Project description:The current paper represents the fourth contribution in the Genera of Fungi series, linking type species of fungal genera to their morphology and DNA sequence data. The present paper focuses on two genera of microfungi, Camarosporium and Dothiora, which are respectively epi- and neotypified. The genus Camarosporium is typified by C. quaternatum, which has a karstenula-like sexual morph, and phoma-like synasexual morph. Furthermore, Camarosporomyces, Foliophoma and Hazslinszkyomyces are introduced as new camarosporium-like genera, while Querciphoma is introduced as a new phoma-like genus. Libertasomycetaceae is introduced as a new family to accommodate Libertasomyces and Neoplatysporoides. Dothiora, which is typified by D. pyrenophora, is shown to produce dothichiza- and hormonema-like synasexual morphs in culture, and D. cactacearum is introduced as a new species. In addition to their typification, ex-type cultures have been deposited in the Westerdijk Fungal Biodiversity Institute (CBS Culture Collection), and species-specific DNA barcodes in GenBank. Authors interested in contributing accounts of individual genera to larger multi-authored papers in this series should contact the associate editors listed on the List of Protected Generic Names for Fungi.
Project description:Advances in our understanding of terrestrial planet formation have come from a multidisciplinary approach. Studies of the ages and compositions of primitive meteorites with compositions similar to the Sun have helped to constrain the nature of the building blocks of planets. This information helps to guide numerical models for the three stages of planet formation from dust to planetesimals (~10(6) y), followed by planetesimals to embryos (lunar to Mars-sized objects; few 10(6) y), and finally embryos to planets (10(7)-10(8) y). Defining the role of turbulence in the early nebula is a key to understanding the growth of solids larger than meter size. The initiation of runaway growth of embryos from planetesimals ultimately leads to the growth of large terrestrial planets via large impacts. Dynamical models can produce inner Solar System configurations that closely resemble our Solar System, especially when the orbital effects of large planets (Jupiter and Saturn) and damping mechanisms, such as gas drag, are included. Experimental studies of terrestrial planet interiors provide additional constraints on the conditions of differentiation and, therefore, origin. A more complete understanding of terrestrial planet formation might be possible via a combination of chemical and physical modeling, as well as obtaining samples and new geophysical data from other planets (Venus, Mars, or Mercury) and asteroids.