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Biographical Memoirs Volume 60 (1991) / Chapter Skim
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10. Donald Howard Menzel
Pages 148-167

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From page 149...
... He was the first to establish the physical characteristics of the solar chromospheres and he initiated the modern era of investigations of physical processes in gaseous nebulae. Although primarily a theorist, he organized and conclucted more than a clozen solar-eclipse expeditions and established two major solar observatories in the western United States.
From page 150...
... proceeds in a partnership in Leadville's largest general store, and the family's financial condition improved markedly. Young Donald displayed a remarkable ability as a "quick study." By age five he was reading Gulliver's Travels, and even before that his father had taught him to send and receive simple messages in Morse code.
From page 151...
... He and his pals performed many experiments with this expanclecl laboratory, some prompted by icleas gained from the library chemistry books he read so voraciously, others inspired simply by the urge to mix chemicals and see what happened. Although some of this involved the clevelopment and manufacture of explosives, good fortune prevailecI, and there were no disasters.
From page 152...
... Fortunately for astronomy, he decided to go to Princeton. WIDE NEW HORIZONS AT PRINCETON Menzel continued to observe variable stars for Professor Dugan as a means of support, but he was most enthusiastic about the lectures of Professor Henry Norris Russell.
From page 153...
... As his thesis for his Ph.D., Menze} sought to establish a stellar temperature scale by applying the Fowler-MiIne theory basect on application of the Saha equation to stellar spectra. HarIow Shapley employed him at Harvard as a research assistant cluring the summers of 1922, 1923, ant]
From page 154...
... He was eager to apply the new clevelopments in atomic physics to the interpretation of astronomical spectra but soon found that the promise of theoretical astrophysics was not at all appreciated by Lick's conservative astronomers. His principal task was to take spectrograms for radial velocity measurements.
From page 155...
... After several years of hard labor, he published his results in a large volume that has become a classic in theoretical astrophysics as one of the earliest examples of quantitative astronomical spectroscopy. He found the temperature of the solar chromosphere to be about 4700°K, but the emission lines of H
From page 156...
... maintained his interest in the solar chromosphere and used spectra from the 1932 Lick Observatory expedition to Fryeburg, Maine, for pioneering investigations of departures in the solar atmosphere from local thermodynamic equilibrium. In the Soviet Union he and MIT's J
From page 157...
... In 1937 this study inspired him to initiate, in collaboration with a number of other physicists and astrophysicists, a series of eighteen papers on physical processes in the highly ionized plasmas of gaseous nebulae. Their work on the solar chromosphere and gaseous nebulae was the first realistic investigation of nonequilibrium conditions in celestial plasmas and represented a major advance in the level of sophistication in the analysis of astronomical spectra.
From page 158...
... By the time Roberts gave up the leadership of the High Altitude Observatory to become the first director of the National Center for Atmospheric Research in Boulder, HAO had become one of the worId's leading centers for solar coronal research. Within the space of eight years, while the country was in deep financial depression and the government provided no financial support, astronomers uncler Menzel's guidance did grouncl-breaking theoretical research in atomic and solar physics and on gaseous nebulae, conclucted an ambitious eclipse expedition, founded the first coronagraphic observatory in the western hemisphere, and established a school of theoretical astrophysics.
From page 159...
... liberal doses of atomic physics and quantum mechanics, subjects in which graduate students of that era were often ill-preparecI. It also must be remembered that in 1934, though theoretical astrophysics thanks to such luminaries as Eddington, Jeans, MiIne, McCrea, Stromgren, Pannekoek, Minnaert, Unsold, and Rosselanc]
From page 160...
... Navy. He was assigned to the Office of the Chief of Naval Communications as an expert on wave propagation, for which his previous training in solar physics, mathematics, cryptanalysts, and shortwave radio macIe him uniquely qualifiecI.
From page 161...
... showed how solar observations could be used to anticipate profound changes in radio communication conditions and to dictate appropriate changes in radio frequencies. Foreseeing the need for an agency that could provide similar services after the war, he played a leading part in establishing the Central Radio Propagation I.aboratory of the National Bureau of Standards, now located in Boulder, Colorado.
From page 162...
... Bok in the acquisition of a sixtyfoot radio telescope and participated in efforts that eventually led to the establishment of the National Radio Astronomical Observatory. During the 1 960s Menzel's activity was slowed by a serious circulatory problem, but he continued to work as his strength permitted.
From page 163...
... Among his diversions while he was a student at Princeton was writing contributions for the magazine, Science and Invention, and science fiction articles under a variety of pseudonyms. In addition, he found time to win the chess championship of Princeton and to participate in several Ivy League matches.
From page 164...
... He was an inspiration to his students, who enjoyed all the benefit of his sound physical insights and technical expertise. Many astrophysicists practicing in the United States today do not realize how much of what they learn originated with Menzel, whose tradition carries on through his many and devotee!
From page 165...
... Multiplet strengths for transitions involving equivalent electrons. Astrophys.
From page 166...
... XIII. The electron temperatures of some typical planetary nebulae.
From page 167...
... The thermodynamic state of the outer solar atmosphere.


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