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Hour angle
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In astronomy and celestial navigation, the hour angle is the dihedral angle between the meridian plane (containing Earth's axis and the zenith) and the hour circle (containing Earth's axis and a given point of interest).[1]
It may be given in degrees, time, or rotations depending on the application. The angle may be expressed as negative east of the meridian plane and positive west of the meridian plane, or as positive westward from 0° to 360°. The angle may be measured in degrees or in time, with 24h = 360° exactly. In celestial navigation, the convention is to measure in degrees westward from the prime meridian (Greenwich hour angle, GHA), from the local meridian (local hour angle, LHA) or from the first point of Aries (sidereal hour angle, SHA).
The hour angle is paired with the declination to fully specify the location of a point on the celestial sphere in the equatorial coordinate system.[2]
Relation with right ascension
[edit]
Assuming in this example the day of the year is the March equinox so the sun lies in the direction of the grey arrow then this star will rise about midnight. Just after the observer reaches the green arrow dawn comes and overwhelms with light the visibility of the star about six hours before it sets on the western horizon. The Right Ascension of the star is about 18h
The local hour angle (LHA) of an object in the observer's sky is or where LHAobject is the local hour angle of the object, LST is the local sidereal time, is the object's right ascension, GST is Greenwich sidereal time and is the observer's longitude (positive east from the prime meridian).[3] These angles can be measured in time (24 hours to a circle) or in degrees (360 degrees to a circle)—one or the other, not both.
Negative hour angles (−180° < LHAobject < 0°) indicate the object is approaching the meridian, positive hour angles (0° < LHAobject < 180°) indicate the object is moving away from the meridian; an hour angle of zero means the object is on the meridian.
Right ascension is frequently given in sexagesimal hours-minutes-seconds format (HH:MM:SS) in astronomy, though may be given in decimal hours, sexagesimal degrees (DDD:MM:SS), or, decimal degrees.
Because the earth rotates 365.2564 times in a sidereal year whereas fixed stars appear to go around one time more, the hour angle of a fixed star increases by 366.2564/365.2564 (about 1.0027) per hour, or in other words it takes 59 minutes and 50.17 seconds for the hour angle to increase by one hour.
Solar hour angle
[edit]Observing the Sun from Earth, the solar hour angle is an expression of time, expressed in angular measurement, usually degrees, from solar noon. At solar noon the hour angle is zero degrees, with the time before solar noon expressed as negative degrees, and the local time after solar noon expressed as positive degrees. For example, at 10:30 AM local apparent time the hour angle is −22.5° (15° per hour times 1.5 hours before noon).[4]
The solar hour angle increases on average by one hour per hour, but because of the equation of time this varies with time of year. In mid-September a solar day is about 22 seconds less than 24 hours, meaning that the solar hour angle increases by 1.00025 hours per hour, whereas in late December a solar day is about 28 seconds more than 24 hours, so the solar hour angle increases by 0.99968 hours per hour.
The cosine of the hour angle (cos(h)) is used to calculate the solar zenith angle. At solar noon, h = 0.000 so cos(h) = 1, and before and after solar noon the cos(± h) term = the same value for morning (negative hour angle) or afternoon (positive hour angle), so that the Sun is at the same altitude in the sky at 11:00AM and 1:00PM solar time.[5]
Sidereal hour angle
[edit]The sidereal hour angle (SHA) of a body on the celestial sphere is its angular distance west of the March equinox generally measured in degrees. The SHA of a star varies by less than a minute of arc per year, due to precession, while the SHA of a planet varies significantly from night to night. SHA is often used in celestial navigation and navigational astronomy, and values are published in nautical almanacs.[citation needed]
See also
[edit]Notes and references
[edit]- ^ U.S. Naval Observatory Nautical Almanac Office (1992). P. Kenneth Seidelmann (ed.). Explanatory Supplement to the Astronomical Almanac. Mill Valley, CA: University Science Books. p. 729. ISBN 0-935702-68-7.
- ^ Explanatory Supplement (1992), p. 724.
- ^ Meeus, Jean (1991). Astronomical Algorithms. Bell, Inc., Richmond, VA. p. 88. ISBN 0-943396-35-2.
- ^ Kreider, J. F. (2007). "Solar Energy Applications". Environmentally Conscious Alternative Energy Production. pp. 13–92. doi:10.1002/9780470209738.ch2. ISBN 9780470209738.
- ^ Schowengerdt, R. A. (2007). "Optical radiation models". Remote Sensing. pp. 45–88. doi:10.1016/B978-012369407-2/50005-X. ISBN 9780123694072.
