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calculation for Sun, Moon, and planets.","homepage":"https://github.com/cosinekitty/astronomy#readme","keywords":["astronomy","ephemeris","planet","sun","moon","solar","system","sunrise","sunset","equinox","solstice","constellation","orbit"],"repository":{"type":"git","url":"git+https://github.com/cosinekitty/astronomy.git"},"author":{"name":"Donald Cross"},"bugs":{"url":"https://github.com/cosinekitty/astronomy/issues"},"license":"MIT","readme":"# Astronomy Engine (JavaScript / TypeScript)\n\n[![npm](https://img.shields.io/npm/v/astronomy-engine.svg)](https://www.npmjs.com/package/astronomy-engine)\n\nThis is the complete programming reference for the JavaScript version\nof Astronomy Engine. It supports client side programming\nin the browser, and backend use of [Node.js](https://nodejs.org).\n\n[Astronomy Engine is available as an npm package](https://www.npmjs.com/package/astronomy-engine).\n\nBoth the browser and backend versions of the JavaScript code are generated from\n[TypeScript](https://www.typescriptlang.org/) code in `astronomy.ts`,\nwhich is also provided here for those who want to use it directly.\n\nOther programming languages are supported also.\nSee the [home page](https://github.com/cosinekitty/astronomy) for more info.\n\n---\n\n## Quick Start\nTo use Astronomy Engine in your own project, you can use the TypeScript file `astronomy.ts`\nfrom this directory.\n\nFor convenience, this directory also contains human-readable JavaScript files `astronomy.js`\nand minified versions for the browser (`astronomy.browser.min.js`) and Node.js (`astronomy.min.js`).\nThese JavaScript sources are all compiled from the TypeScript source `astronomy.ts`.\n\nTo get started quickly, here are some [browser scripting examples](../../demo/browser/)\nand some [Node.js examples](../../demo/nodejs/).\n\n---\n\n## Topic Index\n\n### Position of Sun, Moon, and planets\n\n| Function | Description |\n| -------- | ----------- |\n| [HelioVector](#HelioVector) | Calculates body position vector with respect to the center of the Sun.   |\n| [GeoVector](#GeoVector)     | Calculates body position vector with respect to the center of the Earth. |\n| [Equator](#Equator)         | Calculates right ascension and declination. |\n| [Ecliptic](#Ecliptic)       | Converts J2000 mean equator (EQJ) coordinates to true ecliptic of date (ECT) coordinates. |\n| [EclipticLongitude](#EclipticLongitude) | Calculates true ecliptic of date (ECT) longitude for a body. |\n| [Horizon](#Horizon)         | Calculates horizontal coordinates (azimuth, altitude) for a given observer on the Earth. |\n| [PairLongitude](#PairLongitude) | Calculates the difference in apparent ecliptic longitude between two bodies, as seen from the Earth. |\n| [BaryState](#BaryState) | Calculates the barycentric position and velocity vectors of the Sun or a planet. |\n\n### Geographic helper functions\n\n| Function | Description |\n| -------- | ----------- |\n| [ObserverVector](#ObserverVector) | Calculates a vector from the center of the Earth to an observer on the Earth's surface. |\n| [VectorObserver](#VectorObserver) | Calculates the geographic coordinates for a geocentric equatorial vector. |\n\n### Rise, set, and culmination times\n\n| Function | Description |\n| -------- | ----------- |\n| [SearchRiseSet](#SearchRiseSet) | Finds time of rise or set for a body as seen by an observer on the Earth. |\n| [SearchAltitude](#SearchAltitude) | Finds time when a body reaches a given altitude above or below the horizon. Useful for finding civil, nautical, or astronomical twilight. |\n| [SearchHourAngle](#SearchHourAngle) | Finds when body reaches a given hour angle for an observer on the Earth. Hour angle = 0 finds culmination, the highest point in the sky. |\n\n### Moon phases\n\n| Function | Description |\n| -------- | ----------- |\n| [MoonPhase](#MoonPhase) | Determines the Moon's phase expressed as an ecliptic longitude. |\n| [SearchMoonQuarter](#SearchMoonQuarter) | Find the first quarter moon phase after a given date and time. |\n| [NextMoonQuarter](#NextMoonQuarter) | Find the next quarter moon phase after a previous one that has been found. |\n\n### Eclipses and Transits\n\n| Function | Description |\n| -------- | ----------- |\n| [SearchLunarEclipse](#SearchLunarEclipse) | Search for the first lunar eclipse after a given date. |\n| [NextLunarEclipse](#NextLunarEclipse) | Continue searching for more lunar eclipses. |\n| [SearchGlobalSolarEclipse](#SearchGlobalSolarEclipse) | Search for the first solar eclipse after a given date that is visible anywhere on the Earth. |\n| [NextGlobalSolarEclipse](#NextGlobalSolarEclipse) | Continue searching for solar eclipses visible anywhere on the Earth. |\n| [SearchLocalSolarEclipse](#SearchLocalSolarEclipse) | Search for the first solar eclipse after a given date that is visible at a particular location on the Earth. |\n| [NextLocalSolarEclipse](#NextLocalSolarEclipse) | Continue searching for solar eclipses visible at a particular location on the Earth. |\n| [SearchTransit](#SearchTransit) | Search for the next transit of Mercury or Venus. |\n| [NextTransit](#NextTransit) | Continue searching for transits of Mercury or Venus. |\n\n### Lunar perigee and apogee\n\n| Function | Description |\n| -------- | ----------- |\n| [SearchLunarApsis](#SearchLunarApsis) | Finds the next perigee or apogee of the Moon after a specified date. |\n| [NextLunarApsis](#NextLunarApsis) | Given an already-found apsis, find the next perigee or apogee of the Moon. |\n\n### Planet perihelion and aphelion\n\n| Function | Description |\n| -------- | ----------- |\n| [SearchPlanetApsis](#SearchPlanetApsis) | Finds the next perihelion or aphelion of a planet after a specified date. |\n| [NextPlanetApsis](#NextPlanetApsis) | Given an already-found apsis, find the next perihelion or aphelion of a planet. |\n\n### Visual magnitude and elongation\n\n| Function | Description |\n| -------- | ----------- |\n| [Illumination](#Illumination) | Calculates visual magnitude and phase angle of bodies as seen from the Earth. |\n| [SearchPeakMagnitude](#SearchPeakMagnitude) | Searches for the date and time Venus will next appear brightest as seen from the Earth. |\n| [AngleFromSun](#AngleFromSun) | Returns full angle seen from Earth between body and Sun. |\n| [Elongation](#Elongation) | Calculates ecliptic longitude angle between a body and the Sun, as seen from the Earth. |\n| [SearchMaxElongation](#SearchMaxElongation) | Searches for the next maximum elongation event for Mercury or Venus that occurs after the given date. |\n\n### Oppositions and conjunctions\n\n| Function | Description |\n| -------- | ----------- |\n| [SearchRelativeLongitude](#SearchRelativeLongitude) | Find oppositions and conjunctions of planets. |\n\n### Equinoxes and solstices\n\n| Function | Description |\n| -------- | ----------- |\n| [Seasons](#Seasons) | Finds the equinoxes and solstices for a given calendar year. |\n| [SunPosition](#SunPosition) | Calculates the Sun's apparent true ecliptic of date (ECT) coordinates as seen from the Earth. |\n\n### Coordinate transforms\n\nThe following orientation systems are supported.\nAstronomy Engine can convert a vector from any of these orientations to any of the others.\nIt also allows converting from a vector to spherical (angular) coordinates and back,\nwithin a given orientation. Note the 3-letter codes for each of the orientation systems;\nthese are used in function and type names.\n\n- **EQJ = J2000 Mean Equator**: Uses the Earth's mean equator (corrected for precession but ignoring nutation) on January 1, 2000, at noon UTC. This moment in time is called J2000.\n- **EQD = True Equator of Date**: Uses the Earth's equator on a given date and time, adjusted for precession and nutation.\n- **ECL = J2000 Mean Ecliptic**: Uses the plane of the Earth's orbit around the Sun at J2000. The x-axis is referenced against the J2000 mean equinox.\n- **ECT = True Ecliptic of Date**: Uses the true (corrected for precession and nutation) orbital plane of the Earth on the given date. The x-axis is referenced against the true equinox for that date.\n- **HOR = Horizontal**: Uses the viewpoint of an observer at a specific location on the Earth at a given date and time.