• Environment of and feedback from massive stars

The symposium will join the flourishing fields of hot luminous stars, dense supersonic stellar winds, hydrodynamics of wind-wind and wind-shell interaction, interstellar matter, high energy astrophysics, evolution of massive stars, and galactic evolution. We will benefit from the importance of IAU Symposia in bringing together specialists in different fields and associated with different IAU Divisions and Commissions. As such, the symposium will be multi-disciplinary in order to provide optimal cross-fertilization.

July 16 to July 20, 2002
Third Euro-Conference
The Evolution of Galaxies. III- From Simple Approaches to Self-consistent Models
Venue: Kiel, Germany
Contact: Gerhard Hensler
Address: Universitat Kiel, Olshausenstr. 40, D-24098 Kiel, Germany
Phone: +49-431-88-04-125
Fax: +49-431-88-04-100
E-mail: hensler@astrophysik.uni-kiel.de
URL: http://www.astrophysik.uni-kiel.de/conferences/eurokiel2002/

From the meeting abstract:
Topics include:

• Analytical approaches to the chemical evolution of galaxies
• The early evolution of galaxies
• The evolution of disk galaxies
• The dwarf galaxy populations
• Large-scale effects on chemical galaxy evolution
• Formation of Galactic centers
• Requirements to observations from models of galaxies

July 28 to August 02, 2002
Ringberg Workshop
The Chemical Evolution of Dwarf Galaxies - Present Status and Perspectives
Venue: Ringberg Castle, Germany
Contact: Eva Grebel
Address: Max-Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Phone: +49 6221 528 225
Fax: +49 6221 528 246
E-mail: grebel@mpia-hd.mpg.de

From the meeting abstract:
This conference will concentrate on processes responsible for chemical evolution in all types of dwarf galaxies. We aim at obtaining a comprehensive picture of the history of chemical enrichment from stars of a range of ages as well as from the ISM. Special emphasis will be placed on identifying common properties and globally valid relationships, on highlighting the differences between the various types of dwarf galaxies, and on the origin of these differences. The latest observational results will be contrasted with predictions from modern theoretical models. Intrinsic evolutionary and externally induced environmental effects will be discussed in depth. Ample time will be devoted to discussing open questions and future directions.

Topics include:

• Nucleosynthesis processes and feedback/mass loss
• Detailed element abundances, isotope ratios, and implications
• The oldest populations and correlations with high-z absorption line studies
• ISM vs. stellar abundances
• The observed age - metallicity evolution
• Abundance gradients, spreads, and degree of chemical inhomogeneity
• Drivers of chemical evolution: Environmental effects vs. intrinsic characteristics

September 3 to 6, 2002
JENAM Workshop
From Observations to Self-Consistent Modelling of the ISM in Galaxies
Venue: Porto, Portugal
Contact: Miguel A. de Avillez
Address: University of Evora, Department of Mathematics, R. Romao Ramalho 59, Evora, Portugal
Phone: +351 266 744 616
Fax: +351 266 744546
E-mail: mavillez@galaxy.lcs.uevora.pt
URL: http://www.sp-astronomia.pt/jenam2002/ws-ism

From the meeting abstract:
Since we are on the verge of studying the ISM in great detail due to immensely improved observational facilities and techniques in all wavelength ranges and similar progress on the computer hard- and software side, a major goal of this symposium will be to stimulate an intense discussion between observers and theoreticians on a self-consistent picture of the ISM. Observers should tell us WHAT we see on ALL scales of the ISM, near and far, and what boundary conditions would be appropriate for realistic models, and theoreticians should point out what assumptions and simplifications their codes need, and WHAT future observations could test their models.

Thus, the symposium will start with sessions on ISM observations: Bubbles, superbubbles, stellar winds, chimneys, galactic fountains, HVCs, X-ray halos, diffuse ionized gas in galaxies, formation of molecular clouds, magnetic fields and the dynamo mechanism in the Galaxy, and turbulence in the ISM. All these subjects are of great importance for the task at hand. Followed on the last day with sessions on the self consistent picture of the ISM where observations that give us information of the self-consistent picture will discussed as well as the numerical modelling and techniques.

