In astronomy, disrupted planet is a planet, or exoplanet, that has been disrupted, or destroyed, by a nearby, or passing, astronomical body or object, such as a star. The result of such a disruption may be the production of excessive amounts of related gas, dust and debris, that may eventually surround the parent star in the form of a circumstellar disk or debris disk. As a consequence, the orbiting debris field may be an "uneven ring of dust", causing erratic light fluctuations in the apparent luminosity of the parent star, as may have been responsible for the oddly flickering light curves associated with the starlight observed from certain variable stars, such as that from KIC 8462852, RZ Piscium and WD 1145+017. Excessive amounts of infrared radiation may be detected from such stars, suggestive evidence in itself that dust and debris may be orbiting the stars.
Examples of planets (or their related remnants), considered to have been a disrupted planet, or part of such a planet, include: 'Oumuamua and WD 1145+017 b, as well as asteroids, hot Jupiters and those that are hypothetical planets, like Fifth planet, Phaeton, Planet V and Theia.
Light curve galleryEdit
KIC 8462852 (Tabby's Star)Edit
KIC 8462852 is an F-type main-sequence star exhibiting unusual light fluctuations, including up to a 22% dimming in brightness. Several hypotheses have been proposed to explain these irregular changes, but none to date fully explain all aspects of the curve. One explanation is that an "uneven ring of dust" orbits KIC 8462852.
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"Note: g'-band and r'-band dip depths (and shapes) may differ, with g'-band being more sensitive to dust cloud scattering due to its shorter wavelength (0.47 vs. 0.62 micron). For a reasonable particle size distribution (e.g., Hanson, 0.2 micron) the extinction cross section ratio would produce a depth at r'-band that is 0.57 x depth at g'-band. If g'-band depth is 0.3 %, for example, depth at r'-band could be 0.17 %. The "Tabby Team" measurements (Fig. 3) at r'-band are compatible with that small dip depth. Incidentally, none of these shapes resemble exo-comet tail transits (as described by Rappaport et al, 2017 link); so the mystery of what's producing these week-timescale dips continues! Actually, long oval shapes are known to produce V-shaped dips (think of rings with a high inclination)." - bg
- Gary, Bruce L. (1 January 2018). "Hereford Arizona Observatory photometry observations of KIC 8462852 between 2 May and 31 December 2017". BruceGary.net. Archived from the original on 1 January 2018. Retrieved 1 January 2018.
- Gary, Bruce L. (4 May 2018). "Hereford Arizona Observatory photometry observations of KIC 8462852 between 2 May 2017 and 4 May 2018". BruceGary.net. Archived from the original on 5 May 2018. Retrieved 5 May 2018.
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