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In astronomy, an epoch is a moment in time for which something is specified that can vary, such as the position or the orbital elements of a celestial body. Astronomy (from the Greek words astron (ἄστρον "star" and nomos (νόμος "law" is the scientific study The elements of an orbit are the parameters needed to specify that Orbit uniquely given a model of two point-masses obeying the Newtonian laws of motion and the s are significant physical entities, associations or structures which current Science has confirmed to exist in Space. Typically, the epoch is either the moment that the observations were made or the moment for which the predictions were calculated.

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Epoch versus equinox

Coordinates are incomplete without a specification of the used coordinate system. In Mathematics and its applications a coordinate system is a system for assigning an n - Tuple of Numbers or scalars to each point The most common celestial coordinate systems are equatorial coordinates and ecliptic coordinates. The equatorial coordinate system is probably the most widely used Celestial coordinate system, whose equatorial coordinates are Declination (\delta The ecliptic coordinate system is a Celestial coordinate system that uses the Ecliptic for its Fundamental plane. These are tied to the position of the vernal equinox, which itself is linked to the orientations of the Earth's rotation axis and orbit around the Sun. An equinox is the event of the Sun passing over the Earth's equator in its annual cycle EARTH was a short-lived Japanese vocal trio which released 6 singles and 1 album between 2000 and 2001 The Sun (Sol is the Star at the center of the Solar System. These orientations vary (though slowly, e. g. due to precession), so there is an infinite number of such coordinate systems. Precession refers to a change in the direction of the axis of a rotating object Infinity (symbolically represented with ∞) comes from the Latin infinitas or "unboundedness Each is defined by the moment at which the coordinate system really fits the orientations of the Earth's rotation axis and orbit around the Sun. EARTH was a short-lived Japanese vocal trio which released 6 singles and 1 album between 2000 and 2001 The Sun (Sol is the Star at the center of the Solar System. That moment is called the equinox.

The equinox defines (partly) which coordinate system is used. The epoch defines (completely) at which moment the observations or predictions are valid. A particular coordinate system (equinox) could be used forever, but a set of predictions for a particular date (epoch) will be (approximately) valid for only a limited time.

For example, the boundaries of the IAU constellations are specified relative to an equinox from near the beginning of the year 1875. In common usage a constellation is a group of celestial bodies that are connected together in some arrangement typically stars to form a visible figure or picture To find out in which constellation a particular comet stands today, the current position of that comet must be expressed in the coordinate system of 1875 (epoch = now, equinox = 1875). That coordinate system can still be used today, while hardly any predictions made originally for 1875 (epoch = 1875) are still useful today.

Equinox of the date means that the equinox is the same as the epoch.

Why switch to another standard equinox and epoch?

Calculation of celestial object visibility to an observer at a specific location on Earth requires the equatorial coordinates of the object, relative to the equinox of the date. If the coordinates relative to some other equinox are used, then that will cause errors in the results. The magnitude of those errors increases with the time difference compared to the equinox of the date, because of precession of the equinoxes. If the time difference is small, then fairly easy and small corrections for the precession suffice. If the time difference gets large, then tedious, complicated corrections must be applied. So, a stellar position read from a star atlas or catalog that is based on a sufficiently old equinox cannot be used without corrections, if reasonable accuracy is required.

Additionally, star positions change even if the coordinate system does not, because the stars move relative to each other through space. Apparent motion across the sky relative to other stars is called proper motion. The proper motion of a Star is the measurement of its change in position in the sky over time after Improper motions are accounted for Most stars have very small proper motions, but a few have proper motions that accumulate to noticeable distances after a few tens of years. So, some stellar positions read from a star atlas or catalog for a sufficiently old epoch require proper motion corrections, for reasonable accuracy.

Because of precession and proper motion, star positions become less useful as their equinox and epoch get older. After a while, it is easier to switch to a newer epoch and equinox than to keep applying the corrections to the data from the older epoch and equinox.

Ways to specify an epoch or equinox

Epochs and equinoxes are moments in time, so they can be specified in the same way as moments that indicate things other than epochs and equinoxes. The following standard ways of specifying epochs and equinoxes seem most popular:

All three of these are expressed in TT = Terrestrial Time. Terrestrial Time (TT is the modern astronomical standard for the passage of time on the surface of the Earth (for civil purposes Coordinated Universal

Besselian and Julian years are not often used to specify an epoch, except for things that vary very slowly, such as star positions. For example, the Hipparcos catalog summary[1] defines the 'catalog epoch' to be equal to J1991. Hipparcos (an Acronym for Hi gh P recision Par allax Co llecting S atellite) was an Astrometry mission 25, which is in terms of Julian years.

