Title: Apsis
Content:  Orbital elements such as the time of perihelion passage are defined at the epoch chosen using an unperturbed two-body solution that does not account for the n-body problem. To get an accurate time of perihelion passage you need to use an epoch close to the perihelion passage. For example, using an epoch of 1996, Comet Hale–Bopp shows perihelion on 1 April 1997. Using an epoch of 2008 shows a less accurate perihelion date of 30 March 1997. Short-period comets can be even more sensitive to the epoch selected. Using an epoch of 2005 shows 101P/Chernykh coming to perihelion on 25 December 2005, but using an epoch of 2012 produces a less accurate unperturbed perihelion date of 20 January 2006. Numerical integration shows dwarf planet Eris will come to perihelion around December 2257. Using an epoch of 2021, which is 236 years early, less accurately shows Eris coming to perihelion is 2260. 4 Vesta comes to perihelion on 26 December 2021, but using a two-body solution at an epoch of July 2021 less accurately shows Vesta coming to perihelion on 25 December 2021.
Title: Epoch (astronomy)
Content:  . . . Incl .. 24.66109 where the epoch is expressed in terms of Terrestrial Time, with an equivalent Julian date. Four of the elements are independent of any particular coordinate system: M is mean anomaly (deg), n: mean daily motion (deg/d), a: size of semi-major axis (AU), e: eccentricity (dimensionless). But the argument of perihelion, longitude of the ascending node and the inclination are all coordinate-dependent, and are specified relative to the reference frame of the equinox and ecliptic of another date "2000.0", otherwise known as J2000, i.e. January 1.5, 2000 (12h on January 1) or JD 2451545.0.
Title: Declination
Content:   The Earth's axis rotates slowly westward about the poles of the ecliptic, completing one circuit in about 26,000 years. This effect, known as precession, causes the coordinates of stationary celestial objects to change continuously, if rather slowly. Therefore, equatorial coordinates (including declination) are inherently relative to the year of their observation, and astronomers specify them with reference to a particular year, known as an epoch. Coordinates from different epochs must be mathematically rotated to match each other, or to match a standard 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.
Title: 1713 Bancilhon
Content:  Bancilhon orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 4 months (1,215 days). Its orbit has an eccentricity of 0.18 and an inclination of 4° with respect to the ecliptic. It was first identified as at Lowell Observatory in 1931, extending the body's observation arc by 20 years prior to its official discovery observation.
Title: Julian year (astronomy)
Content:  In astronomy, an epoch specifies a precise moment in time. The positions of celestial objects and events, as measured from Earth, change over time, so when measuring or predicting celestial positions, the epoch to which they pertain must be specified. A new standard epoch is chosen about every 50 years. The standard epoch in use today is Julian epoch J2000.0. It is exactly 12:00 TT (close to but not exactly Greenwich mean noon) on January 1, 2000 in the Gregorian (not Julian) calendar. Julian within its name indicates that other Julian epochs can be a number of Julian years of 365.25 days each before or 
Title: Epoch (astronomy)
Content: B = 1900.0 + (Julian date − 2415020.31352) / 365.242198781 The IAU constellation boundaries are defined in the equatorial coordinate system relative to the equinox of B1875.0. ; The Henry Draper Catalog uses the equinox B1900.0. ; The classical star atlas Tabulae Caelestes used B1925.0 as its equinox. B1900.0 = JDE 2415020.3135 = 1900 January 0.8135 TT ; B1950.0 = JDE 2433282.4235 = 1950 January 0.9235 TT A Besselian year is named after the German mathematician and astronomer Friedrich Bessel (1784–1846). 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. This moment falls near the beginning of the corresponding Gregorian year. The definition depended on a particular theory of the orbit 
Title: Epoch (astronomy)
Content:  quoted to 1 or 2 decimal places, has come to mean a date that is an interval of x Julian years of 365.25 days away from the epoch J2000 = JD 2451545.0 (TT), still corresponding (in spite of the use of the prefix "J" or word "Julian") to the Gregorian calendar date of January 1, 2000, at 12h TT (about 64 seconds before noon UTC on the same calendar day). (See also Julian year (astronomy).) Like the Besselian epoch, an arbitrary Julian epoch is therefore related to the Julian date by  J = 2000 + (Julian date − 2451545.0) ÷ 
Title: Equinox (celestial coordinates)
Content: B = 1900.0 + (Julian date − 2415020.31352) / 365.242198781 A Besselian epoch, named after German mathematician and astronomer Friedrich Bessel (1784–1846), is an epoch that is based on a Besselian year of 365.242198781 days, which is a tropical year measured at the point where the Sun's longitude is exactly 280°. Since 1984, Besselian equinoxes and epochs have been superseded by Julian equinoxes and epochs. The current standard equinox and epoch is J2000.0, which is a Julian epoch. Besselian epochs are calculated according to:  The previous standard equinox and epoch were B1950.0, a Besselian epoch. Since the right ascension and declination of stars are constantly changing due to precession, astronomers always specify these with reference to a particular equinox. Historically used Besselian equinoxes include B1875.0, B1900.0, B1925.0 and B1950.0. The official constellation boundaries were defined in 1930 using B1875.0.
Title: Ecliptic
Content:  ecliptic coordinates of objects on the celestial sphere are continuously changing. Specifying a position in ecliptic coordinates requires specifying a particular equinox, that is, the equinox of a particular date, known as an epoch; the coordinates are referred to the direction of the equinox at that date. For instance, the Astronomical Almanac lists the heliocentric position of Mars at 0h Terrestrial Time, 4 January 2010 as: longitude 118°09′15.8″, latitude +1°43′16.7″, true heliocentric distance 1.6302454 AU, mean equinox and ecliptic of date. This specifies the mean equinox of 4 January 2010 0h TT as above, without the addition of nutation.
Title: Equinox (celestial coordinates)
Content: The Bonner Durchmusterung started by Friedrich Wilhelm August Argelander uses B1855.0 ; The Henry Draper Catalog uses B1900.0 ; Constellation boundaries were defined in 1930 along lines of right ascension and declination for the B1875.0 epoch. ; Occasionally, non-standard equinoxes have been used, such as B1925.0 and B1970.0 ; The Hipparcos Catalog uses the International Celestial Reference System (ICRS) coordinate system (which is essentially equinox J2000.0) but uses an epoch of J1991.25. For objects with a significant proper motion, assuming that the epoch is J2000.0 leads to a large position error.  Assuming that the equinox is J1991.25 leads to a large error for nearly all objects. Gregorian date with 24-hour time: 2000 January 1, 12:00 TT ; Gregorian date with fractional day: 2000 January 1.5 TT ; Julian day with fractional day: JDT 2451545.0 ; NASA/NORAD's Two-line elements format with fractional day: 00001.50000000 Other equinoxes and epochs that have been used include: Epochs and equinoxes for orbital elements are usually given in Terrestrial Time, in several different formats, including:

Question: Verify the following claims with "True" or "False": The epoch of a planet, formely known as Collegium Carolinum, is 31 December 2006 and it has an orbital period of 183309000.0.
Answer: False