Interstellar Matter and Chemical Evolution
- 27 April 1984
- journal article
- research article
- Published by American Association for the Advancement of Science (AAAS) in Science
- Vol. 224 (4647) , 345-350
- https://doi.org/10.1126/science.224.4647.345
Abstract
The determination of chemical abundances of the interstellar medium is related to three different areas of astronomy: pregalactic conditions, stellar evolution, and chemical evolution of galaxies. The observed abundances permit the testing of theories associated with these areas. Knowledge of the abundances of helium, carbon, nitrogen, and neon relative to the abundance of hydrogen in the interstellar medium puts limits on current models of cosmology, stellar evolution, and galactic evolution.Keywords
This publication has 38 references indexed in Scilit:
- The H I absorption in NGC 5128 /Centaurus A/The Astrophysical Journal, 1983
- Constraints on the primordial helium abundance from the optical emission spectra of dwarf galaxiesPhilosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences, 1982
- Abundances of elements of cosmological interestPhilosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences, 1982
- Gradients in the physical conditions of M101 and the pregalactic helium abundanceThe Astrophysical Journal, 1982
- CNO isotopes and galactic chemical evolutionThe Astrophysical Journal, 1982
- The carbon abundance in the Magellanic Clouds from IUE observations of H II regionsThe Astrophysical Journal, 1982
- On the fragmentation of cosmic gas clouds. III - The initial stellar mass functionThe Astrophysical Journal, 1977
- Chemical composition of H II regions in the Small Magellanic Cloud and the pregalactic helium abundanceThe Astrophysical Journal, 1976
- Some Recent Results from Galactic and Stellar Evolution TheoryThe Astrophysical Journal, 1974
- Abundances in Some Population II K Giants.The Astrophysical Journal, 1959