Encyclopedia of Physics Astrophysics-V - download pdf or read online

By Flügge S. (ed.)

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Soc. London 102, 134 (1942). 3 W. W. Campbell: Publ. Astronom. Soc. Pacific 10, 129 (1898). — D. H. Menzel: Publ. Lick Obs. 17, 1 (1931). 2 S. R. R. 36 McMath and O. C. Mohler: Solar Instruments. Sect. 1?. predicted, nearly ideal conditions should occur on an isolated, high mountain peak from an ocean, far from land, within the latitude zone ±35°- The mountain should be high enough to rise above ordinary formations of cumulus clouds. The nearest approaches to such sites are the island of Tenerife 1 and the island of Hawaii 2 but little is known of the solar observing conditions at these sites.

M. A. Ellison 7ieme Rapp. Comm. pour l'etude des relations entre les phenomenes solaires 1 — 2 : 1. Paris: Hemmerle, Petit & Cie. 1951. The Solar System, Vol. P. Kuiper. Chicago: Univ. Chicago Press 1953. * H. S. Jones: Sunspot and Geomagnetic Data derived from Greenwich Observations 1874 — 1954 compiled under the direction of H. S. Jones. M. Stationery Office 1955. 5 F. C. McMath, H. S. Hulbert and R. R. McMath Publ. Obs. Univ. Michigan 4, et terrestres, p. 3 : : 53 (1931). 6 W. O. Roberts: Draft Reports, Internat.

Ft. in area). The panels will adjust the temperature of this structure as required to minimize thermal air currents. The surfaces of the mirror and lenses in a solar telescope present more difficult problems for control than the telescope structure itself. A clean lens transmits and reflects nearly 99% of the total energy of the solar radiation incident on it, and if initially at air temperature requires only slight heating or cooling to follow the diurnal changes. However, no successful scheme for controlling the temperature of a lens has been developed.

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Encyclopedia of Physics Astrophysics-V by Flügge S. (ed.)


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