Hour angle
View on Grokipediafrom Grokipedia
In astronomy, the hour angle (HA) of a celestial object is defined as the angular distance, measured westward along the celestial equator from the observer's local meridian to the hour circle passing through the object, typically expressed in hours, minutes, and seconds of time, with each hour corresponding to 15 degrees of arc. This coordinate quantifies the object's position relative to the observer's meridian, serving as a direct measure of the elapsed sidereal time since the object last crossed that meridian (transit), with an HA of 0 indicating the object is due south (in the Northern Hemisphere) at its highest point.[2][3]
Hour angle is a fundamental component of the equatorial coordinate system, complementing right ascension (RA) and declination to fully specify an object's position on the celestial sphere from a given location and time.[4] It is calculated as the difference between the local sidereal time (LST) and the object's right ascension: HA = LST - RA, allowing astronomers to convert between equatorial coordinates and the observer's local horizon system for tasks like telescope pointing or stellar timing.[5] In practice, hour angle varies continuously due to Earth's rotation, increasing at a rate of 15 degrees (or 1 hour) per sidereal hour, and is essential for precise observations, as objects are generally above the horizon and observable when |HA| < 6 hours (for objects with declination near 0°), spanning both before and after meridian transit.[2]
A specific variant, the Greenwich Hour Angle (GHA), measures the same angular distance but from the prime meridian at Greenwich, England, rather than the local meridian, making it a global reference for celestial navigation and ephemeris calculations.[6] This standardization facilitates worldwide coordination in fields like maritime navigation, where GHA is combined with an observer's longitude to derive the local hour angle (LHA = GHA + longitude, adjusted for east/west).[7] Overall, hour angle's role in bridging time, position, and Earth's rotation underscores its importance in both theoretical astronomy and applied geodesy.
where both terms are in the same units (hours or degrees).[33] When using degrees, the result in hours can be converted by multiplying by 15, since 360° corresponds to 24 hours.[28] To compute HA, first determine LST from Universal Time (UT), the observer's longitude, and sidereal time corrections. LST in hours is obtained by adding the longitude (in degrees, divided by 15 to convert to hours) to the Greenwich Apparent Sidereal Time (GAST), which itself is derived from UT via the Julian date, accounting for mean sidereal time and the equation of the equinoxes (a nutation correction typically on the order of seconds).[24] Once LST is available, subtract the RA (in the same units) to yield HA; normalize the result to the range 0 to 360° or 0 to 24 hours if it falls outside, by adding or subtracting 360° (or 24 hours) as needed.[28] For the solar hour angle, a variant replaces LST with local apparent solar time, but the core sidereal method applies to general stellar objects.[24] At the Greenwich meridian, the Greenwich hour angle (GHA) simplifies to GAST minus RA (in hours), or equivalently (GAST - RA) × 15 in degrees.[33] The local HA is then obtained by adding the observer's longitude if east of Greenwich or subtracting it if west (with longitude in degrees): LHA = GHA ± longitude, ensuring consistent angular units.[28] For long-term accuracy over centuries, adjustments for precession (the gradual shift of the equinox due to Earth's axial wobble) and nutation (short-period oscillations) are incorporated into the RA and sidereal time computations using models such as IAU 2006 precession and IAU 2000A nutation.[33] Precise ephemeris calculations, including these effects, are facilitated by software libraries like the Naval Observatory Vector Astrometry Software (NOVAS), which implements both equinox-based (using GST) and Celestial Intermediate Origin (CIO)-based (using Earth Rotation Angle) schemes for hour angle determination.[33]
Basic Concepts
Definition
In astronomy, the hour angle of a celestial object is defined as the dihedral angle between the observer's local celestial meridian and the hour circle passing through the object.[8] The local celestial meridian is the great circle on the celestial sphere that passes through the observer's zenith, the north celestial pole, and the south celestial pole.[9] This meridian serves as the reference plane for local observations, dividing the sky into eastern and western hemispheres from the observer's perspective. Hour circles are great circles on the celestial sphere that pass through the north and south celestial poles, functioning similarly to meridians of longitude on Earth.[3] Each celestial object lies on its own hour circle, which intersects the celestial equator at the point defined by the object's right ascension, providing a framework for equatorial coordinates. The hour angle is measured westward along the celestial equator from the local meridian, with values ranging from 0° to 360° or equivalently from -180° to +180°.[9] The term "hour" in hour angle originates from its expression in units of time, where 1 hour of sidereal time corresponds to 15° of angular displacement, based on Earth's sidereal rotation completing a full 360° in 24 hours of sidereal time.[10] This measure differs from azimuth, which quantifies direction from true north along the horizon in the horizontal coordinate system, and from declination, which denotes the angular distance north or south of the celestial equator like latitude.[9] Instead, hour angle captures the temporal progression of an object's position relative to the local meridian due to Earth's rotation.Units and Conventions
