From 83895bd8df3b2d09b107e7ee10ae0d01024ba556 Mon Sep 17 00:00:00 2001 From: Michael Johne Date: Sun, 3 Nov 2019 19:57:13 +0100 Subject: [PATCH] Add files via upload --- .../Resources/terminology_ArgPeri.html | 34 +++++---- .../Resources/terminology_ComputerName.html | 31 ++++---- .../Resources/terminology_DesgnName.html | 29 ++++---- PlanetoidDB/Resources/terminology_Epoch.html | 73 +++++++++++++++---- PlanetoidDB/Resources/terminology_Flags.html | 62 ++++++++++++---- PlanetoidDB/Resources/terminology_Incl.html | 34 +++++---- .../Resources/terminology_IndexNo.html | 31 ++++---- .../Resources/terminology_LongAscNode.html | 37 ++++++---- PlanetoidDB/Resources/terminology_MagAbs.html | 35 +++++---- .../Resources/terminology_MeanAnomaly.html | 27 ++++--- PlanetoidDB/Resources/terminology_Motion.html | 32 ++++---- .../Resources/terminology_NumbObs.html | 31 ++++---- .../Resources/terminology_NumbOppos.html | 33 +++++---- .../Resources/terminology_ObsLastDate.html | 31 ++++---- .../Resources/terminology_ObsSpan.html | 31 ++++---- PlanetoidDB/Resources/terminology_OrbEcc.html | 31 ++++---- PlanetoidDB/Resources/terminology_Ref.html | 31 ++++---- .../Resources/terminology_RmsResidual.html | 33 +++++---- .../Resources/terminology_SemiMajorAxis.html | 33 +++++---- .../Resources/terminology_SlopeParam.html | 31 ++++---- 20 files changed, 433 insertions(+), 277 deletions(-) diff --git a/PlanetoidDB/Resources/terminology_ArgPeri.html b/PlanetoidDB/Resources/terminology_ArgPeri.html index e193112b..5299053e 100644 --- a/PlanetoidDB/Resources/terminology_ArgPeri.html +++ b/PlanetoidDB/Resources/terminology_ArgPeri.html @@ -1,17 +1,23 @@ - - - - - Argument of perihelion, J2000.0 (degrees) - - - -

Argument of perihelion, J2000.0 (degrees)

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- + + + + + Argument of perihelion, J2000.0 (degrees) + + + +

Argument of perihelion, J2000.0 (degrees)

+

The argument of periapsis (also called argument of perifocus or argument of pericenter), symbolized as <ω, is one of the orbital elements of an orbiting body. Parametrically, ω is the angle from the body's ascending node to its periapsis, measured in the direction of motion.

+

For specific types of orbits, words such as perihelion (for heliocentric orbits), perigee (for geocentric orbits), periastron (for orbits around stars), and so on may replace the word periapsis.

+

An argument of periapsis of 0° means that the orbiting body will be at its closest approach to the central body at the same moment that it crosses the plane of reference from South to North. An argument of periapsis of 90° means that the orbiting body will reach periapsis at its northmost distance from the plane of reference.

+

Adding the argument of periapsis to the longitude of the ascending node gives the longitude of the periapsis. However, especially in discussions of binary stars and exoplanets, the terms "longitude of periapsis" or "longitude of periastron" are often used synonymously with "argument of periapsis".

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_ComputerName.html b/PlanetoidDB/Resources/terminology_ComputerName.html index d2688808..30b413c1 100644 --- a/PlanetoidDB/Resources/terminology_ComputerName.html +++ b/PlanetoidDB/Resources/terminology_ComputerName.html @@ -1,17 +1,20 @@ - - - - - Computer name - - - -

Computer name

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- + + + + + Computer name + + + +

Computer name

+

This is the computer name.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_DesgnName.html b/PlanetoidDB/Resources/terminology_DesgnName.html index 3d054d27..bac01030 100644 --- a/PlanetoidDB/Resources/terminology_DesgnName.html +++ b/PlanetoidDB/Resources/terminology_DesgnName.html @@ -1,17 +1,20 @@ - - - - - Terminology: Readable designation - - - -

Readable designation

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+ + + + + Terminology: Readable designation + + + +

Readable designation

+

This is the readable designation.

\ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_Epoch.html b/PlanetoidDB/Resources/terminology_Epoch.html index 2aca1a8e..763b52bf 100644 --- a/PlanetoidDB/Resources/terminology_Epoch.html +++ b/PlanetoidDB/Resources/terminology_Epoch.html @@ -1,17 +1,62 @@ - - - - - Terminology: Epoch (in packed form, .0 TT) - - - -

Epoch (in packed form, .0 TT)

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- + + + + + Terminology: Epoch (in packed form, .0 TT) + + + +

Epoch (in packed form, .0 TT)

+

In astronomy, an epoch is a moment in time used as a reference point for some time-varying astronomical quantity, such as the celestial coordinates or elliptical orbital elements of a celestial body, because these are subject to perturbations and vary with time. These time-varying astronomical quantities might include, for example, the mean longitude or mean anomaly of a body, the node of its orbit relative to a reference plane, the direction of the apogee or aphelion of its orbit, or the size of the major axis of its orbit.

+

The main use of astronomical quantities specified in this way is to calculate other relevant parameters of motion, in order to predict future positions and velocities. The applied tools of the disciplines of celestial mechanics or its subfield orbital mechanics (for predicting orbital paths and positions for bodies in motion under the gravitational effects of other bodies) can be used to generate an ephemeris, a table of values giving the positions and velocities of astronomical objects in the sky at a given time or times.

+

Astronomical quantities can be specified in any of several ways, for example, as a polynomial function of the time-interval, with an epoch as a temporal point of origin (this is a common current way of using an epoch). Alternatively, the time-varying astronomical quantity can be expressed as a constant, equal to the measure that it had at the epoch, leaving its variation over time to be specified in some other way—for example, by a table, as was common during the 17th and 18th centuries.

+

The word epoch was often used in a different way in older astronomical literature, e.g. during the 18th century, in connection with astronomical tables. At that time, it was customary to denote as "epochs", not the standard date and time of origin for time-varying astronomical quantities, but rather the values at that date and time of those time-varying quantities themselves. In accordance with that alternative historical usage, an expression such as 'correcting the epochs' would refer to the adjustment, usually by a small amount, of the values of the tabulated astronomical quantities applicable to a fixed standard date and time of reference (and not, as might be expected from current usage, to a change from one date and time of reference to a different date and time).

+

Dates of the form YYYYMMDD may be packed into five characters to conserve space.

+

The first two digits of the year are packed into a single character in column 1 (I = 18, J = 19, K = 20). Columns 2-3 contain the last two digits of the year. Column 4 contains the month and column 5 contains the day, coded as detailed below:

+ + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + +
MonthDayCharacter
in Col 4 or 5
Jan.11
Feb.22
Mar.33
Apr.44
May55
June66
July77
Aug.88
Sept.99
Oct.10A
Nov.11B
Dec.12C
13D
14E
15F
16G
17H
18I
19J
20K
21L
22M
23N
24O
25P
26Q
27R
28S
29T
30U
31V
+

Examples:
1996 Jan. 1 = J9611
1996 Jan. 10 = J961A
1996 Sept.30 = J969U
1996 Oct. 1 = J96A1
2001 Oct. 22 = K01AM

+

This system can be extended to dates with non-integral days. The decimal fraction of the day is simply appended to the five characters defined above.

+

Examples:
1998 Jan. 18.73 = J981I73
2001 Oct. 22.138303 = K01AM138303

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_Flags.html b/PlanetoidDB/Resources/terminology_Flags.html index 089e6f80..1e218249 100644 --- a/PlanetoidDB/Resources/terminology_Flags.html +++ b/PlanetoidDB/Resources/terminology_Flags.html @@ -1,17 +1,51 @@ - - - - - 4-hexdigit flags - - - -

4-hexdigit flags

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- + + + + + 4-hexdigit flags + + + +

4-hexdigit flags

+

This information has been updated 2014 July 16, for files created after 18:40 UTC on that day. Classification of distant-orbit types will resume after the MPC ingest data from an outside collaborator.

