Solar Speed Measurement
Clocking the sun’s speed at specific latitudes in connection with the equinox and solstice.
Procedure and Equipment
The intent of this experiment is to measure the speed of the solar disk across the earth’s surface at a given latitude and at various days of the year in connection with solstice and equinox. The overall time of sunrise to sunset observations we have recorded for many years. But this would be testing the actual speed of passing by specific latitude for the days selected. The observation devices could even be used to check speed variations during the entire day.
FECORE would perform this test by selecting 2 or more locations of the same latitude 18 miles apart. 18 miles will provide that the passing of solar noon will be at least 1 minute apart for any two stations. The distance of 18 miles and the fact that the observation points are on the same latitude would be determined by a portable self contained inertial navigation system without GPS input. This means that GPS would not be used as a latitude or distance determination. Sextant observations or a reliable survey marker could be used to establish the first observation point.
The unit pictured on the right above is a small self contained micro-electro-mechanical system accelerometer. In connection with a memory device it can store all the movements and read out the exact route and end point of any travel. It can run on battery power for days. Total cost of this portion of the distance and positioning system is USD $1300.
At each location identical observation structures would be built. The structure will be two 4 foot by 4 foot opaque sheets spaced 1/4 inch apart and then attached as the top of a 4 X 8 X 8 ft box with solid walls and a flat floor. All the sides would be parallel and the top being level in the east/west and north/south planes. The illustration on the right shows the interior of the box with as if one wall was removed. The box will be aligned east/west so the door seen on the left will be on the west end.
This box will create a narrow shaft of sunlight which will project on the floor of the box. On the floor of the box two straight lines very easy to observe would be drawn directly below the 1/4 inch space in the top of the box. This would create a clear marker of local solar noon from that observation point. A video recording device would be either set on a tripod or set in a holder on the wall to allow the camera to record the observation. The taller the box is the more exactly it can determine solar noon. testing the design in the building phase determine if a taller box is required.
On the day of observation at least 2 boxes would be in operation with observers managing the recording of the observation.
The floor of the box could also be marked out so that morning and afternoon speed checks could be performed. This would provide data on hourly atmospheric refraction changes.
Only by direct observation of the raw facts can useful data be obtained. If we assume certain facts without knowing their accuracy then our experiment’s results will be misinterpreted. The sun’s speed accross the sky does vary over the year. This fact can’t be explained with the mainstream theory. So a very simple straight forward measurement will tell us data that we need to forma better model.