Discovery and Measurement of Double Stars by Lunar Occultations

1965 ◽  
Vol 5 ◽  
pp. 28-37
Author(s):  
R. Edward Nather ◽  
David S. Evans

When a star is occulted by the dark limb of the Moon its apparent intensity drops to zero very quickly. MacMahon (1909) proposed that the time of disappearance would measure the diameter of the star, but Eddington (1909) demonstrated that diffraction effects at the lunar limb would lengthen the apparent time of disappearance to about 20 msec, and suggested that these effects would greatly limit the usefulness of the technique. MacMahon’s paper indicates that he was aware that stellar duplicity could be detected from occultation observations, but he did not amplify the point and Eddington did not comment on it. While it has been demonstrated theoretically by Williams (1939) and experimentally by Whitford (1939) and others that stellar diameters of a few arcmsec can be measured by this technique, its use for the discovery and measurement of double stars has been only incidental to other programs (O’Keefe and Anderson, 1952; Evanset al., 1954). Properly exploited, the method can contribute materially to the study of double stars.

1971 ◽  
Vol 2 ◽  
pp. 688-691
Author(s):  
Nathaniel M. White

A program for the measurement of diffraction patterns resulting from the lunar occultations of stars was begun at the Lowell Observatory by Rakos (1964), resumed by him in 1967 and continued by Pettauer through the summer of 1969. The expected results were accurate timing of occultations and hence accurate position measurements, the discovery of close double stars, and the determination of stellar diameters. The author is continuing the program using new equipment designed by R. E. Nather of the University of Texas.The equipment was built at the Lowell Observatory and put into operation on its new 42-in. reflector in March, 1970.


1971 ◽  
Vol 5 ◽  
pp. 28-37
Author(s):  
R. Edward Nather ◽  
David S. Evans

When a star is occulted by the dark limb of the Moon its apparent intensity drops to zero very quickly. MacMahon (1909) proposed that the time of disappearance would measure the diameter of the star, but Eddington (1909) demonstrated that diffraction effects at the lunar limb would lengthen the apparent time of disappearance to about 20 msec, and suggested that these effects would greatly limit the usefulness of the technique.


1868 ◽  
Vol 16 ◽  
pp. 159-161

My dear Friend,— As you express a wish to know my recent impressions respecting the great telescope, I can say that they are very satisfac­tory. When I saw it six weeks ago the first of the two great specula was just polished; and though the essential parts of the equatoreal were in position, and one could estimate the facility with which it could be managed, the optical part of the telescope remained incomplete. Now, I found the great and small specula in their places, a finder of four inches aperture at­tached, the circles divided, and the clock for driving the telescope en­shrined in the pier. One thing was wanting, weather fit for trying its power; and during eighteen nights there was only one of even middling goodness. That, however, was sufficient to prove that the instrument is thoroughly up to its intended work. I examined several nebulae and clusters, with whose appearance in Lord Rosse’s six-feet reflector I am familial, and the difference was far less than I expected. I may specify among them 51 Messier, whose spirals were seen on strong aurora, and the nebula in Aquarius, with its appendages like the ring of Saturn. Its defi­nition of stars is very good: a Lyræ had as small and sharp an image as I ever saw on such a night; and a few pretty close double stars were well and clearly separated. Part of this is probably due to the lattice-tube, which permits the escape of heated air, but more to the figure of the spe­culum, which is truly parabolic. The peculiar nature of the mounting brings the circles completely within reach of the observer s assistant; and the mechanical appliances for the motions in right ascension and polar distance are so perfect, that we set the instrument on the faint objects winch; we were examining with great facility and rapidity. One man can reverse the telescope in a minute and a quarter; the quick motion in polar distance is of course far easier, and the slow one acts more like the tangent screw of a circle than the mover of such a huge mass. The clock is rather gigantic, but does its work with great precision, the objects which I examined re­maining steady on the wire as long as I watched them; and there is at ingenious and new contrivance for suiting its speed to planets or the moon, There remain but a few matters to be completed; the second great specu­lum is nearly polished, the glass small one is ready; the micrometer and observing-chair are not commenced, nor the photographic apparatus and spectroscope. These two last are no part of Mr. Grubb’s contract; but the Committee thought themselves justified by the correspondence in order­ing them, as their cost is small, and they will add greatly to the utility oi the telescope. In. the fine sky of Melbourne it will, I trust, yield spectroscopic results surpassing any that have as vet been obtained. That it will realize fully the expectations of the people whose enlightened liberality has ordered its construction I am quite certain; but I am not so certain that it will retain its present perfection very long if exposed without some shelter. It is true that Mr. Cooper’s great achromatic has stood exposed to the rain and wind of Connaught for more than thirty years, and is still serviceable; but besides its inferior size it is of coarser workmanship, and is provided with fewer of those beautiful contrivances which in this instru­ment make its movements so easy. At Melbourne the rain of Markree is not to be feared; but if one may judge from its position on the verge of a great continent, and from the analogy of India and the Cape, another enemy is to he dreaded, the fine dust which winds from the interior will probably bring. This would find its way into all the bearings, and besides logging their action would grind them out of truth. The danger of this induces me, after careful discussion with Messrs. Le Sueur and the two Grubbs, n lay before you my views, which (if you think them sound) you may hold it advisable to mention to the authorities of Victoria. Three modes occur to me of covering the telescope. In any case it must be surrounded by a wall, for the comfort of the observer and to prevent in­ trusion. This wall may support a moveable covering of such a kind as let the instrument be pointed to every part of the sky.


