The Planets in Aztec Culture

Author(s):  
Susan Milbrath

The Spanish chronicles do not mention planets other than Venus, although they compare certain Aztec gods with classical gods such as Jupiter and Mars. Creation myths recorded by the Spanish chroniclers frequently name Venus gods, most notably Ehecatl-Quetzalcoatl and Tlahuizcalpantecuhtli. The focus on Venus seen in these texts is also mirrored in colonial period Aztec codices, which feature several Venus gods as rulers of calendar periods associated with the 260-day calendar. The famous Aztec Calendar Stone represents Venus symbols prominently in an image showing the predicted demise of the Sun in an eternal solar eclipse, to be accompanied by earthquakes. Venus is apparently seen as the cause of a total solar eclipse in the Codex Borgia, a pre-conquest codex from Tlaxcala, a community neighboring the Aztecs in central Mexico. Although no pre-conquest Aztec codices survive, the painted screenfold books attributed to neighboring communities in central Mexico provide evidence of the kinds of almanacs that were probably also found in Preconquest Aztec screenfold books. The Codex Borgia has two Venus almanacs associated with heliacal rise events and another focusing on dates that coordinate with events involving Venus and possibly other planets. A unique narrative in the Codex Borgia traces Venus over the course of a year, representing different aspects of the synodical cycle. The transformation of Venus in the narrative is evidenced by subtle changes in the Venus god, Quetzalcoatl, who represents the planet Venus throughout the synodical cycle. Another god, Tlahuizcalpantecuhtli (“lord of dawn”), appears in the narrative associated with Venus as the morning star and also is represented in a death aspect during superior conjunction. This is in keeping with Aztec legends that tell how the Sun killed Tlahuizcalpantecuhtli with his solar rays. The Borgia narrative also helps identify Xolotl as the planet Mercury and provides hints about other planets that may be linked with different aspects of Tezcatlipoca, an Aztec god who ruled the night sky.

1998 ◽  
Vol 162 ◽  
pp. 197-201
Author(s):  
R.H. Trevisan

This project had two principal objectives: to communicate safe methods to observe the Sun, so as to prevent ophthalmological accidents to people during the total solar eclipse of 3rd November 1994, and to collaborate with the primary school teachers in the science classroom, illustrating the classes, motivating the students to observe sky phenomena.In January 1993, a commission called “ECLIPSE 94“Executive Commission, of the Brazilian Astronomical Society was created to coordinate assistance with arrangements for observing the total solar eclipse of 3rd November 1994, that in Brazil was total in the western part of Paraná State, in Santa Catarina State and in a Rio Grande do Sul zone. Professional astronomers from Brazil and from several parts of the world were mobilized to observe this eclipse.


Solar Physics ◽  
1987 ◽  
Vol 108 (1) ◽  
pp. 191-194 ◽  
Author(s):  
Jay M. Pasachoff ◽  
Brant O. Nelson

An expedition to observe the total solar eclipse of August 30 having been sanctioned by the Admiralty, it was arranged, in concert with the Joint Permanent Eclipse Committee, that a party from the Royal Observatory should make observations at Sfax, a town on the north coast of Africa, about 150 miles south of Tunis. The programme of observations consisted of photographs of the corona on various scales for coronal detail and streamers, and photographs of the spectrum of the corona and chromosphere. The observers from Greenwich who took part in the expedition were Sir William Christie, Mr. Dyson, and Mr. Davidson. Professor Sampson, Mr. J. J. Atkinson, and Captain Brett, D. S. O., generously volunteered their assistance and shared the work of erecting and adjusting the instruments as well as of the observations on the day of the eclipse.


