method of detecting extrasolar planets oor Spaans
method of detecting extrasolar planets
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método de detección de planetas extrasolares
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Comparing this method of detecting extrasolar planets with other techniques such as the transit method, one advantage is that the intensity of the planetary deviation does not depend on the planet mass as strongly as effects in other techniques do.
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Mass[edit] The existence of Gliese 581 c and its mass have been measured by the radial velocity method of detecting extrasolar planets.
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It is known that a very small number of extrasolar planets is in a suitable plane for the transition and the early detection method of the atmosphere and its composition was limited to a small number of planets, and in a very short period of time suitable for this type of research.
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Hot Jupiters are the easiest extrasolar planets to detect via the radial-velocity method, because the oscillations they induce in their parent stars' motion are relatively large and rapid compared to those of other known types of planets.
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This method of detecting binaries is also used to locate extrasolar planets orbiting a star.
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Though direct imaging may become more important in the future, the vast majority of known extrasolar planets have only been detected through indirect methods.
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Specially designed direct-imaging instruments such as Gemini Planet Imager, VLT-SPHERE, and SCExAO will image dozens of gas giants, however the vast majority of known extrasolar planets have only been detected through indirect methods.
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Their method for the detection of a celestial body was applied here for the first time in the search for extrasolar planets, and measures with a precision of a few seconds the moments in which the two stars eclipse each other at a maximum.
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Hot Jupiters are the easiest extrasolar planets to detect via the radial-velocity method, because the oscillations they induce in their parent stars' motion are relatively large and rapid, compared to other known types of planets.
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