+

The bottom 6 bits (bits 0 to 5) are used to encode a value representing the orbit type (other values are undefined):

+ + + + + + + + + + + + + +
ValueObject Class
1Atira
2Aten
3Apollo
4Amor
5Object with q < 1.665 AU
6Hungaria
7Unused or internal MPC use only
8Hilda
9Jupiter Trojan
10Distant object
+

Additional information is conveyed by adding in the following bit values:

+ + + + + + + + + + + + +
BitValue
664Unused or internal MPC use only
7128Unused or internal MPC use only
8256Unused or internal MPC use only
9512Unused or internal MPC use only
101024Unused or internal MPC use only
112048Object is NEO
124096Object is 1-km (or larger) NEO
1381921-opposition object seen at earlier opposition
1416384Critical list numbered object
1532768Object is PHA
+

Note that the orbit classification is based on cuts in osculating element space and is not 100% reliable.

+

Note also that certain of the flags are for internal MPC use and are not documented.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_Incl.html b/PlanetoidDB/Resources/terminology_Incl.html index 3ebda6db..866dcc65 100644 --- a/PlanetoidDB/Resources/terminology_Incl.html +++ b/PlanetoidDB/Resources/terminology_Incl.html @@ -1,17 +1,23 @@ - - - - - Inclination to the ecliptic, J2000.0 (degrees) - - - -

Inclination to the ecliptic, J2000.0 (degrees)

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- + + + + + Inclination to the ecliptic, J2000.0 (degrees) + + + +

Inclination to the ecliptic, J2000.0 (degrees)

+

Orbital inclination measures the tilt of an object's orbit around a celestial body. It is expressed as the angle between a reference plane and the orbital plane or axis of direction of the orbiting object.

+

For a satellite orbiting the Earth directly above the equator, the plane of the satellite's orbit is the same as the Earth's equatorial plane, and the satellite's orbital inclination is 0°. The general case for a circular orbit is that it is tilted, spending half an orbit over the northern hemisphere and half over the southern. If the orbit swung between 20° north latitude and 20° south latitude, then its orbital inclination would be 20°.

+

The inclination is one of the six orbital elements describing the shape and orientation of a celestial orbit. It is the angle between the orbital plane and the plane of reference, normally stated in degrees. For a satellite orbiting a planet, the plane of reference is usually the plane containing the planet's equator. For planets in the Solar System, the plane of reference is usually the ecliptic, the plane in which the Earth orbits the Sun. This reference plane is most practical for Earth-based observers. Therefore, Earth's inclination is, by definition, zero.

+

Inclination can instead be measured with respect to another plane, such as the Sun's equator or the invariable plane (the plane that represents the angular momentum of the Solar System, approximately the orbital plane of Jupiter).

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_IndexNo.html b/PlanetoidDB/Resources/terminology_IndexNo.html index 2c8d145b..e80a26a6 100644 --- a/PlanetoidDB/Resources/terminology_IndexNo.html +++ b/PlanetoidDB/Resources/terminology_IndexNo.html @@ -1,17 +1,20 @@ - - - - - Terminology: Index No. - - - -

Index No.

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- + + + + + Terminology: Index No. + + + +

Index No.

