scholarly journals ‘The Earth but a Satellite of the Sun’

1958 ◽  
Vol 11 (4) ◽  
pp. 409-410
Author(s):  
R. d'E. Atkinson ◽  
E. G. R. Taylor

I Have read Professor Taylor's article with great enjoyment. There are, however, two matters of fact on which, though they do not affect her main thesis, the record should, I think, be set right, (a) The earliest experimental proof of the Earth's revolution round the Sun was neither Bessel's detection of the relative parallax of 61 Cygni, nor Henderson's determination of the absolute parallax of α Centauri (both of which occurred in 1838) but Bradley's very beautiful discovery of aberration in 1725, together with his slightly later explanation. The discovery was made in a deliberate search for parallaxes; and although that particular proof of the Earth's movement was not then achieved, it was at once recognized that aberration provided a different and equally cogent one. Bradley's work was indeed resisted, in some quarters and for a short while, for reasons which Professor Taylor will by no means find unexpected. His later discovery of one term in the nutation was also a discovery of something which would have embarrassed Ptolemy, and delighted Newton; it certainly tended to confirm the picture, if that were needed. By the time parallaxes actually were discovered, though there still were individuals, sometimes of high rank, whose prejudices were stronger than their intellects, the only point of genuine doubt was the question how far away the nearest stars really were.

Among the celestial bodies the sun is certainly the first which should attract our notice. It is a fountain of light that illuminates the world! it is the cause of that heat which main­tains the productive power of nature, and makes the earth a fit habitation for man! it is the central body of the planetary system; and what renders a knowledge of its nature still more interesting to us is, that the numberless stars which compose the universe, appear, by the strictest analogy, to be similar bodies. Their innate light is so intense, that it reaches the eye of the observer from the remotest regions of space, and forcibly claims his notice. Now, if we are convinced that an inquiry into the nature and properties of the sun is highly worthy of our notice, we may also with great satisfaction reflect on the considerable progress that has already been made in our knowledge of this eminent body. It would require a long detail to enumerate all the various discoveries which have been made on this subject; I shall, therefore, content myself with giving only the most capital of them.


1765 ◽  
Vol 55 ◽  
pp. 326-344 ◽  

The observations of the late transit of Venus, though made with all possible care and accuracy, have not enabled us to determine with certainty the real quantity of the sun's parallax; since, by a comparison of the observations made in several parts of the globe, the sun's parallax is not less than 8" 1/2, nor does it seem to exceed 10". From the labours of those gentlemen, who have attempted to deduce this quantity from the theory of gravity, it should seem that the earth performs its annual revolution round the sun at a greater distance than is generally imagined: since Mr. Professor Stewart has determined the sun's parallax to be only 6', 9, and Mr. Mayer, the late celebrated Professor at Gottingen, who hath brought the lunar tables to a degree of perfection almost unexpected, is of opinion that it cannot exceed 8".


2013 ◽  
Vol 40 (1) ◽  
pp. 135-146
Author(s):  
Aleksandar Tomic

Newton's formula for gravity force gives greather force intensity for atraction of the Moon by the Sun than atraction by the Earth. However, central body in lunar (primary) orbit is the Earth. So appeared paradox which were ignored from competent specialist, because the most important problem, determination of lunar orbit, was inmediately solved sufficiently by mathematical ingeniosity - introducing the Sun as dominant body in the three body system by Delaunay, 1860. On this way the lunar orbit paradox were not canceled. Vujicic made a owerview of principles of mechanics in year 1998, in critical consideration. As an example for application of corrected procedure he was obtained gravity law in some different form, which gave possibility to cancel paradox of lunar orbit. The formula of Vujicic, with our small adaptation, content two type of acceleration - related to inertial mass and related to gravity mass. So appears carried information on the origin of the Moon, and paradox cancels.


