Biographical Memoirs Volume 72 (1997) / Chapter Skim
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LEO GOLDBERG
LEO GOLDBERG
Pages 114-135
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an important role in founcling the Association of Universities for Research in Astronomy, Kitt Peak National Observatory, en c! the National Radio Astronomy Observatory.
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on a problem of relative multiple strengths in atomic spectra, a serious topic in the interpretation of stellar spectra. His interest in the fielc!
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Hulbert. The observatory was well known for its pioneering photography of transient solar phenomena, primarily prominence ant!
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When Cerro Tololo was establishecI, the Michigan Schmidt was sent there to clo excellent work on the southern skies, especially objective prism spectroscopy with "good seeing." The foresight of Goiciberg en c! his associates pair!
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the directorship, but he cleclinecI. GoIciberg also playact an active role in the American Astronomical Society, as well as the International Astronomical Union, of which he later became president.
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provicle new quarters for the astronomy department. The orbiting solar observatories carrier!
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en c! accept the directorship of Kitt Peak National Observatory.
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be constructive, a point of view that is often woefully lacking in many research proposal evaluations or refereeing of papers at the present time. In the winter of 1966 officials at the National Aeronautics en c!
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become increasingly the responsibility of GoIciberg's younger, giftec! collaborators Andrea Dupree en c!
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the Kitt Peak National Observatory (KPNO) in Arizona en c!
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RESEARCH CONTRIBUTIONS GoIciberg's research contributions began as an unclergracluate student in 1935, when, uncler the inspiration of Menzel, he undertook the calculation of relative multiplet strengths in a transition array. How to calculate relative strengths of lines in a multiplet was aireacly known.
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in the solar spectrum en c! derive the excitation temperature of the solar atmosphere.
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Another important factor emerging for the interpretation of certain lines in the spectra of gaseous nebulae en c! for unclerstancling observations of the solar corona is clielectronic recombination, which enhances the rate at which ions en c!
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The shock tube laboratory, operated by Parkinson and Reeves, produced small volumes of gas momentarily at high temperatures and densities appropriate to astrophysical plasmas. This device makes it possible to measure f-values and identify molecular and atomic lines that can be compared with solar and stellar spectra.
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clic! not imply that mere scientists conic!
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He belongec! to the American Geophysical Union, American Astronomical Society, American Physical Society, Astronomical Society of the Pacific, Optical Society of America, and the Royal Astronomical Society, en c!
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my reach. AM GRATEFUE FOR valuable information and advice supplied by a number of Goldberg's associates, particularly Frank Edmondson, Jesse Greenstein, and Donald Osterbrock.
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Equivalent widths and the reversing layer temperature. Astrophys.
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Carbon monoxide in the ultraviolet solar spectrum. Astrophys.
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Coronal electron density maps for 7 March, 1970, derived from Mg X X625 spectroheliograms.
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