KPL/LSK

LEAPSECONDS KERNEL FILE

===========================================================================

Modifications:

--------------

2016, Jul. 14 NJB Modified file to account for the leapsecond that

will occur on December 31, 2016.

2015, Jan. 5 NJB Modified file to account for the leapsecond that

will occur on June 30, 2015.

2012, Jan. 5 NJB Modified file to account for the leapsecond that

will occur on June 30, 2012.

2008, Jul. 7 NJB Modified file to account for the leapsecond that

will occur on December 31, 2008.

2005, Aug. 3 NJB Modified file to account for the leapsecond that

will occur on December 31, 2005.

1998, Jul 17 WLT Modified file to account for the leapsecond that

will occur on December 31, 1998.

1997, Feb 22 WLT Modified file to account for the leapsecond that

will occur on June 30, 1997.

1995, Dec 14 KSZ Corrected date of last leapsecond from 1-1-95

to 1-1-96.

1995, Oct 25 WLT Modified file to account for the leapsecond that

will occur on Dec 31, 1995.

1994, Jun 16 WLT Modified file to account for the leapsecond on

June 30, 1994.

1993, Feb. 22 CHA Modified file to account for the leapsecond on

June 30, 1993.

1992, Mar. 6 HAN Modified file to account for the leapsecond on

June 30, 1992.

1990, Oct. 8 HAN Modified file to account for the leapsecond on

Dec. 31, 1990.

Explanation:

------------

The contents of this file are used by the routine DELTET to compute the

time difference

[1] DELTA_ET = ET - UTC

the increment to be applied to UTC to give ET.

The difference between UTC and TAI,

[2] DELTA_AT = TAI - UTC

is always an integral number of seconds. The value of DELTA_AT was 10

seconds in January 1972, and increases by one each time a leap second

is declared. Combining [1] and [2] gives

[3] DELTA_ET = ET - (TAI - DELTA_AT)

= (ET - TAI) + DELTA_AT

The difference (ET - TAI) is periodic, and is given by

[4] ET - TAI = DELTA_T_A + K sin E

where DELTA_T_A and K are constant, and E is the eccentric anomaly of the

heliocentric orbit of the Earth-Moon barycenter. Equation [4], which ignores

small-period fluctuations, is accurate to about 0.000030 seconds.

The eccentric anomaly E is given by

[5] E = M + EB sin M

where M is the mean anomaly, which in turn is given by

[6] M = M + M t

0 1

where t is the number of ephemeris seconds past J2000.

Thus, in order to compute DELTA_ET, the following items are necessary.

DELTA_TA

K

EB

M0

M1

DELTA_AT after each leap second.

The numbers, and the formulation, are taken from the following sources.

1) Moyer, T.D., Transformation from Proper Time on Earth to

Coordinate Time in Solar System Barycentric Space-Time Frame

of Reference, Parts 1 and 2, Celestial Mechanics 23 (1981),

33-56 and 57-68.

2) Moyer, T.D., Effects of Conversion to the J2000 Astronomical

Reference System on Algorithms for Computing Time Differences

and Clock Rates, JPL IOM 314.5--942, 1 October 1985.

The variable names used above are consistent with those used in the

Astronomical Almanac.

\begindata

DELTET/DELTA_T_A = 32.184

DELTET/K = 1.657D-3

DELTET/EB = 1.671D-2

DELTET/M = ( 6.239996D0 1.99096871D-7 )

DELTET/DELTA_AT = ( 10, @1972-JAN-1

11, @1972-JUL-1

12, @1973-JAN-1

13, @1974-JAN-1

14, @1975-JAN-1

15, @1976-JAN-1

16, @1977-JAN-1

17, @1978-JAN-1

18, @1979-JAN-1

19, @1980-JAN-1

20, @1981-JUL-1

21, @1982-JUL-1

22, @1983-JUL-1

23, @1985-JUL-1

24, @1988-JAN-1

25, @1990-JAN-1

26, @1991-JAN-1

27, @1992-JUL-1

28, @1993-JUL-1

29, @1994-JUL-1

30, @1996-JAN-1

31, @1997-JUL-1

32, @1999-JAN-1

33, @2006-JAN-1

34, @2009-JAN-1

35, @2012-JUL-1

36, @2015-JUL-1

37, @2017-JAN-1 )

\begintext