+

This is the intern index number.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_LongAscNode.html b/PlanetoidDB/Resources/terminology_LongAscNode.html index e4dc3370..402047b2 100644 --- a/PlanetoidDB/Resources/terminology_LongAscNode.html +++ b/PlanetoidDB/Resources/terminology_LongAscNode.html @@ -1,17 +1,26 @@ - - - - - Longitude of the ascending node, J2000.0 - - - -

Longitude of the ascending node, J2000.0

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- + + + + + Longitude of the ascending node, J2000.0 + + + +

Longitude of the ascending node, J2000.0

+

The longitude of the ascending node (☊ or Ω) is one of the orbital elements used to specify the orbit of an object in space. It is the angle from a reference direction, called the origin of longitude, to the direction of the ascending node, measured in a reference plane. The ascending node is the point where the orbit of the object passes through the plane of reference, as seen in the adjacent image. Commonly used reference planes and origins of longitude include:

+ +

In the case of a binary star known only from visual observations, it is not possible to tell which node is ascending and which is descending. In this case the orbital parameter which is recorded is the longitude of the node, Ω, which is the longitude of whichever node has a longitude between 0 and 180 degrees.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_MagAbs.html b/PlanetoidDB/Resources/terminology_MagAbs.html index 257cfe5a..762537bb 100644 --- a/PlanetoidDB/Resources/terminology_MagAbs.html +++ b/PlanetoidDB/Resources/terminology_MagAbs.html @@ -1,17 +1,24 @@ - - - - - Absolute magnitude, H - - - -

Absolute magnitude, H

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- + + + + + Absolute magnitude, H + + + +

Absolute magnitude, H

+

Absolute magnitude (M) is a measure of the luminosity of a celestial object, on an inverse logarithmic astronomical magnitude scale. An object's absolute magnitude is defined to be equal to the apparent magnitude that the object would have if it were viewed from a distance of exactly 10.0 parsecs (32.6 light-years), without extinction (or dimming) of its light due to absorption by interstellar matter and cosmic dust. By hypothetically placing all objects at a standard reference distance from the observer, their luminosities can be directly compared on a magnitude scale.

+

As with all astronomical magnitudes, the absolute magnitude can be specified for different wavelength ranges corresponding to specified filter bands or passbands; for stars a commonly quoted absolute magnitude is the absolute visual magnitude, which uses the visual (V) band of the spectrum (in the UBV photometric system). Absolute magnitudes are denoted by a capital M, with a subscript representing the filter band used for measurement, such as MV for absolute magnitude in the V band.

+

The more luminous an object, the smaller the numerical value of its absolute magnitude. A difference of 5 magnitudes between the absolute magnitudes of two objects corresponds to a ratio of 100 in their luminosities, and a difference of n magnitudes in absolute magnitude corresponds to a luminosity ratio of 100(n/5). For example, a star of absolute magnitude MV=3.0 would be 100 times more luminous than a star of absolute magnitude MV=8.0 as measured in the V filter band. The Sun has absolute magnitude MV=+4.83. Highly luminous objects can have negative absolute magnitudes: for example, the Milky Way galaxy has an absolute B magnitude of about −20.8.

+

An object's absolute bolometric magnitude (Mbol) represents its total luminosity over all wavelengths, rather than in a single filter band, as expressed on a logarithmic magnitude scale. To convert from an absolute magnitude in a specific filter band to absolute bolometric magnitude, a bolometric correction (BC) is applied.

+

For Solar System bodies that shine in reflected light, a different definition of absolute magnitude (H) is used, based on a standard reference distance of one astronomical unit.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_MeanAnomaly.html b/PlanetoidDB/Resources/terminology_MeanAnomaly.html index 861ab36c..f3803839 100644 --- a/PlanetoidDB/Resources/terminology_MeanAnomaly.html +++ b/PlanetoidDB/Resources/terminology_MeanAnomaly.html @@ -1,17 +1,20 @@ - - - - - Terminology: Mean anomaly at the epoch, in degrees - - + + + + + Terminology: Mean anomaly at the epoch, in degrees + +

Mean anomaly at the epoch, in degrees

-

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- +

In celestial mechanics, the mean anomaly is the fraction of an elliptical orbit's period that has elapsed since the orbiting body passed periapsis, expressed as an angle which can be used in calculating the position of that body in the classical two-body problem. It is the angular distance from the pericenter which a fictitious body would have if it moved in a circular orbit, with constant speed, in the same orbital period as the actual body in its elliptical orbit.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_Motion.html b/PlanetoidDB/Resources/terminology_Motion.html index cedf443e..b53c6161 100644 --- a/PlanetoidDB/Resources/terminology_Motion.html +++ b/PlanetoidDB/Resources/terminology_Motion.html @@ -1,17 +1,21 @@ - - - - - Mean daily motion (degrees per day) - - - -