Besselian years

A Besselian year is named after the German mathematician and astronomer Friedrich Bessel (1784 – 1846). Friedrich Wilhelm Bessel (22 July 1784 &ndash 17 March 1846 was a German Mathematician, Astronomer, and systematizer of the Bessel functions Meeus[2] defines the beginning of a Besselian year to be the moment at which the mean longitude of the Sun, including the effect of aberration and measured from the mean equinox of the date, is exactly 280 degrees. In Astrodynamics or Celestial dynamics mean longitude is the Longitude at which an orbiting body could be found if its orbit were circular and This moment falls near the beginning of the corresponding Gregorian year. A year (from Old English gēr) is the time between two recurrences of an event related to the Orbit of the Earth around the Sun Unfortunately, the orbit of the Earth around the Sun is not entirely fixed, so the length of the Besselian year according to this definition is not constant. This makes Besselian years somewhat difficult to work with.

Lieske[3] says that a 'Besselian epoch' can be calculated from the Julian date according to

B = 1900. 0 + (Julian date − 2415020. 31352) / 365. 242198781

This relationship is included in the SOFA software library[4], which implies endorsement by the IAU. The SOFA (Standards of Fundamental Astronomy software libraries are a collection of subroutines that implement official IAU algorithms for astronomical computations

Lieske's definition is not consistent with the earlier definition in terms of the mean longitude of the Sun. When using Besselian years, specify which definition is being used.

To distinguish between calendar years and Besselian years, it became customary to add '. 0' to the Besselian years. Since the switch to Julian years in the mid-1980s, it has become customary to prefix 'B' to Besselian years. So, '1950' is the calendar year 1950, and '1950. 0' = 'B1950. 0' is the beginning of Besselian year 1950.

According to Meeus, and also according to the formula given above,

B1900. 0


B1950. 0


Julian years

A Julian year, named after Julius Caesar (100 BC — 44 BC), is a year of exactly 365. 25 days. Julian year 2000 began on 2000 January 1 at exactly 12:00 TT. The beginning of Julian years are indicated with prefix 'J' and suffix '. 0', for example 'J2000. 0' for the beginning of Julian year 2000.

Because Julian years have a fixed length, their beginning is far easier to calculate than that of Besselian years.

The IAU decided at their General Assembly of 1976[5] that the new standard equinox of J2000. 0 should be used starting in 1984. (Before that, the equinox of B1950. 0 seems to have been the standard. ) If the past is a good guide, then we may expect to switch to J2050. 0 in the mid-2030s.

Julian epochs are calculated according to:

J = 2000. 0 + (Julian date − 2451545. 0)/365. 25

J2000. 0


J2000. 0 is precisely Julian date 2451545. 0 TT (Terrestrial Time), or January 1, 2000, noon TT. This is equivalent to January 1, 2000, 11:59:27. 816 TAI or January 1, 2000, 11:58:55. International Atomic Time ( TAI, from the French name Temps Atomique International) is a high-precision atomic Time standard that tracks 816 UTC.

See also

References

  1. ^ "The Hipparcos and Tycho Catalogues", ESA SP-1200, Vol. In Astronomy, equinox is a moment in time at which the vernal point Celestial equator, and other such elements are taken to be used in the definition of a The International Celestial Reference System (ICRS is the current standard celestial reference system adopted by the International Astronomical Union (IAU The International Celestial Reference Frame (ICRF is a quasi- Inertial reference frame centered at the Barycenter of the Solar System, defined by the measured Astrometry is the branch of Astronomy that relates to precise measurements and explanations of the positions and movements of Stars and other celestial bodies 1, page XV. ESA, 1997
  2. ^ Meeus, J. : "Astronomical Algorithms", page 125. Willmann-Bell, 1991
  3. ^ Lieske, J. H. : "Precession Matrix Based on IAU (1976) System of Astronomical Constants", page 282. Astronomy & Astrophysics, 73, 282-284 (1979)
  4. ^ http://www.iau-sofa.rl.ac.uk/, issue 2007-08-10, revised 2007-08-28 (downloaded 2007-12-02)
  5. ^ S. Aoki, et al. , "Conversion matrix of epoch B 1950. 0 FK 4-based positions of stars to epoch J 2000. 0 positions in accordance with the new IAU resolutions", page 263. Astron. Astrophys. 128(2), 263–267, (1983)

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