Author(s):  
L. V. Morrison ◽  
F. R. Stephenson ◽  
C. Y. Hohenkerk ◽  
M. Zawilski

Historical reports of solar eclipses are added to our previous dataset (Stephenson et al. 2016 Proc. R. Soc. A 472 , 20160404 ( doi:10.1098/rspa.2016.0404 )) in order to refine our determination of centennial and longer-term changes since 720 BC in the rate of rotation of the Earth. The revised observed deceleration is −4.59 ± 0.08 × 10 −22  rad s −2 . By comparison the predicted tidal deceleration based on the conservation of angular momentum in the Sun–Earth–Moon system is −6.39 ± 0.03 × 10 −22  rad s −2 . These signify a mean accelerative component of +1.8 ± 0.1 × 10 −22  rad s −2 . There is also evidence of an oscillatory variation in the rate with a period of about 14 centuries.


1859 ◽  
Vol 6 (31) ◽  
pp. 39-49
Author(s):  
J. Stevenson Bushnan

Physiology is co-extensive with organic nature. Organic nature is wholly composed of individuals, comprising the two great kingdoms of plants and animals. A unity of structure pervades the whole of this wide field of nature; and this unity is a great principle, applicable to the determination of truth in the investigation of this part of knowledge. Every individual in organic nature is a system made up of reciprocally dependent and connected parts. The objects of investigation in physiology are phenomena, organs, and principles. The study of phenomena stands first in order; but while it must essentially be first cultivated and advanced, in the ulterior stages of its progress it gains continually fresh additions from the progress made in the knowledge of organs and principles. That phenomena attract attention before organs, is manifest on the slightest consideration. Thus the phenomena of locomotion were familiar to mankind long before the part taken by the muscular flesh in locomotion was discovered. To this moment it is far more certain that absorption takes place throughout the animal body, than what the organs are by which that office is performed. And it would be easy to multiply examples of the same kind, not-withstanding that there are some phenomena of the human body—such as those connected with the sense of sight, the sense of hearing, and other senses—the organs concerned in which must have been known, in a general manner, almost as soon as the earliest phenomena in which they are concerned. Principles, in their larger sense, take their place subsequently to the study of organs; yet, as referring to the more common genera of phenomena, these must also have had their rise almost coeval with the observation of phenomena. Thus the grouping of colours, sounds, smells, and tastes together, under the name of qualities derived from sense, must have been a very early and universal generalization. Nevertheless, it will, I think, be conceded, after these examples, that the study of phenomena is of a more elementary character in physiology, than the study of organs and principles; and, therefore, in the difficult parts of any physiological subject, that more progress is likely to be made by the study of phenomena, than by the study of organs and principles. But before proceeding further, it may be desirable to give some examples of physiological phenomena:—the alternation of sleep and waking; of hunger and satiety; thirst; the effect of drink; breathing; the exercise of the senses, and trains of thought; the various kinds of locomotion, walking, running, leaping, dancing. Here a question naturally arises—if trains of thought be physiological phenomena, does not all human knowledge fall within the definition of physiological phenomena? If the human race were not yet called into being, neither would human knowledge, it is true, have any existence in the world. And, it is doubtless true, under one point of view, that all that man has discovered; all that he has recorded; all the changes which he has made upon the earth since his first creation—are the effects of his physiological nature. But to place all knowledge under the head of physiology would be to defeat the very end of methodical arrangement, to which the progress of knowledge is so largely indebted. Nor is it difficult to mark out at least the general character of the boundaries within which physiology, in the largest sense in which it is convenient to accept it, should be circumscribed. Let us take as an example man's susceptibility of locomotion. It is a sufficient illustration of the physiology of locomotion to point out, that every man without any extraordinary effort learns to walk, run, hop, leap, climb; but there is at least a manifest convenience in separating such more difficult acquisitions as dancing, skating, writing, from the order of physiological phenomena, and placing each in a department by itself, as subject to its own rules. So also it is at least a convenience to consider painting and music as separate departments of study, and not merely as physiological phenomena, falling under the senses of sight and of hearing. It may be supposed to be a matter of the like convenience, to separate from physiology all the phenomena which enter into what are commonly called trains of thought; that is nearly all that comes under the head of psychology, in its most appropriate extent of signification. But several objections will readily occur to such a mutilation of physiology. In particular, it is objectionable, because, as was already hinted, the phenomenal departments of physiology, though the first to take a start, are often much augmented by the subsequent study of the organs concerned; and, more so that, since psychology, disjoined from physiology, and limited to one mode of culture, namely, by reflexion on the subjects of consciousness, were psychology thrown out from physiology, the probable advantages from the study of the organs concerned in the mental processes, and the other modes of culture, admissible in physiological enquiry, would be lost. If it be said that psychology proper rejects all evidence, except the evidence of consciousness, on no other ground, but because of the uncertainty of every other source of evidence—the answer is, that in those sciences which have made most progress, possibility, probability, and moral certainty have always been admitted as sufficient interim grounds for the prosecution of such inquiries as have finally, though at first leading to inexact conclusions, opened the way to the attainment of the most important truths; and that psychology, by the over-rigidness of its rules of investigation, has plainly fallen behind sciences, in advance of which it at one time stood in its progress.


