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Journal of the Royal Astronomical Society of Canada, 2004
Eos, Transactions American Geophysical Union, 2004
2004
The transits of Venus in 1761 and 1769 initiated the first global observation campaigns performed with international cooperation. The goal of these campaigns was the determination of the solar parallax with high precision. Enormous efforts were made to send expeditions to the most distant and then still unknown regions of the Earth to measure the instants of contact of the transits. The determination of the exact value of the solar parallax from these observations was not only of scientific importance, but it was expected to improve the astronomical tables which were used, e.g., for navigation. Hundreds of single measurements were acquired. The astronomers, however, were faced by a new problem: How is such a small quantity like the solar parallax to be derived from observations deteriorated by measuring errors? Is it possible to determine the solar parallax with an accuracy of 0.02" as asserted by Halley? Only a few scientists accepted this challenge, but without adequate processing methods this was a hopeless undertaking. Parameter estimation methods had to be developed at first. The procedures used by Leonhard Euler and Achille-Pierre Dionis Duséjour were similar to modern methods and therefore superior to all other traditional methods. Their results were confirmed by Simon Newcomb at the end of the 19 th century, thus proving the success of these campaigns.
EAS Publications Series, 2005
The Pamplona Planetarium hosted the Spain National Node for the international project named VT-2004, a whole compendium of activities of science popularisation based on the Venus Transit of June 8, 2004, including an on-line calculation of the Astronomical Unit using the transit observation method depicted by Edmond Halley in 17th Century. To achieve a wide knowledge of the activities, and to encourage citizens to participate in, several different networks (mainly using the Internet) were established that coordinated the participation of different institutions and individuals: planetariums and science centres; research institutions, observatories and universities; colleges and schools; amateur astronomer associations and groups; other cultural associations and the media. A wide range of activities were promoted throughout the nation, all of them having thus a common coordination centre. Acceptance from the society was achieved, with a wide coverage of media and great participation of people in all the activities.
The data of 2012 transit of Venus are compared with the ones of 2004. The thickness of the atmosphere of Venus, its aureole and the effect of oblateness and other asphericities in the figure of the Sun are taken into consideration, as well as the black drop effect. A new extrapolation method for the contact times is presented. The next Mercury transit in 2016 will be fully visible from Europe, and the data will be gathered in view of this new method of analysis, to obtain the solar diameter.
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