\n- **GAL = Galactic**: Based on the IAU 1958 definition of galactic coordinates.\n\n| Function | Description |\n| -------- | ----------- |\n| [RotateVector](#RotateVector) | Applies a rotation matrix to a vector, yielding a vector in another orientation system. |\n| [InverseRotation](#InverseRotation) | Given a rotation matrix, finds the inverse rotation matrix that does the opposite transformation. |\n| [CombineRotation](#CombineRotation) | Given two rotation matrices, returns a rotation matrix that combines them into a net transformation. |\n| [IdentityMatrix](#IdentityMatrix) | Returns a 3x3 identity matrix, which can be used to form other rotation matrices. |\n| [Pivot](#Pivot) | Transforms a rotation matrix by pivoting it around a given axis by a given angle. |\n| [VectorFromSphere](#VectorFromSphere) | Converts spherical coordinates to Cartesian coordinates. |\n| [SphereFromVector](#SphereFromVector) | Converts Cartesian coordinates to spherical coordinates. |\n| [EquatorFromVector](#EquatorFromVector) | Given an equatorial vector, calculates equatorial angular coordinates. |\n| [VectorFromHorizon](#VectorFromHorizon) | Given apparent angular horizontal coordinates, calculates horizontal vector. |\n| [HorizonFromVector](#HorizonFromVector) | Given a vector in horizontal orientation, calculates horizontal angular coordinates. |\n| [Rotation_EQD_EQJ](#Rotation_EQD_EQJ) | Calculates a rotation matrix from true equator of date (EQD) to J2000 mean equator (EQJ). |\n| [Rotation_EQD_ECT](#Rotation_EQD_ECT) | Calculates a rotation matrix from true equator of date (EQD) to true ecliptic of date (ECT). |\n| [Rotation_EQD_ECL](#Rotation_EQD_ECL) | Calculates a rotation matrix from true equator of date (EQD) to J2000 mean ecliptic (ECL). |\n| [Rotation_EQD_HOR](#Rotation_EQD_HOR) | Calculates a rotation matrix from true equator of date (EQD) to horizontal (HOR). |\n| [Rotation_EQJ_EQD](#Rotation_EQJ_EQD) | Calculates a rotation matrix from J2000 mean equator (EQJ) to true equator of date (EQD). |\n| [Rotation_EQJ_ECT](#Rotation_EQJ_ECT) | Calculates a rotation matrix from J2000 mean equator (EQJ) to true ecliptic of date (ECT). |\n| [Rotation_EQJ_ECL](#Rotation_EQJ_ECL) | Calculates a rotation matrix from J2000 mean equator (EQJ) to J2000 mean ecliptic (ECL). |\n| [Rotation_EQJ_HOR](#Rotation_EQJ_HOR) | Calculates a rotation matrix from J2000 mean equator (EQJ) to horizontal (HOR). |\n| [Rotation_ECT_EQD](#Rotation_ECT_EQD) | Calculates a rotation matrix from true ecliptic of date (ECT) to true equator of date (EQD). |\n| [Rotation_ECT_EQJ](#Rotation_ECT_EQJ) | Calculates a rotation matrix from true ecliptic of date (ECT) J2000 mean equator (EQJ). |\n| [Rotation_ECL_EQD](#Rotation_ECL_EQD) | Calculates a rotation matrix from J2000 mean ecliptic (ECL) to true equator of date (EQD). |\n| [Rotation_ECL_EQJ](#Rotation_ECL_EQJ) | Calculates a rotation matrix from J2000 mean ecliptic (ECL) to J2000 mean equator (EQJ). |\n| [Rotation_ECL_HOR](#Rotation_ECL_HOR) | Calculates a rotation matrix from J2000 mean ecliptic (ECL) to horizontal (HOR). |\n| [Rotation_HOR_EQD](#Rotation_HOR_EQD) | Calculates a rotation matrix from horizontal (HOR) to true equator of date (EQD). |\n| [Rotation_HOR_EQJ](#Rotation_HOR_EQJ) | Calculates a rotation matrix from horizontal (HOR) to J2000 mean equator (EQJ). |\n| [Rotation_HOR_ECL](#Rotation_HOR_ECL) | Calculates a rotation matrix from horizontal (HOR) to J2000 mean ecliptic (ECL). |\n| [Rotation_EQJ_GAL](#Rotation_EQJ_GAL) | Calculates a rotation matrix from J2000 mean equator (EQJ) to galactic (GAL). |\n| [Rotation_GAL_EQJ](#Rotation_GAL_EQJ) | Calculates a rotation matrix from galactic (GAL) to J2000 mean equator (EQJ). |\n\n### Gravitational simulation of small bodies\n\nAstronomy Engine provides a [GravitySimulator](#GravitySimulator) class\nthat allows you to model the trajectories of one or more small bodies like asteroids,\ncomets, or coasting spacecraft. If you know an initial position vector\nand velocity vector for a small body, the gravity simulator can incrementally\nsimulate the pull of gravity on it from the Sun and planets, to calculate its\nmovement through the Solar System.\n\n---\n\n## API Reference\n\n<a name=\"AstroTime\"></a>\n\n## AstroTime\n**Kind**: global class  \n**Brief**: The date and time of an astronomical observation.\n\nObjects of type `AstroTime` are used throughout the internals\nof the Astronomy library, and are included in certain return objects.\nUse the constructor or the [MakeTime](#MakeTime) function to create an `AstroTime` object.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| date | <code>Date</code> | The JavaScript Date object for the given date and time.      This Date corresponds to the numeric day value stored in the `ut` property. |\n| ut | <code>number</code> | Universal Time (UT1/UTC) in fractional days since the J2000 epoch.      Universal Time represents time measured with respect to the Earth's rotation,      tracking mean solar days.      The Astronomy library approximates UT1 and UTC as being the same thing.      This gives sufficient accuracy for the precision requirements of this project. |\n| tt | <code>number</code> | Terrestrial Time in fractional days since the J2000 epoch.      TT represents a continuously flowing ephemeris timescale independent of      any variations of the Earth's rotation, and is adjusted from UT      using a best-fit piecewise polynomial model devised by      [Espenak and Meeus](https://eclipse.gsfc.nasa.gov/SEhelp/deltatpoly2004.html). |\n\n\n* * *\n\n<a name=\"new_AstroTime_new\"></a>\n\n### new AstroTime(date)\n\n| Param | Type | Description |\n| --- | --- | --- |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | A JavaScript Date object, a numeric UTC value expressed in J2000 days, or another AstroTime object. |\n\n\n* * *\n\n<a name=\"AstroTime+toString\"></a>\n\n### astroTime.toString() ⇒ <code>string</code>\nFormats an `AstroTime` object as an [ISO 8601](https://en.wikipedia.org/wiki/ISO_8601)\ndate/time string in UTC, to millisecond resolution.\nExample: `2018-08-17T17:22:04.050Z`\n\n**Kind**: instance method of [<code>AstroTime</code>](#AstroTime)  \n\n* * *\n\n<a name=\"AstroTime+AddDays\"></a>\n\n### astroTime.AddDays(days) ⇒ [<code>AstroTime</code>](#AstroTime)\nReturns a new `AstroTime` object adjusted by the floating point number of days.\nDoes NOT modify the original `AstroTime` object.\n\n**Kind**: instance method of [<code>AstroTime</code>](#AstroTime)  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| days | <code>number</code> | The floating point number of days by which to adjust the given date and time.      Positive values adjust the date toward the future, and      negative values adjust the date toward the past. |\n\n\n* * *\n\n<a name=\"AstroTime.FromTerrestrialTime\"></a>\n\n### AstroTime.FromTerrestrialTime(tt) ⇒ [<code>AstroTime</code>](#AstroTime)\n**Kind**: static method of [<code>AstroTime</code>](#AstroTime)  \n**Returns**: [<code>AstroTime</code>](#AstroTime) - An `AstroTime` object for the specified terrestrial time.  \n**Brief**: Creates an `AstroTime` value from a Terrestrial Time (TT) day value.\n\nThis function can be used in rare cases where a time must be based\non Terrestrial Time (TT) rather than Universal Time (UT).\nMost developers will want to invoke `new AstroTime(ut)` with a universal time\ninstead of this function, because usually time is based on civil time adjusted\nby leap seconds to match the Earth's rotation, rather than the uniformly\nflowing TT used to calculate solar system dynamics. In rare cases\nwhere the caller already knows TT, this function is provided to create\nan `AstroTime` value that can be passed to Astronomy Engine functions.  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| tt | <code>number</code> | The number of days since the J2000 epoch as expressed in Terrestrial Time. |\n\n\n* * *\n\n<a name=\"LibrationInfo\"></a>\n\n## LibrationInfo\n**Kind**: global class  \n**Brief**: Lunar libration angles, returned by [Libration](#Libration).  