Variable stars are stars that change their brightness or magnitude. We are studying extrinsic variable stars, which means the variability in magnitude is caused by the transit of an extrasolar planet. The first transiting extrasolar planet was observed in 1992 by Aleksander Wolszczan. There were three transiting extrasolar planets all orbiting the star pulsar PSR 1257+12 in the constellation Virgo. (Polish Successors of Copernicus, May 2013). Transiting extrasolar planets can be located due to the light of the host star being attenuated by the transit of the extrasolar planet across the star with the process repeating during every orbital period. The period of transit, or how long the extrasolar planet resides in front of the variable star is much shorter than the orbital period. Exoplanet detection has been difficult because not only are extrasolar planets dozens to hundereds of light years away, but the light of their variable star (host star) bleeds in to the image and makes extrasolar planets more difficult to locate and detect. The transit is not able to be seen with the naked eye, but when measured with a telescope, you can detect a slight magnitude change as the extrasolar planet travels in front of the variable star.You can measure the magnitude, airmass, standard deviation, and signal noise ratio of a series of variable stars using online photometry tools such as vPHOT (variable star photometry software). You can observe variable stars and extrasolar planets using online telescope rental services such as itelescope.net with a primary telescope in Sierra Nevada Mountains, California with back up telescopes in Nerpio, Spain and Mayhill, New Mexico, U.S.A. The exoplanet we are looking at is TrES-3B which was first discovered in 2007. It orbits the star GSC 03089-00929 (TrES-3) which is located in the constellation Hercules. This is in the north portion of the sky, and we learned that the best time for viewing the right ascension this star is located at was between 1am and 2am in Denver, CO (2014 Skygazer’s Almanac 2014). This means if there were to be a transit at this time, it would be at the optimal point in the sky for viewing. We are using the telescope Ti24, which is a deep space telescope in Sierra Nevada Mountains, CA, U.S.A. to view the extrasolar planet TrES-3B. To view the correct location at the correct time, astronomers use measurements like Right Ascension, Declination and Universal Time. Right Ascension is measured in hours (h) minutes (m) and seconds (s). Right Asecension and Declination resemble geographic coordinate systems. Declination is measured in degrees (°) arc-minutes (‘) and arc-seconds (“). Universal time is the time kept on the Greenwich Meridian, a standard time that is not relative to location. This is constant throughout the world at any time, which makes time easier to keep track of while using telescopes across the globe. Using this information, you can take photos with a telescope and transfer these images to vPHOT to get an approximate magnitude. Using the magnitudes you can find the influxes to determine the time of transit of the extrasolar planet. The most common method of extrasolar planet detection is entitled Doppler Spectroscopy. This method studies the wavelength that is determined by the frequencies given off by the exoplanet that affect the variable star. This method is proven to be more accurate, but it is more difficult to detect. This is due to the fact that this method is not visible to the eye and you must have suspicion of the location of the extrasolar planet to find it worth your time to use this method to attempt to initially detect the extrasolar planet.