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The pictures below represent the best results of those participants who have been able to take series of images which could be well aligned. Further results can be found on the page with "First results".
The images in the left column are originals in their original orientation. In order to be able to compare Mercury's position in front of the sun with that on an image taken at a distant place both images must have exactly the same orientation. In this project the east-west-direction of the images has been determined by taking two images with fixed camera (central column). The successful observers could construct a superposition of all of their images after having oriented them (right column).
in their original orientation
(Superposition of two images)
|Selfmade Transit Series|
|14:30 UT||13:48 UT||13:37 - 15:00 UT|
|13:14:59 UT||13:14:59+13:15:59 UT||12:45 - 18:00 UT|
|12:59:59 UT||12:59:59+13:02:29 UT||12:44:59 - 14:14:58 UT|
|18:00 UT||17:06 UT + 17:09 UT|
|Rosario SF, Argentina
|17:00:00 UT||17:00:00+17:02:30 UT||13:00 - 18:00 UT|
|Parallax effect 13:00 UT
Gifhorn, Germany - Bariloche, Argentina
measured on this combined images: πS=12.9"
|Parallax effect 13:30 UT
Bamberg, Germany - Rosario SF, Argentina
measured on this combined images: πS=13.3"
|Parallax effect 17:00 UT
Medellin, Columbia - Rosario SF, Argentina
measured on this combined images: πS=9.4"
The influence of the above mentioned uncertainties is the larger the smaller the angle to be measured, i. e., the smaller the distance between the observation sites is. But on earth the distance between this distance cannot be larger than twice the earth's radius RE. In this situation we were happy to find the photos which had been taken by the Solar Dynamics Observatory (SDO). That telescope is mounted on a satellite moving around the earth on a geosynchronous orbit the radius of which is approximately six times as large as the earth's radius. SDO, therefore, allows us parallax measurements with a baselength of about 6RE.
In the SDO images the sun's axis of rotation points upwards, i.e., for alignment they must be rotated by about 22.4° counterclockwise.
|Superposition of the SDO images
taken closest to the proposed times
|Rotated to equatorial north and
restricted to only one image per point of time
|Position results which are used in the following|
|Leiferde, Germany - SDO 13:30 UT||Bariloche, Argentina - SDO 14:30 UT|
The following table shows the results which could be derived by combining complete series of project photos with the according SDO photos. Here, not only the uncertainties of the single comparisons are smaller than those of earth-bound measures, but the series additionally allow statistical analysis and an easy estimation of the standard deviation.
and their locations
|Alignments of their series
with the SDO series
|Resulting measures of the
|Mean solar parallax
and its standard deviation
(derived from the line fit values)
|πS = 9.1" ± 0.7"|
|πS = 9.0" ± 0.4"|
|πS = 9.1" ± 0.3"|
|πS = 10.8" ± 0.5"
|Rosario SF, Argentina|
|πS = 10.2" ± 0.4"|
One of our participants, Aldo Kleiman, answered to these remarks as follows: "Beauty may dwell in a sky vista, and even more in a scientific study of a math's formula, beauty dwells without a doubt in the "Transit of Mercury Internet Project." (Thank you!). I remain waiting for the final report."Here it is.