The hour angle is commonly measured in units of time—hours (h), minutes (m), and seconds (s)—with its zero point defined at the observer's local celestial meridian and increasing westward up to 24^h (equivalent to 360°) as the celestial sphere rotates due to Earth's motion.[11] This time-based convention aligns with standard astronomical practice, where 1 h = 15°, 1 m = 15', and 1 s = 15", facilitating integration with sidereal time measurements.[12] An alternative representation expresses the hour angle in angular degrees (0° to 360° or -180° to +180°), tracking the dihedral angle along the celestial equator.[7] This angular notation is used in some computational contexts but is less common than the time units, which are standardized by the International Astronomical Union (IAU) to ensure precision in observations, recommending decimal subdivisions for clarity (e.g., 06^h 19^m 05.18^s).[12] The sign convention for hour angle is positive when measured westward from the meridian, which is the predominant standard in astronomy to reflect the direction of apparent celestial motion.[7] In some contexts, negative values are used for eastward positions, particularly for computational efficiency, allowing the hour angle to range from -180° to +180° (or -12^h to +12^h) instead of the full 0° to 360° span.[13] Due to Earth's rotation, the hour angle of any celestial object increases at a rate of 15° (or 1 hour) per sidereal hour.[14] The IAU conventions further emphasize consistent use of these units to maintain accuracy across global observations.[12]Relation to Celestial Coordinates
Connection to Right Ascension
Right ascension (RA) serves as the equatorial coordinate system's analog to terrestrial longitude, quantifying a celestial object's position by measuring the angular distance eastward from the vernal equinox along the celestial equator.[9] This measurement is conventionally expressed in hours, minutes, and seconds, spanning 0 hours to 24 hours to complete a full 360-degree circle, with each hour corresponding to 15 degrees of arc.[9] The vernal equinox, where the ecliptic intersects the celestial equator, establishes the zero point for RA, providing a fixed reference frame aligned with Earth's orbital plane.[15] Hour angle (HA) functions as the local counterpart to right ascension, adapting the global equatorial coordinates to an observer's specific location on Earth by referencing the local meridian.[9] Whereas RA defines an object's absolute position in the celestial sphere, HA indicates the angular separation westward from the observer's meridian to the hour circle passing through the object, also measured in hours.[16] This transformation enables astronomers to determine an object's current position relative to the local sky, shifting the perspective from a universal stellar catalog to time- and location-dependent observations.[17] The connection between hour angle and right ascension lies in their shared use of hour circles—great circles on the celestial sphere that pass through the north and south celestial poles, analogous to meridians on Earth.[9] Right ascension delineates positions absolutely from the vernal equinox along these hour circles, offering a stable, equator-based framework independent of the observer.[15] In contrast, hour angle measures the object's offset relative to the observer's meridian, which is itself an hour circle aligned with the local zenith and celestial poles, emphasizing HA's role in bridging fixed celestial coordinates to dynamic, local viewing conditions.[16] This distinction underscores how RA provides a global "longitude" for stars, while HA localizes that coordinate for practical astronomical applications.[17]Role of Local Sidereal Time
Local sidereal time (LST) serves as the fundamental temporal reference for determining the hour angle of a celestial object, acting as the right ascension of the point on the celestial sphere that currently coincides with the observer's local meridian.[18] This equivalence enables the direct relation between hour angle (H) and right ascension (α) via the formula H = LST - α, where LST provides the dynamic coordinate of the meridian in right ascension units, allowing observers to compute an object's position relative to their local horizon as Earth rotates.[19] Without LST, the conversion from equatorial coordinates to the observer's local frame would lack the precise rotational offset required for accurate tracking.[20] LST is defined in sidereal terms because it measures Earth's rotation relative to the fixed stars, rather than the Sun, ensuring that the celestial sphere's apparent motion aligns with the 360° rotation completed in one sidereal day of approximately 23 hours 56 minutes 4 seconds of solar time.[21] This sidereal basis is essential for precise astronomical observations, as it accounts for the true rotational period against distant, effectively stationary reference points in the stellar background, avoiding distortions from Earth's orbital motion around the Sun.