Right ascension

related topics
{math, energy, light}
{line, north, south}
{day, year, event}
{mi², represent, 1st}

Right ascension (abbrev. RA; symbol α) is the astronomical term for one of the two coordinates of a point on the celestial sphere when using the equatorial coordinate system. The other coordinate is the declination.

Contents

Explanation

Right ascension is the celestial equivalent of terrestrial longitude. Both right ascension and longitude measure an angle that increases toward the east as measured from a zero point on an equator. For longitude, the zero point is the Prime Meridian on the geographic equator; for right ascension, the zero point is known as the first point of Aries, which is the place in the sky where the Sun crosses the celestial equator at the March equinox.

Any units of angular measure can be used for right ascension, but it is customarily measured in hours, minutes, and seconds, with 24 hours being equivalent to a full circle. The reason for this choice is that the earth rotates at an approximately constant rate (see sidereal time). Since a complete circle has 360 degrees, an hour of right ascension is equal to 124 of this, or 15 degrees of arc, a single minute of right ascension equal to 15 minutes of arc, and a second of right ascension equal to 15 seconds of arc. Sidereal hour angle, used in celestial navigation, is similar to right ascension, but increases westward rather than eastward. It is important not to confuse sidereal hour angle with the astronomical concept of hour angle, which is how far west an object is from one's local meridian.

Right ascension can be used to determine a star's location and to determine how long it will take for a star to reach a certain point in the sky. For example, if a star with RA = 01:30:00 is at a location's meridian, then a star with RA = 20:00:00 will be in the meridian 18.5 sidereal hours later.

The tilt of the Earth's axis gradually rotates over time. This effect, known as precession, causes the measured right ascension and declination of even a perfectly stationary celestial object to change noticeably over the span of decades. Therefore, equatorial coordinates are inherently relative to the year of their observation. Astronomers always specify equatorial coordinates with reference to a particular epoch. An astronomer comparing coordinates from different epochs must mathematically rotate one of the coordinate systems to match the other, or rotate both to match a common epoch.

The currently used standard epoch is J2000.0, which is January 1, 2000 at 12:00 TT. The prefix "J" indicates that it is a Julian epoch. Prior to J2000.0, astronomers used the successive Besselian Epochs B1875.0, B1900.0, and B1950.0.

Full article ▸

related documents
Celestial coordinate system
Planetary ring
Theory of relativity
Adrastea (moon)
Analemma
Wave impedance
Antihydrogen
Intensity (physics)
Principle of relativity
Plum pudding model
Azimuth
Dioptre
Conservative force
Mirror image
Apsis
Quantum Hall effect
Nemesis (star)
Giant impact hypothesis
Cycloid
Ampere
Interstellar cloud
Electro-optic modulator
Gyrocompass
Hoag's Object
Rhea (moon)
Murray Gell-Mann
Polaris
South Atlantic Anomaly
Radiation pressure
Deimos (moon)