1869 ◽  
Vol 17 ◽  
pp. 125-125

These observations are contained in a letter dated “S. S. 'Carnatic,' Suez, 28th August, 1868,” addressed to the Managing Directors, Peninsular and Oriental Steam Navigation Company. One of the hand spectroscopes sent out by the Royal Society had been entrusted to Captain Perrins; but as his ship at the time of the eclipse was about 20 miles north of the track of the total phase, he had no opportunity of using it for the observations contemplated. He thus describes the appearance at the time of greatest obscuration:— "That portion of the sun remaining uneclipsed consisted of a narrow streak (in shape like a crescent) of its upper left limb, in size about 1/16 part of its diameter. The light emitted from this was of a very peculiar description and difficult to describe, being at the same time extremely brilliant and yet most remarkably pale. The high sea running appeared like huge waves of liquid lead, and the ghastly paleness of the light thrown upon it and all around revealed a scene which, for its weird-like effect, it would be as impossible to depict as it is to describe."


2019 ◽  
pp. 83-87 ◽  
Author(s):  
V. Merzlyakov ◽  
Ts. Tsvetkov ◽  
L. Starkova ◽  
R. Miteva

Ground-based total solar eclipse observations are still the key method for coronal investigations. The question about its white-light degree of polarization remains unanswered. There are hypotheses claiming that the degree of polarization in certain regions of the corona may be higher than the maximal theoretically predicted value determined by Thomson scattering. We present polarization of the white-light solar corona observations obtained by three different teams during the March 29, 2006 solar total eclipse. We give an interpretation on how the polarization of the sky impacts brightness of the polarized solar corona, depending on the landscape during the totality. Moreover, it is shown that the singular polarization points of the corona are in linear dependence with the height of the Sun above the horizon.


2020 ◽  
Vol 29 (11) ◽  
pp. 2041001
Author(s):  
Luís C. B. Crispino

In 1911, Einstein proposed that light bending by the Sun’s gravitational field could be measured during a total solar eclipse. The first opportunity in which this measurement would be tried was during the total solar eclipse of October 10, 1912. We report about the expeditions sent to Brazil to observe this eclipse, including the one from the Córdoba Observatory, from Argentina, which aimed to measure this Einstein’s effect.


1868 ◽  
Vol 16 ◽  
pp. 241-243

The instrument described in this paper was contrived in the summer of 1866, for the purpose of observing the spectra of meteors and their trains. The special suitability of this apparatus, as a hand-spectroscope , for the examination of the spectra of the lights which may be seen about the sun during the total solar eclipse of next year, induces me to offer a description of it to the Royal Society. The apparatus consists essentially of a direct-vision prism placed in front of a small achromatic telescope.


2015 ◽  
Vol 11 (S320) ◽  
pp. 351-354 ◽  
Author(s):  
David W. Dunham ◽  
Sabatino Sofia ◽  
Konrad Guhl ◽  
David Herald

AbstractThe widths of total solar eclipse paths depends on the diameter of the Sun, so if observations are obtained near both the northern and southern limits of the eclipse path, in principle, the angular diameter of the Sun can be measured. Concerted efforts have been made to obtain contact timings from locations near total solar eclipse path edges since the mid 19th century, and Edmund Halley organized a rather successful first effort in 1715. Members of IOTA have been making increasingly sophisticated observations of the Baily's bead phenomena near central solar eclipse path edges since 1970.


1853 ◽  
Vol 20 (3) ◽  
pp. 503-511
Author(s):  
C. Piazzi Smyth

Eclipses are still, as they have ever been, very important phenomena for the astronomical observer; partly on account of the crucial test which they afford for the examination of the truth of the theory and calculation of the motions, real and apparent, of the Sun and Moon, partly also for the special opportunities which they furnish of inquiring into some of the arcana of the physical characteristics of those bodies.For the former purpose, a partial eclipse will serve almost as well as a total one; while the continued improvement of the observation of meridian passages is now raising these daily measures fully to the importance of the other occasional phenomena, as a test of the theory. But for inquiry into the physics of the Sun, a perfectly total eclipse of that body is necessary; revelations may then happily be procured, which no observation of any other phenomena at any other time, can hope to afford any suspicion of.


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