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| elat | <code>number</code> | Sub-Earth libration ecliptic latitude angle, in degrees. |\n| elon | <code>number</code> | Sub-Earth libration ecliptic longitude angle, in degrees. |\n| mlat | <code>number</code> | Moon's geocentric ecliptic latitude, in degrees. |\n| mlon | <code>number</code> | Moon's geocentric ecliptic longitude, in degrees. |\n| dist_km | <code>number</code> | Distance between the centers of the Earth and Moon in kilometers. |\n| diam_deg | <code>number</code> | The apparent angular diameter of the Moon, in degrees, as seen from the center of the Earth. |\n\n\n* * *\n\n<a name=\"Vector\"></a>\n\n## Vector\n**Kind**: global class  \n**Brief**: A 3D Cartesian vector with a time attached to it.\n\nHolds the Cartesian coordinates of a vector in 3D space,\nalong with the time at which the vector is valid.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| x | <code>number</code> | The x-coordinate expressed in astronomical units (AU). |\n| y | <code>number</code> | The y-coordinate expressed in astronomical units (AU). |\n| z | <code>number</code> | The z-coordinate expressed in astronomical units (AU). |\n| t | [<code>AstroTime</code>](#AstroTime) | The time at which the vector is valid. |\n\n\n* * *\n\n<a name=\"Vector+Length\"></a>\n\n### vector.Length() ⇒ <code>number</code>\nReturns the length of the vector in astronomical units (AU).\n\n**Kind**: instance method of [<code>Vector</code>](#Vector)  \n\n* * *\n\n<a name=\"StateVector\"></a>\n\n## StateVector\n**Kind**: global class  \n**Brief**: A combination of a position vector, a velocity vector, and a time.\n\nHolds the state vector of a body at a given time, including its position,\nvelocity, and the time they are valid.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| x | <code>number</code> | The position x-coordinate expressed in astronomical units (AU). |\n| y | <code>number</code> | The position y-coordinate expressed in astronomical units (AU). |\n| z | <code>number</code> | The position z-coordinate expressed in astronomical units (AU). |\n| vx | <code>number</code> | The velocity x-coordinate expressed in AU/day. |\n| vy | <code>number</code> | The velocity y-coordinate expressed in AU/day. |\n| vz | <code>number</code> | The velocity z-coordinate expressed in AU/day. |\n| t | [<code>AstroTime</code>](#AstroTime) | The time at which the vector is valid. |\n\n\n* * *\n\n<a name=\"Spherical\"></a>\n\n## Spherical\n**Kind**: global class  \n**Brief**: Holds spherical coordinates: latitude, longitude, distance.\n\nSpherical coordinates represent the location of\na point using two angles and a distance.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| lat | <code>number</code> | The latitude angle: -90..+90 degrees. |\n| lon | <code>number</code> | The longitude angle: 0..360 degrees. |\n| dist | <code>number</code> | Distance in AU. |\n\n\n* * *\n\n<a name=\"EquatorialCoordinates\"></a>\n\n## EquatorialCoordinates\n**Kind**: global class  \n**Brief**: Holds right ascension, declination, and distance of a celestial object.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| ra | <code>number</code> | Right ascension in sidereal hours: [0, 24). |\n| dec | <code>number</code> | Declination in degrees: [-90, +90]. |\n| dist | <code>number</code> | Distance to the celestial object expressed in      <a href=\"https://en.wikipedia.org/wiki/Astronomical_unit\">astronomical units</a> (AU). |\n| vec | [<code>Vector</code>](#Vector) | The equatorial coordinates in cartesian form, using AU distance units.      x = direction of the March equinox,      y = direction of the June solstice,      z = north. |\n\n\n* * *\n\n<a name=\"RotationMatrix\"></a>\n\n## RotationMatrix\n**Kind**: global class  \n**Brief**: Contains a rotation matrix that can be used to transform one coordinate system to another.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| rot | <code>Array.&lt;Array.&lt;number&gt;&gt;</code> | A normalized 3x3 rotation matrix. For example, the identity matrix is represented      as `[[1, 0, 0], [0, 1, 0], [0, 0, 1]]`. |\n\n\n* * *\n\n<a name=\"HorizontalCoordinates\"></a>\n\n## HorizontalCoordinates\n**Kind**: global class  \n**Brief**: Represents the location of an object seen by an observer on the Earth.\n\nHolds azimuth (compass direction) and altitude (angle above/below the horizon)\nof a celestial object as seen by an observer at a particular location on the Earth's surface.\nAlso holds right ascension and declination of the same object.\nAll of these coordinates are optionally adjusted for atmospheric refraction;\ntherefore the right ascension and declination values may not exactly match\nthose found inside a corresponding [EquatorialCoordinates](#EquatorialCoordinates) object.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| azimuth | <code>number</code> | A horizontal compass direction angle in degrees measured starting at north      and increasing positively toward the east.      The value is in the range [0, 360).      North = 0, east = 90, south = 180, west = 270. |\n| altitude | <code>number</code> | A vertical angle in degrees above (positive) or below (negative) the horizon.      The value is in the range [-90, +90].      The altitude angle is optionally adjusted upward due to atmospheric refraction. |\n| ra | <code>number</code> | The right ascension of the celestial body in sidereal hours.      The value is in the reange [0, 24).      If `altitude` was adjusted for atmospheric reaction, `ra`      is likewise adjusted. |\n| dec | <code>number</code> | The declination of of the celestial body in degrees.      The value in the range [-90, +90].      If `altitude` was adjusted for atmospheric reaction, `dec`      is likewise adjusted. |\n\n\n* * *\n\n<a name=\"EclipticCoordinates\"></a>\n\n## EclipticCoordinates\n**Kind**: global class  \n**Brief**: Ecliptic coordinates of a celestial body.\n\nThe origin and date of the coordinate system may vary depending on the caller's usage.\nIn general, ecliptic coordinates are measured with respect to the mean plane of the Earth's\norbit around the Sun.\nIncludes Cartesian coordinates `(ex, ey, ez)` measured in\n<a href=\"https://en.wikipedia.org/wiki/Astronomical_unit\">astronomical units</a> (AU)\nand spherical coordinates `(elon, elat)` measured in degrees.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| vec | [<code>Vector</code>](#Vector) | Ecliptic cartesian vector with components measured in astronomical units (AU).      The x-axis is within the ecliptic plane and is oriented in the direction of the      <a href=\"https://en.wikipedia.org/wiki/Equinox_(celestial_coordinates)\">equinox</a>.      The y-axis is within the ecliptic plane and is oriented 90 degrees      counterclockwise from the equinox, as seen from above the Sun's north pole.      The z-axis is oriented perpendicular to the ecliptic plane,      along the direction of the Sun's north pole. |\n| elat | <code>number</code> | The ecliptic latitude of the body in degrees.      This is the angle north or south of the ecliptic plane.      The value is in the range [-90, +90].      Positive values are north and negative values are south. |\n| elon | <code>number</code> | The ecliptic longitude of the body in degrees.      This is the angle measured counterclockwise around the ecliptic plane,      as seen from above the Sun's north pole.      This is the same direction that the Earth orbits around the Sun.      The angle is measured starting at 0 from the equinox and increases      up to 360 degrees. |\n\n\n* * *\n\n<a name=\"Observer\"></a>\n\n## Observer\n**Kind**: global class  \n**Brief**: Represents the geographic location of an observer on the surface of the Earth.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| latitude | <code>number</code> | The observer's geographic latitude in degrees north of the Earth's equator.      The value is negative for observers south of the equator.      Must be in the range -90 to +90. |\n| longitude | <code>number</code> | The observer's geographic longitude in degrees east of the prime meridian      passing through Greenwich, England.      The value is negative for observers west of the prime meridian.      The value should be kept in the range -180 to +180 to minimize floating point errors. |\n| height | <code>number</code> | The observer's elevation above mean sea level, expressed in meters. |\n\n\n* * *\n\n<a name=\"JupiterMoonsInfo\"></a>\n\n## JupiterMoonsInfo\n**Kind**: global class  \n**Brief**: Holds the positions and velocities of Jupiter's major 4 moons.