[22] In contrast, solar time is calibrated to the Sun's apparent daily path, which includes both Earth's rotation and its ~1° orbital advance per day, resulting in a mean solar day of 24 hours that overestimates the rotational period by about 3 minutes 56 seconds.[21] Consequently, one sidereal day corresponds exactly to a 360° rotation relative to the stars, while the solar day incorporates an additional ~0.986° due to the orbital progression.[23] The calculation of LST begins with Greenwich sidereal time (GST), which is derived from Universal Time (UT) adjusted for effects like nutation and precession to yield both mean and apparent forms.[21] LST is then obtained by adding the observer's geographic longitude in hours (with east longitudes positive and west negative) to GST, converting the longitude from degrees to time units by dividing by 15 since 15° corresponds to one hour of right ascension.[24] This adjustment localizes the Greenwich reference to the observer's meridian, providing the sidereal clock reading necessary for hour angle computations at any longitude.[23] Over each solar day, LST advances by approximately 24 hours 3 minutes 57 seconds relative to solar time, reflecting the cumulative effect of Earth's orbit that shifts the stellar backdrop westward by ~0.986° daily.[21]Types of Hour Angle
Solar Hour Angle
The solar hour angle, also denoted as , represents the angular position of the Sun relative to the observer's local meridian, serving as the specialized application of the hour angle concept to solar observations. It is defined as zero degrees at local solar noon, the moment when the Sun reaches its highest point in the sky by crossing the meridian, and increases westward at a uniform rate throughout the day. This angle ranges from -180° before noon (indicating the Sun's position in the eastern sky during morning hours) to +180° after noon (marking the Sun's progression in the western sky during the afternoon).[25] The SHA follows a daily cycle tied directly to the apparent motion of the Sun across the celestial sphere, advancing by 15° for every hour elapsed from solar noon due to Earth's rotation. It is computed using the formula where is the local solar time in hours (with solar noon at ). This relationship reflects the Sun's average diurnal path, completing a full 360° rotation relative to the meridian every 24 hours. However, the SHA deviates from uniform mean solar time because of the equation of time, a correction factor arising from Earth's elliptical orbit around the Sun (which causes variations in orbital speed) and the 23.44° axial tilt (which affects the Sun's declination). These effects result in apparent solar time—based on the true SHA—differing from mean solar time by up to about 16 minutes throughout the year, necessitating adjustments in applications requiring precise timing.[26][13] Unlike the hour angles of fixed stars, the SHA is uniquely adapted to the Sun's variable apparent motion, making it essential for timekeeping devices like sundials, which directly track apparent solar time via the shadow's alignment with the SHA. It also plays a central role in solar position algorithms, such as the Position of the Sun Algorithm (PSA), which uses inputs like latitude, longitude, and date to determine the Sun's coordinates, including the SHA, with high accuracy (typically within 0.5 arcminutes). These algorithms enable precise calculations for solar energy systems, where the SHA helps model the Sun's path for optimizing panel orientation and predicting insolation.[27]Sidereal Hour Angle
The sidereal hour angle (SHA) of a celestial object, such as a fixed star, is the angular distance measured westward along the celestial equator from the observer's local meridian to the hour circle passing through the star, computed using local sidereal time (LST) and the star's fixed right ascension (RA). It is given by the formula SHA = LST - RA, where both are expressed in hours or degrees (with 15° per hour).[28] Because stars maintain constant RA in the equatorial coordinate system relative to the fixed stars, the sidereal hour angle directly tracks the Earth's rotation without influences from orbital motion around the Sun.[21] For any given star, the sidereal hour angle completes a full cycle of 360° (or 24 hours) every sidereal day, which is the time for one rotation of Earth relative to the distant stars, lasting approximately 23 hours, 56 minutes, and 4 seconds of mean solar time.[29] The value is zero when the star transits the observer's meridian, marking the moment it crosses directly overhead or due south/north depending on declination. This cyclical behavior arises solely from Earth's rotational period against the stellar background, providing a uniform measure for tracking stellar positions over short timescales. In contrast to solar-based calculations, the sidereal hour angle incorporates no corrections for the equation of time, as it relies exclusively on sidereal time rather than apparent or mean solar time, which account for Earth's elliptical orbit and axial tilt.[13] This purity makes it essential for applications requiring high precision in rotational tracking, such as aligning and pointing telescopes to maintain stars in the field of view during observations.[30] A representative example is Polaris (α Ursae Minoris), the current North Star, which has a right ascension of 02ʰ 31ᵐ 49ˢ (J2000 epoch).[31] Its sidereal hour angle at a specific location and time, calculated as LST minus this RA, determines the star's exact azimuthal offset from the north celestial pole, aiding in polar alignment for equatorial telescope mounts to ensure accurate sidereal tracking.[32]Calculations and Applications
