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OGLE-2006-BLG-109L
OGLE-2006-BLG-109L (where the last 'L' stands for lens) is a dim magnitude 17 M0V galactic bulge star approximately 4,920 light-years away in the constellation of Scorpius. Planetary system In 2008, two extrasolar planets were discovered around the star using gravitational microlensing. The two planets are at a distance from their star that make them suspected analogs of Jupiter and Saturn. The star is surrounded by a planetary system consisting of at least two planets: b with a mass of 0.727 of Jupiter and c with the mass of approximately 0.271 of Jupiter. Their mass ratios, distance ratios, and equilibrium temperatures are similar to those of Jupiter and Saturn in the Solar System as well as the 47 UMa system. Both planets were discovered simultaneously by gravitational microlensing in a common effort by the Optical Gravitational Lensing ExperimentmicroFUN MOA, PLANET and RoboNet collaborations, as announced on 14 February 2008. This is the first planetary system ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Optical Gravitational Lensing Experiment
The Optical Gravitational Lensing Experiment (OGLE) is a Polish astronomy, astronomical project based at the University of Warsaw that runs time-domain astronomy, a long-term variability sky survey (1992–present). The main goals are the detection and classification of variable stars (Pulsating variable, pulsating and Eclipsing variable stars, eclipsing), discovery of microlensing events, dwarf novae, and studies of the structure of the Galaxy and the Magellanic Clouds. Since the project began in 1992, it has discovered a multitude of extrasolar planets, together with the first planet discovered using the transit method (OGLE-TR-56b) and Methods of detecting exoplanets#Gravitational microlensing, gravitational microlensing. The project has been led by professor Andrzej Udalski since its inception. Description The main targets of the experiment are the Magellanic Clouds and the Galactic Bulge, because of the large number of intervening stars that can be used for microlensing du ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
RoboNet
RoboNet-1.0 was a prototype global network of UK-built 2-metre robotic telescopes, the largest of their kind in the world, comprising the Liverpool Telescope on La Palma (Canary Islands), the Faulkes Telescope North on Maui (Hawaii), and the Faulkes Telescope South in Australia, managed by a consortium of ten UK universities under the lead of Liverpool John Moores University. For the technological aims of integrating a global network to act effectively as a single instrument, and maximizing the scientific return by applying the newest developments in e-Science, RoboNet adopted the intelligent-agent architecture devised and maintained by the eSTAR project. With the flexible scheduling and short response time of robotic telescopes being ideal for time-domain astronomy, RoboNet-1.0 had two major science goals that critically depend on these requirements: the determination of origin and nature of gamma-ray bursts, and the detection of cool extra-solar planets by means of gravitational ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Gravitational Microlensing
Gravitational microlensing is an astronomical phenomenon caused by the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light (clouds of gas and dust). These objects make up only a minor portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light. When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Albert Einstein in 1915, leads to two distorted images (generally unresolved), resulting in an observable magnification. The time-scale of the transient brightening depends on the mass of the foreground object as well as on the relative proper motion between the background 'source' and the foreground 'l ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
