The Physics of Star Cluster Formation and Evolution

© 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00689-4.Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.Peer reviewe

A proposal for the nomenclature of Venturia inaequalis races.

The Venturia inaequalis-Malus pathosystem was one of the first for which gene-for-gene relationships were demonstrated following the discovery of such relationships between Melampsora lini and flax by Flor in the 1950s. An understanding of these relationships forms the basis for monitoring pathotypes of V. inaequalis at the population level and is employed to assess the usefulness of resistance genes for breeding durable resistance to scab. These pathotypes are difficult to accommodate in the current system of nomenclature for V. inaequalis races where each new combination of avirulence alleles is assigned a simple numerical descriptor as its name. We propose a system that is better suited to the increasing complexities of combinations of genes involved in both race-specific and race-nonspecific recognition by the host, while at the same time updating the name of scab resistance loci (Rvik) and QTL loci (Qvik) to international standards. For the race-specific interactions, the basic premise is that each Rvik-AvrRvik and Qvik-AvrQvik relationship should be represented by a differential host (k), abbreviated to h(k), carrying only the specific Rvik or (major) Qvik resistance allele and an isolate of the pathogen having lost only the complementary allele at the AvrRvik or AvrQvik locus, race (k), with k representing the number of the specific interaction. Races lacking more than one avirulence gene at different loci will be identified as race (k,l,m,\u2026) and apple hosts carrying multiple scab resistance genes as host (k,l,m,\u2026). The proposed system has some continuity with the current system, but should simplify the presentation and interpretation of studies on avirulence alleles in V. inaequalis at the population level. Gene-for-gene relationships reported to date for this pathosystem are reviewed, some inconsistencies clarified, and several new interactions added. The gene-for-gene relationships of European isolates collected in the last decade have been studied in order to establish a new set of reference isolates that represent various V. inaequalis races