8 research outputs found
Endoreduplication Cycles during Hypocotyl Growth of Cabbage (Brassica oleracea L.) under Light and Dark Conditions
The origins and abundances of the chemical elements before 1957: from Prout's hypothesis to Pasadena
The 1957 papers by Burbidge, Burbidge, Fowler, and Hoyle and by Cameron are generally
regarded as the foundations upon which our modern understanding of nucleosynthesis has
been erected. They were, however, also the capstones of an extended period of
investigation of the composition of the cosmos (earth, sun, and beyond) and of the
processes that might have given rise to that composition, dating back at least as far as
1885, that is longer before 1957 than “now” is after 1957
A review of the pharmacology, pharmacokinetics, and regulatory control in the US of local anaesthetics in the horse
The origin and abundances of the chemical elements revisited
The basic scheme of nucleosynthesis (building of heavy elements from light ones) has held up very well since it was first proposed more than 30 years ago by E.M. Burbidge, G.R. Burbidge, A.G.W. Cameron, W.A. Fowler, and F. Hoyle. Significant advances in the intervening years include (a) observations of elemental and a few isotopic ratios in many more extrasolar-system sites, including metal-poor dwarf irregular galaxies, where very little has happened, and supernovae and their remnants, where a great deal has happened, (b) recognition of the early universe as good for making all the elements up to helium, (c) resolution of heavy element burning in stars into separate carbon, neon, oxygen, and silicon burning, with fine tuning of the resulting abundances by explosive nucleosynthesis in outgoing supernova shock waves, (d) clarification of the role of Type I supernovae, (e) concordance between elements produced in short-lived and long-lived stars with those that increased quickly and slowly over the history of the galaxy, and (f) calibration of calculations of the evolution and explosion of massive stars against the detailed observations of SN 1987A. The discussion presupposes a reader (a) with some prior knowledge of astronomy at the level of recognizing what is meant by an A star and an AGB star and (b) with at least a mild interest in how we got to where we currently are. © 1991 Springer-Verlag