Mean daily motion (degrees per day)

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- + + + + + Mean daily motion (degrees per day) + + + +

Mean daily motion (degrees per day)

+

In orbital mechanics, mean motion (represented by n) is the angular speed required for a body to complete one orbit, assuming constant speed in a circular orbit which completes in the same time as the variable speed, elliptical orbit of the actual body. The concept applies equally well to a small body revolving about a large, massive primary body or to two relatively same-sized bodies revolving about a common center of mass. While nominally a mean, and theoretically so in the case of two-body motion, in practice the mean motion is not typically an average over time for the orbits of real bodies, which only approximate the two-body assumption. It is rather the instantaneous value which satisfies the above conditions as calculated from the current gravitational and geometric circumstances of the body's constantly-changing, perturbed orbit.

+

Mean motion is used as an approximation of the actual orbital speed in making an initial calculation of the body's position in its orbit, for instance, from a set of orbital elements. This mean position is refined by Kepler's equation to produce the true position.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_NumbObs.html b/PlanetoidDB/Resources/terminology_NumbObs.html index 59c0016a..e230d1cf 100644 --- a/PlanetoidDB/Resources/terminology_NumbObs.html +++ b/PlanetoidDB/Resources/terminology_NumbObs.html @@ -1,17 +1,20 @@ - - - - - Number of observations - - - -

Number of observations

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- + + + + + Number of observations + + + +

Number of observations

+

This is the number of observations.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_NumbOppos.html b/PlanetoidDB/Resources/terminology_NumbOppos.html index f7a6652c..ea56a73f 100644 --- a/PlanetoidDB/Resources/terminology_NumbOppos.html +++ b/PlanetoidDB/Resources/terminology_NumbOppos.html @@ -1,17 +1,22 @@ - - - - - Number of oppositions - - - -

Number of oppositions

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- + + + + + Number of oppositions + + + +

Number of oppositions

+

This is the number of oppositions.

+

In positional astronomy, two astronomical objects are said to be in opposition when they are on opposite sides of the celestial sphere, as observed from a given body (usually Earth).

+

A planet (or asteroid or comet) is said to be "in opposition" when it is in opposition to the Sun. Because most orbits in the Solar System are nearly coplanar to the ecliptic, this occurs when the Sun, Earth, and the body are configured in an approximately straight line, or syzygy; that is, Earth and the body are in the same direction as seen from the Sun. Opposition occurs only for superior planets.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_ObsLastDate.html b/PlanetoidDB/Resources/terminology_ObsLastDate.html index 66d2170c..839c5664 100644 --- a/PlanetoidDB/Resources/terminology_ObsLastDate.html +++ b/PlanetoidDB/Resources/terminology_ObsLastDate.html @@ -1,17 +1,20 @@ - - - - - Date of last observation - - - -

Date of last observation

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- + + + + + Date of last observation + + + +

Date of last observation

+

This is the date of last observation included in orbit solution (YYYYMMDD format).

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_ObsSpan.html b/PlanetoidDB/Resources/terminology_ObsSpan.html index d65dbf83..39108665 100644 --- a/PlanetoidDB/Resources/terminology_ObsSpan.html +++ b/PlanetoidDB/Resources/terminology_ObsSpan.html @@ -1,17 +1,20 @@ - - - - - Observation span - - - -

Observation span

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- + + + + + Observation span + + + +

Observation span

+

This is the observation span with the year of first observation and year of last observation for multiple-opposition orbits or the arc length in days for single-opposition orbits.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_OrbEcc.html b/PlanetoidDB/Resources/terminology_OrbEcc.html index e5aaf53a..1cae1afb 100644 --- a/PlanetoidDB/Resources/terminology_OrbEcc.html +++ b/PlanetoidDB/Resources/terminology_OrbEcc.html @@ -1,17 +1,20 @@ - - - - - Orbital eccentricity - - - -