September 9 to 13, 2002
Conference to Honour John Dyson
Winds, Bubbles and Explosions
Venue: Pátzcuaro, Michoacán, México
Contact: Jane Arthur
Address: Instituto de Astronomia, UNAM, Morelia, Michoacan, Mexico
Phone: +52 443 3222750
Fax: +52 443 322726
E-mail: bubbles@astrosmo.unma.mx
URL: http://www.astrosmo.unam.mx/~bubbles

From the meeting abstract:
This meeting will discuss the dynamical effects that mass loss and radiation from astrophysical objects have on their environment in the light of new observational results and theoretical models. The topics of the meeting are:

• Low Mass Stars - Formation, Outflows, Jets
• High Mass Stars - Formation, Ionization Fronts, Stellar Winds, Shocks
• Post Main Sequence Winds (Planetary Nebulae, WR stars, LBV)
• Supernovae and their Remnants
• Line Forming Regions of AGN
• Starburst Superwinds

September 10 to 14, 2002
CNO in the Universe
Venue: St-Luc (Valais, Switzerland)
Contact: Georges Meynet
Address: Geneva Observatory, 51, Ch. Des Maillettes, 1290 Sauverny, Switzerland
E-mail: cnoloc@obs.unige.ch
URL: http://obswww.unige.ch/cno

From the meeting abstract:
Carbon, nitrogen and oxygen share a special place among the chemical elements. Oxygen represents about half of the mass fraction of the heavy elements in the solar neighbourhood. Produced by massive stars, the evolution of its abundance as a function of time is related to the star formation activity. Carbon, which is an essential ingredient of the building blocks of life, is produced by both massive and intermediate mass stars in proportions which still remain to be determined. Nitrogen, long considered to be a purely secondary element and produced mainly by intermediate mass stars, probably has a more complicated nucleosynthesis history in which massive and AGB stars play a role.

Many observational and theoretical results have modified our view of CNO abundances in the universe. The opening of new observational facilities as the VLT and the HST has extended the horizon for detailed abundance determinations, providing unique probes of high-redshift star formation and galaxy evolution. There is now growing evidence that many QSO environments have roughly solar or higher metallicities out to redshifts > 4. Observations of DLA systems provide direct measurements of the chemical enrichment history of the neutral gas in the early universe.

The important question is: how should we interpret these observations? What do they tell us about the nature of the galaxies in the young universe and about their star formation activity? A prerequisite to the interpretation of the observations of CNO abundances in high redshift regions is the confrontation of the theoretical predictions with well observed features in our nearby universe. The observed CNO abundances at the surface of stars in galaxies of the Local Group provide strong constraints on stellar evolution models in different environments. In the same way, abundance gradients in galaxies are cornerstones for galactic chemical evolution models.

NOvember 11 to 15, 2002
IAU Symposium 215
Stellar Rotation
Venue: Cancún, Yucatan, Mexico
Contact: André Maeder
Address: Geneva Observatory, Chemin des Maillettes, 51, CH-1290 Sauverny, Switzerland
Phone: +52-4 732 9607
Fax: +52-4 732 0253
E-mail: andre.maeder@obs.unige.ch
URL: http://www.astro.ugto.mx/~eenens/iau215

From the meeting abstract:
The last years have seen new observations of rotational velocities in solar types stars, in red giants, in intermediate and massive stars, which put new constraints on the evolution of the angular momentum. Anomalies of chemical abundances also constrain the effects of rotation, these are: the Li abundances in low mass stars, the CNO anomalies in red giants, in OB stars and in A- and B-supergiants. Some recent observations in the Galaxy, the LMC and SMC suggest possible differences of v sini and of the related N/C excesses between galaxies. For the Sun, the results on the constancy of the angular velocity in the interior and on the thickness of the tachocline offer major constraints on the hydrodynamics of rotation. The velocities of rotation in binaries are a test of the tidal interaction and of the synchronisation mechanisms. Last but not least, the asymmetric nebulae around Luminous Blue Variables, WR and Be stars, and around planetary nebulae are also signatures of rotational effects and mass loss in these advanced stages.

On the theoretical side, there are new hydrodynamical studies of the various rotational instabilities and of the meridional circulation. There are 2D- and 3D-hydrodynamic simulations, new studies of the synchronisation in binaries and of the interaction between rotation, mass loss, convection and magnetic chromospheric coupling. New models of the evolution of rotating stars are currently being calculated by several groups for low and high mass stars from the MS to the final stages.(We do not intend to cover the theory of star formation and pre-MS evolution because it is a whole subject in itself). The many broad consequences of stellar rotation will be analysed: for the age determinations, the star populations, the chemical yields at low and high metallicities, the nature of the supernovae and the rotation periods of pulsars.

The meeting information on this page is in part taken from Liz Bryson's excellent compilation on International Astronomy Meetings and supplemented by information obtained from the webpages of the meetings.

Last update: December 8, 2001.
mcnews@astro.uiuc.edu