Exoplanets Search Plan

Details Exoplanets Search Plan Exoplanets Search Plan

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.2211q&link_type=abstract

American Astronomical Society, DPS meeting #39, #22.11; Bulletin of the American Astronomical Society, Vol. 39, p.451

Statistics

Methodology

Scientific paper

The event of the variable stars by eclipse occurs owing to the rotation of at least two stars around its center of mass and it's relatively easy to detect because of the large size of the bodies that are involved on it. But in the case of the exoplanets the eclipse that originates is very small, because the variation of the luminous intensity generated is very little on the whole. However, with photometric techniques of high precision, it is possible to detect those passages. Also, there exist astrometrical methods quite complicated for an amateur, so the one we will employ at the Astronomical Observatory of the University of Nariño (COLOMBIA) and which better adapts to our equipment and capacity is the photometric method. Through differential photometry, we will analyze first variable stars weaker than tenth magnitude so we can acquire enough experience on determining stellar passages and then begin a systematic search for exoplanets, in which case photometry must have an accuracy of the order of thousandths of magnitude.
We have already made trials with some variable stars, like the GCVS FZ ORIONIS and the results are quite good, because the accuracy is of the hundredths order of magnitude, but in order to search exoplanets, photometry must have a resolution in the order of few thousandths of magnitude.
First of all we'll test our methodology with stars that have already been established as to hold planets so then we'll start the research seeking after possible exoplanets around other stars.
On the poster it'll be explained the scientific methodology.

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