For correcting the Apparent Distance of the Moon from the Sun or a Fixed Star

Author(s):  
Nevil Maskelyne
Keyword(s):  
The Sun ◽  
1788 ◽  
Vol 1 (2) ◽  
pp. 191-199
Author(s):  
Thomas Elliot

ProblemHaving the apparent distance of the Moon's centre from a fixed Star, or from the centre of the Sun, together with the apparent altitudes of their centres, to find the true distance.SolutionThe difference between the apparent and true altitudes, and the angles which the Moon and Star make with the zenith and each other, must be known before the several corrections of distance are computed.


1764 ◽  
Vol 54 ◽  
pp. 263-276

The following rules, excepting one, are the same which I have already communicated to the Royal Society, but without demonstration, in a letter to the reverend Dr. Birch from St. Helena, containing the results of my observations of the distance of the Moon from the Sun and fixed stars, taken in my voyage thither, for finding the longitude of the ship from time to time; since printed in Part II. Vol. LII. of the Philosophical Transactions for 1762. The two rules for the correction or refraction and parallax I have also since communicated to the public in my British Mariner's Guide to the discovery of longitude from like observations of the Moon; and have added in the Preface a rule for computing a second but smaller correction of parallax, necessary on account of a small imperfection lying in the first rule derived from the fluxions of a spherical triangle. To the rules I have here subjoined their demonstrations.


It has been inferred from measuring the barometrical pressure at different elevations, that the earth’s atmosphere extends to the height of 40 miles, beyond which limit we are left to conjectures, founded on the supposed divisibility of matter; which, if infinite, indicates an infinity of atmosphere. If, however, it consist of ultimate indivisible particles, then expansion of the medium composed of them must cease at that point where the force of gravity downwards, upon a single particle, is equal to the resistance arising from the repulsive force of the medium. If we adopt the latter hypothesis, no part of our atmosphere could ever leave the earth; if the former, every planetary body must possess its respective share, provided we rest our reasoning upon the known properties of matter. The author, therefore, thought it deserving of consideration, whether, in any instance, any deficiency of atmosphere could be proved, and whether, from such source, any conclusive argument could be drawn in favour of ultimate atoms of matter in general; for since the chemical law of definite proportions applies to all forms of matter, if it can be proved that any one body consists of particles no longer divisible, we then can scarcely doubt that all others are similarly constituted. In respect to the non-existence of an atmosphere round the moon, Dr. Wollaston observes, that the quantity of such matter retainable by a body of the moon’s magnitude, could not give rise to any phenomena observable by our instruments; that we should therefore look for information in an opposite direction, and examine that body which has the greatest power; if we there find no appearance of an atmosphere, we may infer that our own is peculiar to the earth. In respect to the sun, for instance, if we calculate at what apparent distance from his body his force is equal to that of gravity at the surface of the earth, it is there that his power would be sufficient to accumulate, from an infinitely divisible medium filling all space, an atmosphere fully equal in density to our own, and therefore producing a refraction of more than 1° in the passage of rays obliquely through it. Dr. Wollaston then proceeds to show, from a detail of observations of the passage of Venus near the sun in superior conjunction, which took place in May last, that no such retardation in the motion of that planet could be perceived in her progress toward the sun, as would occur from increasing refraction, and that the phenomenon does not offer the least evidence of the existence of a solar atmosphere.


2018 ◽  
Vol 3 (2) ◽  
pp. 207-216 ◽  
Author(s):  
David Fisher ◽  
Lionel Sims

Claims first made over half a century ago that certain prehistoric monuments utilised high-precision alignments on the horizon risings and settings of the Sun and the Moon have recently resurfaced. While archaeoastronomy early on retreated from these claims, as a way to preserve the discipline in an academic boundary dispute, it did so without a rigorous examination of Thom’s concept of a “lunar standstill”. Gough’s uncritical resurrection of Thom’s usage of the term provides a long-overdue opportunity for the discipline to correct this slippage. Gough (2013), in keeping with Thom (1971), claims that certain standing stones and short stone rows point to distant horizon features which allow high-precision alignments on the risings and settings of the Sun and the Moon dating from about 1700 BC. To assist archaeoastronomy in breaking out of its interpretive rut and from “going round in circles” (Ruggles 2011), this paper evaluates the validity of this claim. Through computer modelling, the celestial mechanics of horizon alignments are here explored in their landscape context with a view to testing the very possibility of high-precision alignments to the lunar extremes. It is found that, due to the motion of the Moon on the horizon, only low-precision alignments are feasible, which would seem to indicate that the properties of lunar standstills could not have included high-precision markers for prehistoric megalith builders.


1967 ◽  
Vol 71 (2) ◽  
pp. 215
Author(s):  
Earle R. Caley ◽  
Andre Emmerich
Keyword(s):  
The Sun ◽  

2011 ◽  
Vol 366 (1565) ◽  
pp. 697-702 ◽  
Author(s):  
M. Dacke ◽  
M. J. Byrne ◽  
E. Baird ◽  
C. H. Scholtz ◽  
E. J. Warrant

Prominent in the sky, but not visible to humans, is a pattern of polarized skylight formed around both the Sun and the Moon. Dung beetles are, at present, the only animal group known to use the much dimmer polarization pattern formed around the Moon as a compass cue for maintaining travel direction. However, the Moon is not visible every night and the intensity of the celestial polarization pattern gradually declines as the Moon wanes. Therefore, for nocturnal orientation on all moonlit nights, the absolute sensitivity of the dung beetle's polarization detector may limit the precision of this behaviour. To test this, we studied the straight-line foraging behaviour of the nocturnal ball-rolling dung beetle Scarabaeus satyrus to establish when the Moon is too dim—and the polarization pattern too weak—to provide a reliable cue for orientation. Our results show that celestial orientation is as accurate during crescent Moon as it is during full Moon. Moreover, this orientation accuracy is equal to that measured for diurnal species that orient under the 100 million times brighter polarization pattern formed around the Sun. This indicates that, in nocturnal species, the sensitivity of the optical polarization compass can be greatly increased without any loss of precision.


2009 ◽  
Vol 5 (S260) ◽  
pp. 514-521
Author(s):  
Ilias M. Fernini

AbstractThe Islamic society has great ties to astronomy. Its main religious customs (start of the Islamic month, direction of prayer, and the five daily prayers) are all related to two main celestial objects: the Sun and the Moon. First, the start of any Islamic month is related to the actual seeing of the young crescent after the new Moon. Second, the direction of prayer, i.e., praying towards Mecca, is related to the determination of the zenith point in Mecca. Third, the proper time for the five daily prayers is related to the motion of the Sun. Everyone in the society is directly concerned by these customs. This is to say that the major impetus for the growth of Islamic astronomy came from these three main religious observances which presented an assortment of problems in mathematical astronomy. To observe these three customs, a new set of astronomical observations were needed and this helped the development of the Islamic observatory. There is a claim that it was first in Islam that the astronomical observatory came into real existence. The Islamic observatory was a product of needs and values interwoven into the Islamic society and culture. It is also considered as a true representative and an integral par of the Islamic civilisation. Since astronomy interested not only men of science, but also the rulers of the Islamic empire, several observatories have flourished. The observatories of Baghdad, Cairo, Córdoba, Toledo, Maragha, Samarqand and Istanbul acquired a worldwide reputation throughout the centuries. This paper will discuss the two most important observatories (Maragha and Samarqand) in terms of their instruments and discoveries that contributed to the establishment of these scientific institutions.


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