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@ -67,7 +67,7 @@
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{GPL}{GPL}{GNU General Public License}
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\newacronym[
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description={Simplified General Perturbations models apply to near earth objects with an orbital period of less than 225 minutes. Simplified \glspl{perturbation} models are a set of five mathematical models (SGP, SGP4, SDP4, SGP8 and SDP8) used to calculate orbital state vectors of satellites and space debris relative to the Earth-centered inertial coordinate system. This set of models is often referred to collectively as SGP4 due to the frequency of use of that model particularly with \gls{TLE} sets produced by \gls{NORAD} and \gls{NASA}. These models predict the effect of \glspl{perturbation} caused by the Earth's shape, drag, radiation, and gravitation effects from other bodies such as the sun and moon. See also: \gls{SDP}.%
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description={Simplified General Perturbations models apply to near earth objects with an orbital period of less than 225 minutes. Simplified \glspl{perturbation} models are a set of five mathematical models (SGP, SGP4, SDP4, SGP8 and SDP8) used to calculate orbital state vectors of \glspl{satellite} and space debris relative to the Earth-centered inertial coordinate system. This set of models is often referred to collectively as SGP4 due to the frequency of use of that model particularly with \gls{TLE} sets produced by \gls{NORAD} and \gls{NASA}. These models predict the effect of \glspl{perturbation} caused by the Earth's shape, drag, radiation, and gravitation effects from other bodies such as the sun and moon. See also: \gls{SDP}.%
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\footnote{\cite{enwiki:Simplified_perturbations_models}}
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}]
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{SGP}{SGP}{Simplified General Perturbations}
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@ -129,6 +129,7 @@
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\newacronym[description={Commodity off the shelf.}]{COTS}{COTS}{Commodity off the shelf}
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\newacronym[description={Free open-source hardware. See also: \gls{OSH}.}]{FOSH}{FOSH}{Free open-source hardware}
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\newacronym[description={Free/libre and open-source software. See also: \gls{FOSS}.}]{FLOSS}{FLOSS}{Free/libre and open-source software}
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\newacronym[description={Simple Imaging Polynomial.}]{SIP}{SIP}{Simple Imaging Polynomial}
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%%%%%%%%%%%
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% Acronyms with citations
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@ -316,7 +317,7 @@
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\newglossaryentry{orbit}
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{ name={orbit},
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description={is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and satellites follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion. For most situations, orbital motion is adequately approximated by Newtonian mechanics, which explains gravity as a force obeying an inverse-square law. However, Albert Einstein's general theory of relativity, which accounts for gravity as due to curvature of spacetime, with orbits following geodesics, provides a more accurate calculation and understanding of the exact mechanics of orbital motion.%
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description={is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and \glspl{satellite} follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion. For most situations, orbital motion is adequately approximated by Newtonian mechanics, which explains gravity as a force obeying an inverse-square law. However, Albert Einstein's general theory of relativity, which accounts for gravity as due to curvature of spacetime, with orbits following geodesics, provides a more accurate calculation and understanding of the exact mechanics of orbital motion.%
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\footnote{\cite{enwiki:Orbit}}
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}}
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@ -356,6 +357,12 @@
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\footnote{\cite{enwiki:Gratis-versus-libre}}
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}}
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\newglossaryentry{plate-solver}
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{ name={plate solver},
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description={is software implementing a technique used in astronomy and applied on celestial images. Solving an image is finding match between the imaged stars and a star catalogue. The solution is a math model describing the corresponding astronomical position of each image pixel. The position of reference catalogue stars has to be known to a high accuracy so an astrometric reference catalogue is used. The image solution contains a reference point, often the image centre, image scale, image orientation and in some cases an image distortion model. With the astrometric solution it is possible to: 1) Calculate the celestial coordinates of any object on the image. 2) Synchronize the telescope mount or satellite pointing position to the center of the image taken. Astrometric solving programs extract the star x,y positions from the celestial image, groups them in three-star triangles or four-star quads. Then it calculates for each group a geometric hash code based on the distance and/or angles between the stars in the group. It then compares the resulting hash codes with the hash codes created from catalogue stars to find a match. If it finds sufficient statistically reliable matches, it can calculate transformation factors. There are several conventions to model the transformation from image pixel location to the corresponding celestial coordinates. The simplest linear model is called the \gls{WCS}. A more advanced convention is \gls{SIP} describing the transformation in polynomials to cope with non-linear geometric distortion in the celestial image, mainly caused by the optics.%
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\footnote{\cite{enwiki:Astrometric-solving}}
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}}
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% TO ADD
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% RamSat
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% Dashboard
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Jeff Moe