\n\nThe [JupiterMoons](#JupiterMoons) function returns an object of this type\nto report position and velocity vectors for Jupiter's largest 4 moons\nIo, Europa, Ganymede, and Callisto. Each position vector is relative\nto the center of Jupiter. Both position and velocity are oriented in\nthe EQJ system (that is, using Earth's equator at the J2000 epoch).\nThe positions are expressed in astronomical units (AU),\nand the velocities in AU/day.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| io | [<code>StateVector</code>](#StateVector) | The position and velocity of Jupiter's moon Io. |\n| europa | [<code>StateVector</code>](#StateVector) | The position and velocity of Jupiter's moon Europa. |\n| ganymede | [<code>StateVector</code>](#StateVector) | The position and velocity of Jupiter's moon Ganymede. |\n| callisto | [<code>StateVector</code>](#StateVector) | The position and velocity of Jupiter's moon Callisto. |\n\n\n* * *\n\n<a name=\"IlluminationInfo\"></a>\n\n## IlluminationInfo\n**Kind**: global class  \n**Brief**: Information about the apparent brightness and sunlit phase of a celestial object.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time pertaining to the other calculated values in this object. |\n| mag | <code>number</code> | The <a href=\"https://en.wikipedia.org/wiki/Apparent_magnitude\">apparent visual magnitude</a> of the celestial body. |\n| phase_angle | <code>number</code> | The angle in degrees as seen from the center of the celestial body between the Sun and the Earth.      The value is always in the range 0 to 180.      The phase angle provides a measure of what fraction of the body's face appears      illuminated by the Sun as seen from the Earth.      When the observed body is the Sun, the `phase` property is set to 0,      although this has no physical meaning because the Sun emits, rather than reflects, light.      When the phase is near 0 degrees, the body appears \"full\".      When it is 90 degrees, the body appears \"half full\".      And when it is 180 degrees, the body appears \"new\" and is very difficult to see      because it is both dim and lost in the Sun's glare as seen from the Earth. |\n| phase_fraction | <code>number</code> | The fraction of the body's face that is illuminated by the Sun, as seen from the Earth.      Calculated from `phase_angle` for convenience.      This value ranges from 0 to 1. |\n| helio_dist | <code>number</code> | The distance between the center of the Sun and the center of the body in      <a href=\"https://en.wikipedia.org/wiki/Astronomical_unit\">astronomical units</a> (AU). |\n| geo_dist | <code>number</code> | The distance between the center of the Earth and the center of the body in AU. |\n| gc | [<code>Vector</code>](#Vector) | Geocentric coordinates: the 3D vector from the center of the Earth to the center of the body.      The components are in expressed in AU and are oriented with respect to the J2000 equatorial plane. |\n| hc | [<code>Vector</code>](#Vector) | Heliocentric coordinates: The 3D vector from the center of the Sun to the center of the body.      Like `gc`, `hc` is expressed in AU and oriented with respect      to the J2000 equatorial plane. |\n| ring_tilt | <code>number</code> \\| <code>undefined</code> | For Saturn, this is the angular tilt of the planet's rings in degrees away      from the line of sight from the Earth. When the value is near 0, the rings      appear edge-on from the Earth and are therefore difficult to see.      When `ring_tilt` approaches its maximum value (about 27 degrees),      the rings appear widest and brightest from the Earth.      Unlike the <a href=\"https://ssd.jpl.nasa.gov/horizons.cgi\">JPL Horizons</a> online tool,      this library includes the effect of the ring tilt angle in the calculated value      for Saturn's visual magnitude.      For all bodies other than Saturn, the value of `ring_tilt` is `undefined`. |\n\n\n* * *\n\n<a name=\"MoonQuarter\"></a>\n\n## MoonQuarter\n**Kind**: global class  \n**Brief**: A quarter lunar phase, along with when it occurs.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| quarter | <code>number</code> | An integer as follows:      0 = new moon,      1 = first quarter,      2 = full moon,      3 = third quarter. |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time of the quarter lunar phase. |\n\n\n* * *\n\n<a name=\"AtmosphereInfo\"></a>\n\n## AtmosphereInfo\n**Kind**: global class  \n**Brief**: Information about idealized atmospheric variables at a given elevation.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| pressure | <code>number</code> | Atmospheric pressure in pascals. |\n| temperature | <code>number</code> | Atmospheric temperature in kelvins. |\n| density | <code>number</code> | Atmospheric density relative to sea level. |\n\n\n* * *\n\n<a name=\"HourAngleEvent\"></a>\n\n## HourAngleEvent\n**Kind**: global class  \n**Brief**: Horizontal position of a body upon reaching an hour angle.\n\nReturns information about an occurrence of a celestial body\nreaching a given hour angle as seen by an observer at a given\nlocation on the surface of the Earth.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time of the celestial body reaching the hour angle. |\n| hor | [<code>HorizontalCoordinates</code>](#HorizontalCoordinates) | Topocentric horizontal coordinates for the body      at the time indicated by the `time` property. |\n\n\n* * *\n\n<a name=\"SeasonInfo\"></a>\n\n## SeasonInfo\n**Kind**: global class  \n**Brief**: When the seasons change for a given calendar year.\n\nRepresents the dates and times of the two solstices\nand the two equinoxes in a given calendar year.\nThese four events define the changing of the seasons on the Earth.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| mar_equinox | [<code>AstroTime</code>](#AstroTime) | The date and time of the March equinox in the given calendar year.      This is the moment in March that the plane of the Earth's equator passes      through the center of the Sun; thus the Sun's declination      changes from a negative number to a positive number.      The March equinox defines      the beginning of spring in the northern hemisphere and      the beginning of autumn in the southern hemisphere. |\n| jun_solstice | [<code>AstroTime</code>](#AstroTime) | The date and time of the June solstice in the given calendar year.      This is the moment in June that the Sun reaches its most positive      declination value.      At this moment the Earth's north pole is most tilted most toward the Sun.      The June solstice defines      the beginning of summer in the northern hemisphere and      the beginning of winter in the southern hemisphere. |\n| sep_equinox | [<code>AstroTime</code>](#AstroTime) | The date and time of the September equinox in the given calendar year.      This is the moment in September that the plane of the Earth's equator passes      through the center of the Sun; thus the Sun's declination      changes from a positive number to a negative number.      The September equinox defines      the beginning of autumn in the northern hemisphere and      the beginning of spring in the southern hemisphere. |\n| dec_solstice | [<code>AstroTime</code>](#AstroTime) | The date and time of the December solstice in the given calendar year.      This is the moment in December that the Sun reaches its most negative      declination value.      At this moment the Earth's south pole is tilted most toward the Sun.      The December solstice defines      the beginning of winter in the northern hemisphere and      the beginning of summer in the southern hemisphere. |\n\n\n* * *\n\n<a name=\"ElongationEvent\"></a>\n\n## ElongationEvent\n**Kind**: global class  \n**Brief**: The viewing conditions of a body relative to the Sun.\n\nRepresents the angular separation of a body from the Sun as seen from the Earth\nand the relative ecliptic longitudes between that body and the Earth as seen from the Sun.  \n**See**: [Elongation](#Elongation)  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time of the observation. |\n| visibility | <code>string</code> | Either `\"morning\"` or `\"evening\"`,      indicating when the body is most easily seen. |\n| elongation | <code>number</code> | The angle in degrees, as seen from the center of the Earth,      of the apparent separation between the body and the Sun.      