Computing Hour Angle
The hour angle (HA) of a celestial object is computed as the difference between the local sidereal time (LST) and the object's right ascension (RA), expressed either in hours of time or degrees:where both terms are in the same units (hours or degrees).[33] When using degrees, the result in hours can be converted by multiplying by 15, since 360° corresponds to 24 hours.[28] To compute HA, first determine LST from Universal Time (UT), the observer's longitude, and sidereal time corrections. LST in hours is obtained by adding the longitude (in degrees, divided by 15 to convert to hours) to the Greenwich Apparent Sidereal Time (GAST), which itself is derived from UT via the Julian date, accounting for mean sidereal time and the equation of the equinoxes (a nutation correction typically on the order of seconds).[24] Once LST is available, subtract the RA (in the same units) to yield HA; normalize the result to the range 0 to 360° or 0 to 24 hours if it falls outside, by adding or subtracting 360° (or 24 hours) as needed.[28] For the solar hour angle, a variant replaces LST with local apparent solar time, but the core sidereal method applies to general stellar objects.[24] At the Greenwich meridian, the Greenwich hour angle (GHA) simplifies to GAST minus RA (in hours), or equivalently (GAST - RA) × 15 in degrees.[33] The local HA is then obtained by adding the observer's longitude if east of Greenwich or subtracting it if west (with longitude in degrees): LHA = GHA ± longitude, ensuring consistent angular units.[28] For long-term accuracy over centuries, adjustments for precession (the gradual shift of the equinox due to Earth's axial wobble) and nutation (short-period oscillations) are incorporated into the RA and sidereal time computations using models such as IAU 2006 precession and IAU 2000A nutation.[33] Precise ephemeris calculations, including these effects, are facilitated by software libraries like the Naval Observatory Vector Astrometry Software (NOVAS), which implements both equinox-based (using GST) and Celestial Intermediate Origin (CIO)-based (using Earth Rotation Angle) schemes for hour angle determination.[33]
Practical Uses in Astronomy and Navigation
In astronomy, the hour angle serves as a critical coordinate for equatorial telescope mounts, where it drives the rotation axis aligned with Earth's rotational pole to track celestial objects by compensating for the planet's daily spin. This setup allows observers to maintain a star or planet in view with a single motor adjustment along the hour angle, simplifying long-exposure imaging and spectroscopic observations. For instance, in alt-azimuth conversions for pointing models, hour angle integrates with declination to achieve arcsecond precision in professional observatories.[30][9] Astronomers also employ hour angle to predict rise and set times of celestial bodies, determining when an object's altitude reaches zero by relating its position to the observer's horizon and local sidereal time. This application aids in scheduling observations, such as monitoring variable stars or exoplanet transits, where hour angle constraints ensure the target remains above the horizon during critical phases like ingress or egress. In exoplanet studies, tools filter viable transit windows based on hour angle limits, typically defaulting to ±12 hours for global observability.[34][35] In celestial navigation, hour angle enables mariners and aviators to compute latitude from sextant measurements of a body's meridian altitude, using the local hour angle to derive the observer's position relative to the celestial equator. The Nautical Almanac supplies Greenwich hour angle (GHA) values for the Sun, Moon, planets, and stars, which, when combined with longitude estimates, yield the local hour angle for sight reduction tables and line-of-position fixes. Historically, this principle underpinned longitude determination with marine chronometers, as the difference between local and Greenwich hour angles—measured via timepieces—revealed east-west displacement from the prime meridian, revolutionizing transoceanic voyages in the 18th and 19th centuries.[36][37] For solar energy systems, the solar hour angle informs photovoltaic panel orientation models by quantifying the Sun's eastward or westward deviation from the local meridian, with maximum direct irradiance occurring at zero hour angle during solar noon. Engineers adjust panel tilt and azimuth based on this angle to optimize annual energy yield, as seen in tracking algorithms that align modules for peak power output in regions like latitudes around 25°N.[38] Although GPS has diminished reliance on hour angle for routine navigation, it persists in specialized applications like satellite tracking, where NASA's Deep Space Network uses hour angle-declination coordinates to point antennas at spacecraft, ensuring continuous communication despite Earth's rotation. Similarly, in exoplanet timing, hour angle refines observation schedules for transit variations, supporting precise orbital period analyses.[9][35]References
- https://science.[nasa](/page/NASA).gov/learn/basics-of-space-flight/chapter2-2/