1924 ◽  
Vol 61 (1) ◽  
pp. 31-34
Author(s):  
W. H. Pickering
Keyword(s):  
The Moon ◽  

Since this subject is now again under discussion by geologists, it may be of interest to recall that in my original paper, published in the American Journal of Geology, 1907, vol. xv, p. 23, and republished and revised in Harper's Monthly, 1907, vol. cxv, p. 120, and in the Scottish Geographical Magazine, 1907, p. 523, this separation was attributed to the great convulsion that occurred at the time of the birth of the Moon, from the side of the Earth. This explanation of the origin of our Moon is at the present time almost universally accepted by astronomers. We see the same phenomenon occurring in many close double stars.


1965 ◽  
Vol 5 ◽  
pp. 13-19
Author(s):  
W. S. Finsen

If we may judge by the number of eulogistic review articles to which it gave rise, one of the main talking points among astronomers in the early nineteen-twenties was undoubtedly the application of the interferometer to optical astronomy. It was only natural that interest was focused mainly on the brilliant success of Michelson and Pease (1921) in measuring stellar diameters with the 20-ft beam interferometer on the 100-in Mount Wilson reflector. But almost equally exciting, to the double-star observer at least, was the success of Anderson (1920) and Merrill (1922) in resolving several very close double stars, notably Capella, also with the 100-in but with much simpler equipment. Perhaps the most courageous venture of all was the attempt made by Pease (1925) to measure the spectroscopic binary Mizar Aa as a visual double star with a separation of the order of only O’.’Ol. This he did by estimating the fringe visibility with the 20-ft beam oriented in four different position angles – a more exacting and tedious operation it would be difficult to imagine. However sceptical one may be regarding the reliability of so delicate a technique, Russell’s (1927) orbit based on these observations still has a place in our catalogues if only as a monument to a daring experiment.


1966 ◽  
Vol 25 ◽  
pp. 373
Author(s):  
Y. Kozai

The motion of an artificial satellite around the Moon is much more complicated than that around the Earth, since the shape of the Moon is a triaxial ellipsoid and the effect of the Earth on the motion is very important even for a very close satellite.The differential equations of motion of the satellite are written in canonical form of three degrees of freedom with time depending Hamiltonian. By eliminating short-periodic terms depending on the mean longitude of the satellite and by assuming that the Earth is moving on the lunar equator, however, the equations are reduced to those of two degrees of freedom with an energy integral.Since the mean motion of the Earth around the Moon is more rapid than the secular motion of the argument of pericentre of the satellite by a factor of one order, the terms depending on the longitude of the Earth can be eliminated, and the degree of freedom is reduced to one.Then the motion can be discussed by drawing equi-energy curves in two-dimensional space. According to these figures satellites with high inclination have large possibilities of falling down to the lunar surface even if the initial eccentricities are very small.The principal properties of the motion are not changed even if plausible values ofJ3andJ4of the Moon are included.This paper has been published in Publ. astr. Soc.Japan15, 301, 1963.


1962 ◽  
Vol 14 ◽  
pp. 441-444 ◽  
Author(s):  
J. E. Geake ◽  
H. Lipson ◽  
M. D. Lumb

Work has recently begun in the Physics Department of the Manchester College of Science and Technology on an attempt to simulate lunar luminescence in the laboratory. This programme is running parallel with that of our colleagues in the Manchester University Astronomy Department, who are making observations of the luminescent spectrum of the Moon itself. Our instruments are as yet only partly completed, but we will describe briefly what they are to consist of, in the hope that we may benefit from the comments of others in the same field, and arrange to co-ordinate our work with theirs.


1962 ◽  
Vol 14 ◽  
pp. 415-418
Author(s):  
K. P. Stanyukovich ◽  
V. A. Bronshten

The phenomena accompanying the impact of large meteorites on the surface of the Moon or of the Earth can be examined on the basis of the theory of explosive phenomena if we assume that, instead of an exploding meteorite moving inside the rock, we have an explosive charge (equivalent in energy), situated at a certain distance under the surface.


1962 ◽  
Vol 14 ◽  
pp. 149-155 ◽  
Author(s):  
E. L. Ruskol

The difference between average densities of the Moon and Earth was interpreted in the preceding report by Professor H. Urey as indicating a difference in their chemical composition. Therefore, Urey assumes the Moon's formation to have taken place far away from the Earth, under conditions differing substantially from the conditions of Earth's formation. In such a case, the Earth should have captured the Moon. As is admitted by Professor Urey himself, such a capture is a very improbable event. In addition, an assumption that the “lunar” dimensions were representative of protoplanetary bodies in the entire solar system encounters great difficulties.


Sign in / Sign up

Export Citation Format

Share Document