This angle is measured in 3D space and is not projected onto the ecliptic plane.      When `elongation` is less than a few degrees, the body is very      difficult to see from the Earth because it is lost in the Sun's glare.      The elongation is always in the range [0, 180]. |\n| ecliptic_separation | <code>number</code> | The absolute value of the difference between the body's ecliptic longitude      and the Sun's ecliptic longitude, both as seen from the center of the Earth.      This angle measures around the plane of the Earth's orbit (the ecliptic),      and ignores how far above or below that plane the body is.      The ecliptic separation is measured in degrees and is always in the range [0, 180]. |\n\n\n* * *\n\n<a name=\"Apsis\"></a>\n\n## Apsis\n**Kind**: global class  \n**Brief**: A closest or farthest point in a body's orbit around its primary.\n\nFor a planet orbiting the Sun, apsis is a perihelion or aphelion, respectively.\nFor the Moon orbiting the Earth, apsis is a perigee or apogee, respectively.  \n**See**\n\n- [SearchLunarApsis](#SearchLunarApsis)\n- [NextLunarApsis](#NextLunarApsis)\n- [SearchPlanetApsis](#SearchPlanetApsis)\n- [NextPlanetApsis](#NextPlanetApsis)\n\n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time of the apsis. |\n| kind | [<code>ApsisKind</code>](#ApsisKind) | For a closest approach (perigee or perihelion), `kind` is `ApsisKind.Pericenter`.      For a farthest distance event (apogee or aphelion), `kind` is `ApsisKind.Apocenter`. |\n| dist_au | <code>number</code> | The distance between the centers of the two bodies in astronomical units (AU). |\n| dist_km | <code>number</code> | The distance between the centers of the two bodies in kilometers. |\n\n\n* * *\n\n<a name=\"ConstellationInfo\"></a>\n\n## ConstellationInfo\n**Kind**: global class  \n**Brief**: Reports the constellation that a given celestial point lies within.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| symbol | <code>string</code> | 3-character mnemonic symbol for the constellation, e.g. \"Ori\". |\n| name | <code>string</code> | Full name of constellation, e.g. \"Orion\". |\n| ra1875 | <code>number</code> | Right ascension expressed in B1875 coordinates. |\n| dec1875 | <code>number</code> | Declination expressed in B1875 coordinates. |\n\n\n* * *\n\n<a name=\"LunarEclipseInfo\"></a>\n\n## LunarEclipseInfo\n**Kind**: global class  \n**Brief**: Returns information about a lunar eclipse.\n\nReturned by [SearchLunarEclipse](#SearchLunarEclipse) or [NextLunarEclipse](#NextLunarEclipse)\nto report information about a lunar eclipse event.\nWhen a lunar eclipse is found, it is classified as penumbral, partial, or total.\nPenumbral eclipses are difficult to observe, because the Moon is only slightly dimmed\nby the Earth's penumbra; no part of the Moon touches the Earth's umbra.\nPartial eclipses occur when part, but not all, of the Moon touches the Earth's umbra.\nTotal eclipses occur when the entire Moon passes into the Earth's umbra.\n\nThe `kind` field thus holds one of the enum values `EclipseKind.Penumbral`, `EclipseKind.Partial`,\nor `EclipseKind.Total`, depending on the kind of lunar eclipse found.\n\nThe `obscuration` field holds a value in the range [0, 1] that indicates what fraction\nof the Moon's apparent disc area is covered by the Earth's umbra at the eclipse's peak.\nThis indicates how dark the peak eclipse appears. For penumbral eclipses, the obscuration\nis 0, because the Moon does not pass through the Earth's umbra. For partial eclipses,\nthe obscuration is somewhere between 0 and 1. For total lunar eclipses, the obscuration is 1.\n\nField `peak` holds the date and time of the peak of the eclipse, when it is at its peak.\n\nFields `sd_penum`, `sd_partial`, and `sd_total` hold the semi-duration of each phase\nof the eclipse, which is half of the amount of time the eclipse spends in each\nphase (expressed in minutes), or 0 if the eclipse never reaches that phase.\nBy converting from minutes to days, and subtracting/adding with `peak`, the caller\nmay determine the date and time of the beginning/end of each eclipse phase.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| kind | [<code>EclipseKind</code>](#EclipseKind) | The type of lunar eclipse found. |\n| obscuration | <code>number</code> | The peak fraction of the Moon's apparent disc that is covered by the Earth's umbra. |\n| peak | [<code>AstroTime</code>](#AstroTime) | The time of the eclipse at its peak. |\n| sd_penum | <code>number</code> | The semi-duration of the penumbral phase in minutes. |\n| sd_partial | <code>number</code> | The semi-duration of the penumbral phase in minutes, or 0.0 if none. |\n| sd_total | <code>number</code> | The semi-duration of the penumbral phase in minutes, or 0.0 if none. |\n\n\n* * *\n\n<a name=\"GlobalSolarEclipseInfo\"></a>\n\n## GlobalSolarEclipseInfo\n**Kind**: global class  \n**Brief**: Reports the time and geographic location of the peak of a solar eclipse.\n\nReturned by [SearchGlobalSolarEclipse](#SearchGlobalSolarEclipse) or [NextGlobalSolarEclipse](#NextGlobalSolarEclipse)\nto report information about a solar eclipse event.\n\nThe eclipse is classified as partial, annular, or total, depending on the\nmaximum amount of the Sun's disc obscured, as seen at the peak location\non the surface of the Earth.\n\nThe `kind` field thus holds one of the values `EclipseKind.Partial`, `EclipseKind.Annular`, or `EclipseKind.Total`.\nA total eclipse is when the peak observer sees the Sun completely blocked by the Moon.\nAn annular eclipse is like a total eclipse, but the Moon is too far from the Earth's surface\nto completely block the Sun; instead, the Sun takes on a ring-shaped appearance.\nA partial eclipse is when the Moon blocks part of the Sun's disc, but nobody on the Earth\nobserves either a total or annular eclipse.\n\nIf `kind` is `EclipseKind.Total` or `EclipseKind.Annular`, the `latitude` and `longitude`\nfields give the geographic coordinates of the center of the Moon's shadow projected\nonto the daytime side of the Earth at the instant of the eclipse's peak.\nIf `kind` has any other value, `latitude` and `longitude` are undefined and should\nnot be used.\n\nFor total or annular eclipses, the `obscuration` field holds the fraction (0, 1]\nof the Sun's apparent disc area that is blocked from view by the Moon's silhouette,\nas seen by an observer located at the geographic coordinates `latitude`, `longitude`\nat the darkest time `peak`. The value will always be 1 for total eclipses, and less than\n1 for annular eclipses.\nFor partial eclipses, `obscuration` is undefined and should not be used.\nThis is because there is little practical use for an obscuration value of\na partial eclipse without supplying a particular observation location.\nDevelopers who wish to find an obscuration value for partial solar eclipses should therefore use\n[SearchLocalSolarEclipse](#SearchLocalSolarEclipse) and provide the geographic coordinates of an observer.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| kind | [<code>EclipseKind</code>](#EclipseKind) | One of the following enumeration values: `EclipseKind.Partial`, `EclipseKind.Annular`, `EclipseKind.Total`. |\n| obscuration | <code>number</code> \\| <code>undefined</code> | The peak fraction of the Sun's apparent disc area obscured by the Moon (total and annular eclipses only) |\n| peak | [<code>AstroTime</code>](#AstroTime) | The date and time when the solar eclipse is darkest.     This is the instant when the axis of the Moon's shadow cone passes closest to the Earth's center. |\n| distance | <code>number</code> | The distance in kilometers between the axis of the Moon's shadow cone     and the center of the Earth at the time indicated by `peak`. |\n| latitude | <code>number</code> \\| <code>undefined</code> | If `kind` holds `EclipseKind.Total`, the geographic latitude in degrees     where the center of the Moon's shadow falls on the Earth at the     time indicated by `peak`; otherwise, `latitude` holds `undefined`. |\n| longitude | <code>number</code> \\| <code>undefined</code> | If `kind` holds `EclipseKind.Total`, the geographic longitude in degrees     where the center of the Moon's shadow falls on the Earth at the     time indicated by `peak`; otherwise, `longitude` holds `undefined`. |\n\n\n* * *\n\n<a name=\"EclipseEvent\"></a>\n\n## EclipseEvent\n**Kind**: global class  \n**Brief**: Holds a time and the observed altitude of the Sun at that time.