Altitude (astronomy)

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## Definition

## General observations

## See also

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This article uses material from the Wikipedia page available here. It is released under the Creative Commons Attribution-Share-Alike License 3.0.

Altitude Astronomy

The **horizontal coordinate system**, also known as **topocentric coordinate system**, is a celestial coordinate system that uses the observer's local horizon as the fundamental plane. Coordinates of an object in the sky are expressed in terms of altitude (or elevation) angle and azimuth.

This celestial coordinate system divides the sky into two hemispheres: the upper hemisphere, where objects above the horizon are visible, and the lower hemisphere, where objects below the horizon cannot be seen, since the Earth obstructs views of them. The great circle separating the hemispheres is called the **celestial horizon**, which is defined as the great circle on the celestial sphere whose plane is normal to the local gravity vector.^{[1]} In practice, the horizon can be defined as the plane tangent to a still liquid surface, such as a pool of mercury.^{[2]} The pole of the upper hemisphere is called the zenith. The pole of the lower hemisphere is called the nadir.^{[3]}

The following are two independent horizontal angular coordinates:

- Altitude (alt.), sometimes referred to as elevation (el.), is the angle between the object and the observer's local horizon. For visible objects, it is an angle between 0° and 90°.
- Alternatively, zenith distance may be used instead of altitude. The zenith distance is the complement of altitude, so that the sum of the altitude and the zenith distance is 90°.

- Azimuth (az.) is the angle of the object around the horizon, usually measured from true north and increasing eastward. Exceptions are, for example, ESO's FITS convention where it is measured from the south and increasing westward, or the FITS convention of the Sloan Digital Sky Survey where it is measured from the south and increasing eastward.

The horizontal coordinate system is sometimes called other names, such as the **az/el system**,^{[4]} the **alt/az system**, or the **alt-azimuth system**, from the name of the mount used for telescopes, whose two axes follow altitude and azimuth.^{[5]}

The horizontal coordinate system is fixed to a location on Earth, not the stars. Therefore, the altitude and azimuth of an object in the sky changes with time, as the object appears to drift across the sky with Earth's rotation. In addition, since the horizontal system is defined by the observer's local horizon, the same object viewed from different locations on Earth at the same time will have different values of altitude and azimuth.

Horizontal coordinates are very useful for determining the rise and set times of an object in the sky. When an object's altitude is 0°, it is on the horizon. If at that moment its altitude is increasing, it is rising, but if its altitude is decreasing, it is setting. However, all objects on the celestial sphere are subject to diurnal motion, which always appears to be westward.

A northern observer can determine whether altitude is increasing or decreasing by instead considering the azimuth of the celestial object:

- If the azimuth is between 0° and 180° (north-east-south), the object is rising.
- If the azimuth is between 180° and 360° (south-west-north), the object is setting.

There are the following special cases:

- All directions are south when viewed from the North Pole, and all directions are north when viewed from the South Pole, so the azimuth is undefined in both locations. When viewed from either pole, a star (or any object with fixed equatorial coordinates) has constant altitude and thus never rises or sets. The Sun, Moon, and planets can rise or set over the span of a year when viewed from the poles because their declinations are constantly changing.
- When viewed from the Equator, objects on the celestial poles stay at fixed points on the horizon.

Note that the above considerations are strictly speaking true for the *geometric* horizon only. That is, the horizon as it would appear for an observer at sea level on a perfectly smooth Earth without an atmosphere. In practice, the *apparent* horizon has a slight negative altitude due to the curvature of Earth, the value of which gets more negative as the observer ascends higher above sea level. In addition, atmospheric refraction causes celestial objects very close to the horizon to appear about half a degree higher than they would if there were no atmosphere.

**^**Clarke, A.E. Roy, D. (2003).*Astronomy principles and practice*(PDF) (4th. ed.). Bristol: Institute of Physics Pub. p. 59. ISBN 9780750309172. Retrieved 2018.**^**Young, Andrew T.; Kattawar, George W.; Parviainen, Pekka (1997). "Sunset science. I. The mock mirage".*Applied Optics*.**36**(12): 2689-2700. Bibcode:1997ApOpt..36.2689Y. doi:10.1364/ao.36.002689.**^**Schombert, James. "Earth Coordinate System". University of Oregon Department of Physics. Retrieved 2011.**^**hawaii.edu**^**"horizon system".*Encyclopædia Britannica*.

This article uses material from the Wikipedia page available here. It is released under the Creative Commons Attribution-Share-Alike License 3.0.

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