The determination of the expansion of mercury by the absolute or hydrostatic method of balancing two vertical columns maintained at different temperatures does not appear to have been seriously attempted since the time of Regnault (‘Mém. de l’Acad. Roy. des Sci. de l’Institut de France,' tome I., Paris, 1847). His results, though doubtless as perfect as the methods and apparatus available in his time would permit, left a much greater margin of uncertainty than is admissible at the present time in many cases to which they have been applied. The order of uncertainty may be illustrated by comparing the value of the fundamental coefficient of expansion (the mean coefficient between 0° and 100°C.) given by Regnault himself, with the values since deduced from his observations by Wüllner and by Broch. They are as follows:— Regnault . . . . . . 0·00018153. Wüllner . . . . . . 0·00018253. Broch . . . . . . . 0·00018216. The discrepancy amounts to 1 in 180 even at this temperature, and would be equivalent to an uncertainty of about 4 per cent, in the expansion of a glass bulb determined with mercury by the weight thermometer method. The uncertainty of the mean coefficient is naturally greater at higher temperatures. If, in place of the mean coefficient, we take the actual coefficient at any temperature, the various reductions of Regnault’s work are still more discordant, and the rate of variation of the coefficient with temperature, which is nearly as important as the value of the mean coefficient itself in certain physical problems, becomes so uncertain that the discrepancies often exceed the value of the correction sought. It is only fair to Regnault to say that these discrepancies arise to some extent from the various assumptions made in reducing his results, and are not altogether inherent in the observations themselves.