\n\nWhen reporting a solar eclipse observed at a specific location on the Earth\n(a \"local\" solar eclipse), a series of events occur. In addition\nto the time of each event, it is important to know the altitude of the Sun,\nbecause each event may be invisible to the observer if the Sun is below\nthe horizon.\n\nIf `altitude` is negative, the event is theoretical only; it would be\nvisible if the Earth were transparent, but the observer cannot actually see it.\nIf `altitude` is positive but less than a few degrees, visibility will be impaired by\natmospheric interference (sunrise or sunset conditions).  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| time | [<code>AstroTime</code>](#AstroTime) | The date and time of the event. |\n| altitude | <code>number</code> | The angular altitude of the center of the Sun above/below the horizon, at `time`,      corrected for atmospheric refraction and expressed in degrees. |\n\n\n* * *\n\n<a name=\"LocalSolarEclipseInfo\"></a>\n\n## LocalSolarEclipseInfo\n**Kind**: global class  \n**Brief**: Information about a solar eclipse as seen by an observer at a given time and geographic location.\n\nReturned by [SearchLocalSolarEclipse](#SearchLocalSolarEclipse) or [NextLocalSolarEclipse](#NextLocalSolarEclipse)\nto report information about a solar eclipse as seen at a given geographic location.\n\nWhen a solar eclipse is found, it is classified by setting `kind`\nto `EclipseKind.Partial`, `EclipseKind.Annular`, or `EclipseKind.Total`.\nA partial solar eclipse is when the Moon does not line up directly enough with the Sun\nto completely block the Sun's light from reaching the observer.\nAn annular eclipse occurs when the Moon's disc is completely visible against the Sun\nbut the Moon is too far away to completely block the Sun's light; this leaves the\nSun with a ring-like appearance.\nA total eclipse occurs when the Moon is close enough to the Earth and aligned with the\nSun just right to completely block all sunlight from reaching the observer.\n\nThe `obscuration` field reports what fraction of the Sun's disc appears blocked\nby the Moon when viewed by the observer at the peak eclipse time.\nThis is a value that ranges from 0 (no blockage) to 1 (total eclipse).\nThe obscuration value will be between 0 and 1 for partial eclipses and annular eclipses.\nThe value will be exactly 1 for total eclipses. Obscuration gives an indication\nof how dark the eclipse appears.\n\nThere are 5 \"event\" fields, each of which contains a time and a solar altitude.\nField `peak` holds the date and time of the center of the eclipse, when it is at its peak.\nThe fields `partial_begin` and `partial_end` are always set, and indicate when\nthe eclipse begins/ends. If the eclipse reaches totality or becomes annular,\n`total_begin` and `total_end` indicate when the total/annular phase begins/ends.\nWhen an event field is valid, the caller must also check its `altitude` field to\nsee whether the Sun is above the horizon at the time indicated by the `time` field.\nSee [EclipseEvent](#EclipseEvent) for more information.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| kind | [<code>EclipseKind</code>](#EclipseKind) | The type of solar eclipse found: `EclipseKind.Partial`, `EclipseKind.Annular`, or `EclipseKind.Total`. |\n| obscuration | <code>number</code> | The fraction of the Sun's apparent disc area obscured by the Moon at the eclipse peak. |\n| partial_begin | [<code>EclipseEvent</code>](#EclipseEvent) | The time and Sun altitude at the beginning of the eclipse. |\n| total_begin | [<code>EclipseEvent</code>](#EclipseEvent) \\| <code>undefined</code> | If this is an annular or a total eclipse, the time and Sun altitude when annular/total phase begins; otherwise undefined. |\n| peak | [<code>EclipseEvent</code>](#EclipseEvent) | The time and Sun altitude when the eclipse reaches its peak. |\n| total_end | [<code>EclipseEvent</code>](#EclipseEvent) \\| <code>undefined</code> | If this is an annular or a total eclipse, the time and Sun altitude when annular/total phase ends; otherwise undefined. |\n| partial_end | [<code>EclipseEvent</code>](#EclipseEvent) | The time and Sun altitude at the end of the eclipse. |\n\n\n* * *\n\n<a name=\"TransitInfo\"></a>\n\n## TransitInfo\n**Kind**: global class  \n**Brief**: Information about a transit of Mercury or Venus, as seen from the Earth.\n\nReturned by [SearchTransit](#SearchTransit) or [NextTransit](#NextTransit) to report\ninformation about a transit of Mercury or Venus.\nA transit is when Mercury or Venus passes between the Sun and Earth so that\nthe other planet is seen in silhouette against the Sun.\n\nThe calculations are performed from the point of view of a geocentric observer.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| start | [<code>AstroTime</code>](#AstroTime) | The date and time at the beginning of the transit.      This is the moment the planet first becomes visible against the Sun in its background. |\n| peak | [<code>AstroTime</code>](#AstroTime) | When the planet is most aligned with the Sun, as seen from the Earth. |\n| finish | [<code>AstroTime</code>](#AstroTime) | The date and time at the end of the transit.      This is the moment the planet is last seen against the Sun in its background. |\n| separation | <code>number</code> | The minimum angular separation, in arcminutes, between the centers of the Sun and the planet.      This angle pertains to the time stored in `peak`. |\n\n\n* * *\n\n<a name=\"NodeEventInfo\"></a>\n\n## NodeEventInfo\n**Kind**: global class  \n**Brief**: Information about an ascending or descending node of a body.\n\nThis object is returned by [SearchMoonNode](#SearchMoonNode) and [NextMoonNode](#NextMoonNode)\nto report information about the center of the Moon passing through the ecliptic plane.  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| kind | [<code>NodeEventKind</code>](#NodeEventKind) | Whether the node is ascending (south to north) or descending (north to south). |\n| time | [<code>AstroTime</code>](#AstroTime) | The time when the body passes through the ecliptic plane. |\n\n\n* * *\n\n<a name=\"AxisInfo\"></a>\n\n## AxisInfo\n**Kind**: global class  \n**Brief**: Information about a body's rotation axis at a given time.\n\nThis structure is returned by [RotationAxis](#RotationAxis) to report\nthe orientation of a body's rotation axis at a given moment in time.\nThe axis is specified by the direction in space that the body's north pole\npoints, using angular equatorial coordinates in the J2000 system (EQJ).\n\nThus `ra` is the right ascension, and `dec` is the declination, of the\nbody's north pole vector at the given moment in time. The north pole\nof a body is defined as the pole that lies on the north side of the\n[Solar System's invariable plane](https://en.wikipedia.org/wiki/Invariable_plane),\nregardless of the body's direction of rotation.\n\nThe `spin` field indicates the angular position of a prime meridian\narbitrarily recommended for the body by the International Astronomical\nUnion (IAU).\n\nThe fields `ra`, `dec`, and `spin` correspond to the variables\nα0, δ0, and W, respectively, from\n[Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2015](https://astropedia.astrogeology.usgs.gov/download/Docs/WGCCRE/WGCCRE2015reprint.pdf).\nThe field `north` is a unit vector pointing in the direction of the body's north pole.\nIt is expressed in the J2000 mean equator system (EQJ).  \n**Properties**\n\n| Name | Type | Description |\n| --- | --- | --- |\n| ra | <code>number</code> | The J2000 right ascension of the body's north pole direction, in sidereal hours. |\n| dec | <code>number</code> | The J2000 declination of the body's north pole direction, in degrees. |\n| spin | <code>number</code> | Rotation angle of the body's prime meridian, in degrees. |\n| north | [<code>Vector</code>](#Vector) | A J2000 dimensionless unit vector pointing in the direction of the body's north pole. |\n\n\n* * *\n\n<a name=\"GravitySimulator\"></a>\n\n## GravitySimulator\n**Kind**: global class  \n**Brief**: A simulation of zero or more small bodies moving through the Solar System.