Orbital eccentricity

-

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- + + + + + Orbital eccentricity + + + +

Orbital eccentricity

+

The orbital eccentricity of an astronomical object is a dimensionless parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabolic escape orbit, and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a Klemperer rosette orbit through the galaxy.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_Ref.html b/PlanetoidDB/Resources/terminology_Ref.html index 3a417695..4f1b9472 100644 --- a/PlanetoidDB/Resources/terminology_Ref.html +++ b/PlanetoidDB/Resources/terminology_Ref.html @@ -1,17 +1,20 @@ - - - - - Reference - - - -

Reference

-

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- + + + + + Reference + + + +

Reference

+

This is the reference where the observation data published.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_RmsResidual.html b/PlanetoidDB/Resources/terminology_RmsResidual.html index 4e236cdd..8b92397b 100644 --- a/PlanetoidDB/Resources/terminology_RmsResidual.html +++ b/PlanetoidDB/Resources/terminology_RmsResidual.html @@ -1,17 +1,22 @@ - - - - - r.m.s. residual (") - - - -

r.m.s. residual (")

-

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- + + + + + r.m.s. residual (") + + + +

r.m.s. residual (")

+

The root-mean-square deviation (RMSD) or root-mean-square error (RMSE) (or sometimes root-mean-squared error) is a frequently used measure of the differences between values (sample or population values) predicted by a model or an estimator and the values observed. The RMSD represents the square root of the second sample moment of the differences between predicted values and observed values or the quadratic mean of these differences. These deviations are called residuals when the calculations are performed over the data sample that was used for estimation and are called errors (or prediction errors) when computed out-of-sample. The RMSD serves to aggregate the magnitudes of the errors in predictions for various times into a single measure of predictive power. RMSD is a measure of accuracy, to compare forecasting errors of different models for a particular dataset and not between datasets, as it is scale-dependent.

+

RMSD is the square root of the average of squared errors. The effect of each error on RMSD is proportional to the size of the squared error; thus larger errors have a disproportionately large effect on RMSD. Consequently, RMSD is sensitive to outliers.

+

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_SemiMajorAxis.html b/PlanetoidDB/Resources/terminology_SemiMajorAxis.html index aad2854a..41440d84 100644 --- a/PlanetoidDB/Resources/terminology_SemiMajorAxis.html +++ b/PlanetoidDB/Resources/terminology_SemiMajorAxis.html @@ -1,17 +1,22 @@ - - - - - Semimajor axis (AU) - - - -

Semimajor axis (AU)

-

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- + + + + + Semimajor axis (AU) + + + +

Semimajor axis (AU)

+

In geometry, the major axis of an ellipse is its longest diameter: a line segment that runs through the center and both foci, with ends at the widest points of the perimeter.

+

The semi-major axis (more properly, major semi-axis) is one half of the major axis, and thus runs from the centre, through a focus, and to the perimeter. The semi-minor axis (more properly, minor semi-axis) of an ellipse or hyperbola is a line segment that is at right angles with the semi-major axis and has one end at the center of the conic section. For the special case of a circle, the lengths of the semi-axes are both equal to the radius of the circle.

+

The length of the semi-major axis a of an ellipse is related to the semi-minor axis's length b through the eccentricity e and the semi-latus rectum l.

+ \ No newline at end of file diff --git a/PlanetoidDB/Resources/terminology_SlopeParam.html b/PlanetoidDB/Resources/terminology_SlopeParam.html index 89fd3710..67d56b07 100644 --- a/PlanetoidDB/Resources/terminology_SlopeParam.html +++ b/PlanetoidDB/Resources/terminology_SlopeParam.html @@ -1,17 +1,20 @@ - - - - - Slope parameter, G - - - -

Slope parameter, G

-

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- + + + + + Slope parameter, G + + + +

Slope parameter, G

+

This is the slope parameter.

+ \ No newline at end of file