1. Any estimate of the rigidity of the Earth must be based partly on some observations from which a deformation of the Earth’s surface can be inferred, and partly on some hypothesis as to the internal constitution of the Earth. The observations may be concerned with tides of long period, variations of the vertical, variations of latitude, and so on. The hypothesis must relate to the arrangement of the matter as regards density in different parts, and to the state of the parts in respect of solidity, compressibility, and so on. In the simplest hypothesis, the one on which Lord Kelvin’s well-known, estimate was based, the Earth is treated as absolutely incompressible and of uniform density and rigidity. This hypothesis was adopted to simplify the problem, not because it is a true one. No matter is absolutely incompressible, and, the Earth is not a body of uniform density. It cannot be held to be probable that it is a body of uniform rigidity. But when any part of the hypothesis, e. g ., the assumption of uniform density, is discarded, the estimate of rigidity is affected. Different estimates are obtained when different laws of density are assumed. Again, whatever hypothesis we adopt as regards the arrangement of the matter, so long as we consider the Earth to be absolutely incompressible and of uniform rigidity, different estimates of this rigidity are obtained by using observations of different phenomena. Variations of the vertical may give one value, variations of latitude a notably different value. It follows that “the rigidity of the Earth” is not a definite physical constant. But there are two determinate constant numbers related to the methods that have been used for obtaining estimates of the rigidity of the Earth. One of these numbers specifies the amount by which the surface of the Earth yields to forces of the type of the tide-generating attractions of the Sun and Moon. The other number specifies the amount by which the potential of the Earth is altered through the rearrangement of the matter within it when this matter is displaced by the deforming influence of the Sun and Moon. If we adopt the ordinarily-accepted theory of the Figure of the Earth, the so-called theory of “fluid equilibrium,” and if we make the very probable assumption that the physical constants of the matter within the Earth, such as the density or the incompressibility, are nearly uniform over any spherical surface having its centre at the Earth’s centre, we can determine both these numbers without introducing any additional hypothesis as to the law of density or the state of the matter. We shall find, in fact, that observations of variations of latitude lead to a determination of the number related to the inequality of potential, and that, when this number is known, observations of variations of the vertical lead to a determination of the number related to the inequality of figure. [ Note added , December 15, 1908.—This statement needs, perhaps, some additional qualification. It is assumed that, in calculating the two numbers from the two kinds of observations, we may adopt an equilibrium theory of the deformations produced in the Earth by the corresponding forces. If the constitution of the Earth is really such that an equilibrium theory of the effects produced in it by these forces is inadequate, we should expect a marked discordance of phase between the inequality of figure produced and the force producing it. Now Hecker’s observations, cited in § 6 below, show that, in the case of the semidiurnal term in the variation of the vertical due to the lunar deflexion of gravity, the agreement of phase is close. If, however, an equilibrium theory is adequate, as it appears to be, for the semidiurnal corporeal tide, a similar theory must be adequate for the corporeal tides of long period and for the variations of latitude.]


2002 ◽  
Vol 185 ◽  
pp. 472-473 ◽  
Author(s):  
F. Bouchy ◽  
J. Schmitt ◽  
J.-L. Bertaux ◽  
P. Connes

The spectrograph EMILIE (Bouchy et al., 1999; Bouchy, 1999; Bouchy et al., 2000) coupled to the Absolute Astronomical Accelerometer (AAA, Connes, 1985; Schmitt, 1997) and implemented at the 152-cm Coudé telescope of the Observatoire de Haute Provence is dedicated to high-precision Doppler measurements. The AAA method uses a sliding reference spectrum constrained to track the stellar lines and to use the spectrograph as a null-checking device. The goal of AAA is to eliminate the calibration of the spectrograph as well as the displacement of the spectra across the CCD pixels due to the earth motion (and suspected to introduce a systematic error in the RV measurement). Here we report seismological results obtained with AAA on the Sun and the bright stars Procyon and ζ Her A that are expected to present solar-like oscillations.


1952 ◽  
Vol 45 (7) ◽  
pp. 553-555
Author(s):  
Aaron Bakst
Keyword(s):  
The Sun ◽  

Calendar problems have fascinated many a mathematician. Every now and then a formula for the determination of the days of the week or of the Easter date is published. Such formulas are valid for a certain number of years. The reason for such limitations is associated with the fact that the length of the year, that is, the length of the period of the year is not the same. The earth completes one cycle on its orbit around the sun in approximately 365.24220 days.


A little over two hundred years ago a number of serious and learned men in Copenhagen, London, Paris, St Petersbourg, Stockholm and elsewhere, men who were academicians, Fellows of the Royal Society, Lords of the Admiralty, politicians and the like, had been thinking seriously and learnedly about the behaviour of Venus, not, of course, about Venus as represented coldly and chastely by the marble statues being imported from Italy or more warmly in the paintings of Boucher and his contemporaries, but about her far distant planet which was calculated to pass across the disk of the Sun in 1769 and not to make another such transit until 1874. Observations of the 1769 transit at widely separated stations would provide, it was hoped, the means of calculating the distance of the Earth from the Sun. The Royal Society in London, having set up in November 1767 a sub-committee ‘to consider the places proper to observe the coming Transit of Venus’ and other particulars relevant to the same, presented a memorial to King George III outlining possible benefits to science and navigation from observations made in the Pacific Ocean and received in return the promise of £4000 and a suitable ship provided by the Royal Navy (8).


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