\n\nThis class calculates the movement of arbitrary small bodies,\nsuch as asteroids or comets, that move through the Solar System.\nIt does so by calculating the gravitational forces on the small bodies\nfrom the Sun and planets. The user of this class supplies a\nlist of initial positions and velocities for the small bodies.\nThen the class can update the positions and velocities over small\ntime steps.  \n\n* * *\n\n<a name=\"new_GravitySimulator_new\"></a>\n\n### new GravitySimulator(originBody, date, bodyStates)\n\n| Param | Type | Description |\n| --- | --- | --- |\n| originBody | [<code>Body</code>](#Body) | Specifies the origin of the reference frame.      All position vectors and velocity vectors will use `originBody`      as the origin of the coordinate system.      This origin applies to all the input vectors provided in the      `bodyStates` parameter of this function, along with all      output vectors returned by [Update](#GravitySimulator+Update).      Most callers will want to provide one of the following:      `Body.Sun` for heliocentric coordinates,      `Body.SSB` for solar system barycentric coordinates,      or `Body.Earth` for geocentric coordinates. Note that the      gravity simulator does not correct for light travel time;      all state vectors are tied to a Newtonian \"instantaneous\" time. |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | The initial time at which to start the simulation. |\n| bodyStates | [<code>Array.&lt;StateVector&gt;</code>](#StateVector) | An array of zero or more initial state vectors (positions and velocities)      of the small bodies to be simulated.      The caller must know the positions and velocities of the small bodies at an initial moment in time.      Their positions and velocities are expressed with respect to `originBody`, using equatorial      J2000 orientation (EQJ).      Positions are expressed in astronomical units (AU).      Velocities are expressed in AU/day.      All the times embedded within the state vectors must exactly match `date`,      or this constructor will throw an exception. |\n\n\n* * *\n\n<a name=\"GravitySimulator+OriginBody\"></a>\n\n### gravitySimulator.OriginBody\n**Kind**: instance property of [<code>GravitySimulator</code>](#GravitySimulator)  \n**Brief**: The body that was selected as the coordinate origin when this simulator was created.  \n\n* * *\n\n<a name=\"GravitySimulator+Time\"></a>\n\n### gravitySimulator.Time\n**Kind**: instance property of [<code>GravitySimulator</code>](#GravitySimulator)  \n**Brief**: The time represented by the current step of the gravity simulation.  \n\n* * *\n\n<a name=\"GravitySimulator+Update\"></a>\n\n### gravitySimulator.Update(date) ⇒ [<code>Array.&lt;StateVector&gt;</code>](#StateVector)\nAdvances the gravity simulation by a small time step.\n\nUpdates the simulation of the user-supplied small bodies\nto the time indicated by the `date` parameter.\nReturns an array of state vectors for the simulated bodies.\nThe array is in the same order as the original array that\nwas used to construct this simulator object.\nThe positions and velocities in the returned array are\nreferenced to the `originBody` that was used to construct\nthis simulator.\n\n**Kind**: instance method of [<code>GravitySimulator</code>](#GravitySimulator)  \n**Returns**: [<code>Array.&lt;StateVector&gt;</code>](#StateVector) - An array of state vectors, one for each simulated small body.  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | A time that is a small increment away from the current simulation time.      It is up to the developer to figure out an appropriate time increment.      Depending on the trajectories, a smaller or larger increment      may be needed for the desired accuracy. Some experimentation may be needed.      Generally, bodies that stay in the outer Solar System and move slowly can      use larger time steps. Bodies that pass into the inner Solar System and      move faster will need a smaller time step to maintain accuracy.      The `date` value may be after or before the current simulation time      to move forward or backward in time. |\n\n\n* * *\n\n<a name=\"GravitySimulator+Swap\"></a>\n\n### gravitySimulator.Swap()\nExchange the current time step with the previous time step.\n\nSometimes it is helpful to \"explore\" various times near a given\nsimulation time step, while repeatedly returning to the original\ntime step. For example, when backdating a position for light travel\ntime, the caller may wish to repeatedly try different amounts of\nbackdating. When the backdating solver has converged, the caller\nwants to leave the simulation in its original state.\n\nThis function allows a single \"undo\" of a simulation, and does so\nvery efficiently.\n\nUsually this function will be called immediately after a matching\ncall to [Update](#GravitySimulator+Update). It has the effect of rolling\nback the most recent update. If called twice in a row, it reverts\nthe swap and thus has no net effect.\n\nThe constructor initializes the current state and previous\nstate to be identical. Both states represent the `time` parameter that was\npassed into the constructor. Therefore, `Swap` will\nhave no effect from the caller's point of view when passed a simulator\nthat has not yet been updated by a call to [Update](#GravitySimulator+Update).\n\n**Kind**: instance method of [<code>GravitySimulator</code>](#GravitySimulator)  \n\n* * *\n\n<a name=\"GravitySimulator+SolarSystemBodyState\"></a>\n\n### gravitySimulator.SolarSystemBodyState(body)\nGet the position and velocity of a Solar System body included in the simulation.\n\nIn order to simulate the movement of small bodies through the Solar System,\nthe simulator needs to calculate the state vectors for the Sun and planets.\n\nIf an application wants to know the positions of one or more of the planets\nin addition to the small bodies, this function provides a way to obtain\ntheir state vectors. This is provided for the sake of efficiency, to avoid\nredundant calculations.\n\nThe state vector is returned relative to the position and velocity\nof the `originBody` parameter that was passed to this object's constructor.\n\n**Kind**: instance method of [<code>GravitySimulator</code>](#GravitySimulator)  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| body | [<code>Body</code>](#Body) | The Sun, Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, or Neptune. |\n\n\n* * *\n\n<a name=\"C_AUDAY\"></a>\n\n## C\\_AUDAY\n**Kind**: global variable  \n**Brief**: The speed of light in AU/day.  \n\n* * *\n\n<a name=\"KM_PER_AU\"></a>\n\n## KM\\_PER\\_AU\n**Kind**: global variable  \n**Brief**: The number of kilometers per astronomical unit.  \n\n* * *\n\n<a name=\"AU_PER_LY\"></a>\n\n## AU\\_PER\\_LY\n**Kind**: global variable  \n**Brief**: The number of astronomical units per light-year.  \n\n* * *\n\n<a name=\"DEG2RAD\"></a>\n\n## DEG2RAD\n**Kind**: global variable  \n**Brief**: The factor to convert degrees to radians = pi/180.  \n\n* * *\n\n<a name=\"HOUR2RAD\"></a>\n\n## HOUR2RAD\n**Kind**: global variable  \n**Brief**: The factor to convert sidereal hours to radians = pi/12.  \n\n* * *\n\n<a name=\"RAD2DEG\"></a>\n\n## RAD2DEG\n**Kind**: global variable  \n**Brief**: The factor to convert radians to degrees = 180/pi.  \n\n* * *\n\n<a name=\"RAD2HOUR\"></a>\n\n## RAD2HOUR\n**Kind**: global variable  \n**Brief**: The factor to convert radians to sidereal hours = 12/pi.  \n\n* * *\n\n<a name=\"JUPITER_EQUATORIAL_RADIUS_KM\"></a>\n\n## JUPITER\\_EQUATORIAL\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The equatorial radius of Jupiter, expressed in kilometers.  \n\n* * *\n\n<a name=\"JUPITER_POLAR_RADIUS_KM\"></a>\n\n## JUPITER\\_POLAR\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The polar radius of Jupiter, expressed in kilometers.  \n\n* * *\n\n<a name=\"JUPITER_MEAN_RADIUS_KM\"></a>\n\n## JUPITER\\_MEAN\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The volumetric mean radius of Jupiter, expressed in kilometers.  \n\n* * *\n\n<a name=\"IO_RADIUS_KM\"></a>\n\n## IO\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The mean radius of Jupiter's moon Io, expressed in kilometers.  \n\n* * *\n\n<a name=\"EUROPA_RADIUS_KM\"></a>\n\n## EUROPA\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The mean radius of Jupiter's moon Europa, expressed in kilometers.  \n\n* * *\n\n<a name=\"GANYMEDE_RADIUS_KM\"></a>\n\n## GANYMEDE\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The mean radius of Jupiter's moon Ganymede, expressed in kilometers.  \n\n* * *\n\n<a name=\"CALLISTO_RADIUS_KM\"></a>\n\n## CALLISTO\\_RADIUS\\_KM\n**Kind**: global variable  \n**Brief**: The mean radius of Jupiter's moon Callisto, expressed in kilometers.  \n\n* * *\n\n<a name=\"Body\"></a>\n\n## Body : <code>enum</code>\n**Kind**: global enum  \n**Brief**: String constants that represent the solar system bodies supported by Astronomy Engine.\n\nThe following strings represent solar system bodies supported by various Astronomy Engine functions.\nNot every body is supported by every function; consult the documentation for each function\nto find which bodies it supports.\n\n\"Sun\", \"Moon\", \"Mercury\", \"Venus\", \"Earth\", \"Mars\", \"Jupiter\",\n\"Saturn\", \"Uranus\", \"Neptune\", \"Pluto\",\n\"SSB\" (Solar System Barycenter),\n\"EMB\" (Earth/Moon Barycenter)\n\nYou can also use enumeration syntax for the bodies, like\n`Astronomy.Body.Moon`, `Astronomy.Body.Jupiter`, etc.  \n\n* * *\n\n<a name=\"ApsisKind\"></a>\n\n## ApsisKind : <code>enum</code>\n**Kind**: global enum  \n**Brief**: The two kinds of apsis: pericenter (closest) and apocenter (farthest).\n\n`Pericenter`: The body is at its closest distance to the object it orbits.\n`Apocenter`:  The body is at its farthest distance from the object it orbits.  \n\n* * *\n\n<a name=\"EclipseKind\"></a>\n\n## EclipseKind : <code>enum</code>\n**Kind**: global enum  \n**Brief**: The different kinds of lunar/solar eclipses..\n\n`Penumbral`: A lunar eclipse in which only the Earth's penumbra falls on the Moon. (Never used for a solar eclipse.)\n`Partial`: A partial lunar/solar eclipse.\n`Annular`: A solar eclipse in which the entire Moon is visible against the Sun, but the Sun appears as a ring around the Moon. (Never used for a lunar eclipse.)\n`Total`: A total lunar/solar eclipse.  \n\n* * *\n\n<a name=\"NodeEventKind\"></a>\n\n## NodeEventKind : <code>enum</code>\n**Kind**: global enum  \n**Brief**: Indicates whether a crossing through the ecliptic plane is ascending or descending.\n\n`Invalid` is a placeholder for an unknown or missing node.\n`Ascending` indicates a body passing through the ecliptic plane from south to north.\n`Descending` indicates a body passing through the ecliptic plane from north to south.  \n\n* * *\n\n<a name=\"AngleBetween\"></a>\n\n## AngleBetween(a, b) ⇒ <code>number</code>\n**Kind**: global function  \n**Returns**: <code>number</code> - The angle between the two vectors expressed in degrees.\n     The value is in the range [0, 180].  \n**Brief**: Calculates the angle in degrees between two vectors.\n\nGiven a pair of vectors, this function returns the angle in degrees\nbetween the two vectors in 3D space.\nThe angle is measured in the plane that contains both vectors.  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| a | [<code>Vector</code>](#Vector) | The first of a pair of vectors between which to measure an angle. |\n| b | [<code>Vector</code>](#Vector) | The second of a pair of vectors between which to measure an angle. |\n\n\n* * *\n\n<a name=\"AngleFromSun\"></a>\n\n## AngleFromSun(body, date) ⇒ <code>number</code>\n**Kind**: global function  \n**Returns**: <code>number</code> - An angle in degrees in the range [0, 180].  \n**Brief**: Calculates the angular separation between the Sun and the given body.\n\nReturns the full angle seen from\nthe Earth, between the given body and the Sun.\nUnlike [PairLongitude](#PairLongitude), this function does not\nproject the body's \"shadow\" onto the ecliptic;\nthe angle is measured in 3D space around the plane that\ncontains the centers of the Earth, the Sun, and `body`.  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| body | [<code>Body</code>](#Body) | The name of a supported celestial body other than the Earth. |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | The time at which the angle from the Sun is to be found. |\n\n\n* * *\n\n<a name=\"Atmosphere\"></a>\n\n## Atmosphere(elevationMeters) ⇒ [<code>AtmosphereInfo</code>](#AtmosphereInfo)\n**Kind**: global function  \n**Brief**: Calculates U.S. Standard Atmosphere (1976) variables as a function of elevation.\n\nThis function calculates idealized values of pressure, temperature, and density\nusing the U.S. Standard Atmosphere (1976) model.\n1. COESA, U.S. Standard Atmosphere, 1976, U.S. Government Printing Office, Washington, DC, 1976.\n2. Jursa, A. S., Ed., Handbook of Geophysics and the Space Environment, Air Force Geophysics Laboratory, 1985.\nSee:\nhttps://hbcp.chemnetbase.com/faces/documents/14_12/14_12_0001.xhtml\nhttps://ntrs.nasa.gov/api/citations/19770009539/downloads/19770009539.pdf\nhttps://www.ngdc.noaa.gov/stp/space-weather/online-publications/miscellaneous/us-standard-atmosphere-1976/us-standard-atmosphere_st76-1562_noaa.pdf  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| elevationMeters | <code>number</code> | The elevation above sea level at which to calculate atmospheric variables.      Must be in the range -500 to +100000, or an exception will occur. |\n\n\n* * *\n\n<a name=\"BackdatePosition\"></a>\n\n## BackdatePosition(date, observerBody, targetBody, aberration) ⇒ [<code>Vector</code>](#Vector)\n**Kind**: global function  \n**Returns**: [<code>Vector</code>](#Vector) - The position vector at the solved backdated time.\n     The `t` field holds the time that light left the observed\n     body to arrive at the observer at the observation time.  \n**Brief**: Solve for light travel time correction of apparent position.\n\nWhen observing a distant object, for example Jupiter as seen from Earth,\nthe amount of time it takes for light to travel from the object to the\nobserver can significantly affect the object's apparent position.\n\nThis function solves the light travel time correction for the apparent\nrelative position vector of a target body as seen by an observer body\nat a given observation time.\n\nFor geocentric calculations, [GeoVector](#GeoVector) also includes light\ntravel time correction, but the time `t` embedded in its returned vector\nrefers to the observation time, not the backdated time that light left\nthe observed body. Thus `BackdatePosition` provides direct\naccess to the light departure time for callers that need it.\n\nFor a more generalized light travel correction solver, see [CorrectLightTravel](#CorrectLightTravel).  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | The time of observation. |\n| observerBody | [<code>Body</code>](#Body) | The body to be used as the observation location. |\n| targetBody | [<code>Body</code>](#Body) | The body to be observed. |\n| aberration | <code>boolean</code> | `true` to correct for aberration, or `false` to leave uncorrected. |\n\n\n* * *\n\n<a name=\"BaryState\"></a>\n\n## BaryState(body, date) ⇒ [<code>StateVector</code>](#StateVector)\n**Kind**: global function  \n**Returns**: [<code>StateVector</code>](#StateVector) - An object that contains barycentric position and velocity vectors.  \n**Brief**: Calculates barycentric position and velocity vectors for the given body.\n\nGiven a body and a time, calculates the barycentric position and velocity\nvectors for the center of that body at that time.\nThe vectors are expressed in J2000 mean equator coordinates (EQJ).  \n\n| Param | Type | Description |\n| --- | --- | --- |\n| body | [<code>Body</code>](#Body) | The celestial body whose barycentric state vector is to be calculated.      Supported values are `Body.Sun`, `Body.Moon`, `Body.EMB`, `Body.SSB`, and all planets:      `Body.Mercury`, `Body.Venus`, `Body.Earth`, `Body.Mars`, `Body.Jupiter`,      `Body.Saturn`, `Body.Uranus`, `Body.Neptune`, `Body.Pluto`. |\n| date | [<code>FlexibleDateTime</code>](#FlexibleDateTime) | The date and time for which to calculate position and velocity. |\n\n\n* * *\n\n<a name=\"CombineRotation\"></a>\n\n## CombineRotation(a, b) ⇒ [<code>RotationMatrix</code>](#RotationMatrix)\n**Kind**: g","readmeFilename":"README.md"}