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Transit and Culmination

The culmination of a celestial body means that the body is at its greatest altitude, whereas the transit is the passage of its center through the meridian.

Only the fixed stars culminate really in the meridian. The Sun, Moon, and the planets culminate out of the meridian.
At mid-latitudes (50) the difference may be up to 18 seconds for the Sun, and more than 6 minutes for the Moon.


To compute the difference in time between transit and culmination we start by the well known equation
  altitude        (1)
    h = altitude
    δ = declination
    Φ = latitude
    H = hour angle = Local Sidereal Time - Right Ascension

Differentiating the above equation with respect to time:
derivative        (2)
At the instant of culmination we have h.  If  declination (constant declination) the culmination is at H=0.

For non constant declination the hour angle of culmination HC is very small
hour
                              angle transit culmination
and we get as an approximation of (2):
       (3)

The altitude at culmination is by h greater than the altitude on the meridian:

altitude culmination transit      (4)


The Sun
In (3) the derivative deltapunkt may be replaced by differentiating the classical equation
declination       (5)
    β = ecliptic latitude
    γ = obliquity of the ecliptic
    L = ecliptic longitude
The ecliptic latitude β of the Sun is very small: | β |<0.0002, beta, cos β=1, and therefore from (5):
Sun Moon
Equation (3) then becomes:

          (6)

L = heliocentric ecliptic longitude
H = hour angle = Local Sidereal Time - Right Ascension
γ
= obliquity of the ecliptic = 23.44
δ = declination
Φ = latitude

For the Sun the rates of change in time (derivatives) of L and H can be approximated by:

Maximum Transit Culmination difference

For equinoxes (δ=0, L=0, L=180) HK is an extremum:

Sun
                                                          transit
                                                          culmination
                                                          time
      (7)

At Φ = 40 we get HC = 9,1410-4 rad = 0,0524 = 0.210 min = 12.6 s

At Φ = 50 we get HC = 1,3010-3 rad = 0,0744 = 0.298 min = 17.9 s
The altitude at culmination is only 0.14'' more than at transit.

For solstices (L=90, L=270) HC = 0.

Between winter solstice and summer solstice culmination occurs later then transit, between summer solstice and winter solstice culmination occurs earlier then transit.


time difference transit culmination Sun
horizontal axis: day of the year
vertical axis: time difference in seconds between culmination and transit
red: latitude Φ = 40blue: latitude Φ = 50.

In NavList the following formula for the difference can be found (as a first order approximation):

T = (48/PI)*(tanΦ-tanδ)*(vLat-vDec)    (8)

    ∆T = difference is seconds of time between culmination and meridian transit

On 2012, Mar 20 at 05:14 UT (spring equinox):
    vLat = hourly latitude speed is arcminutes per hour = 0 (observer at rest)
    vDec = hourly declination change declination is arcminutes per hour = -0,988 arcmin/hour
    δ = 0.0
    at Φ = 50:
T = 18.0 s

This result agrees with (7).

***

The Moon

The orbital plane of the Moon is inclined (| β |< 5.1) aganst the ecliptic, and formula (6) is not valid.

On 2024, Oct 15 at 50N, 0E (computed by MICA, Multiyear Interactive Computer Almanac by USNO) there is an extreme value of difference:

    culmination    22:31:14.5 UT
    transit           22:25:19.3 UT
    difference      5 min 55 s

The result from calsky is  6 min 03 s.      

On 2024, Oct 15 at 22:30 UT we apply the formula (3) for the Moon using MICA:
   
deltapunkt = dδ/dt = 0.303/hour
    dH/dt = 14.56/hour
    δ = 0.00
    HC = 0.0248 rad = 1.42 = 5.68 min

HC = 5 min 41 s

The NavList formula, derived by Wilson, writes:

T = [10800/(PI*(dH/dt)2)]*(tanΦ-tanδ)*(vLat-vDec)       (9)

    ∆T = difference is seconds of time between culmination and meridian transit
    ∆H/dt = hourly change of hour angle, H in degrees
  
vLat = hourly latitude speed of the observer is arcminutes per hour

For the Moon:

14.38/hour dH/dt < 14.61/hour
mean: 14.495/hour = 360/24h 50min
16.105 hour2/ < 10800/[PI*(dH/dt)2] < 16.625 hour2/
mean: 10800/[PI*(dH/dt)2] = 16.365 hour2/

On 2024, Oct 15 at 22:30 UT using MICA:
    vLat = 0 (observer is at rest)
   
vDec = hourly declination change deltapunkt in arcminutes per hour = 18.19 arcmin/hour =         = (18.19/60) /hour
    δ = 0.025
   
dH/dt = 14.49/hour
    10800/[PI*(dH/dt)2] = 16.37 hour2/ = 16.37 hour60 s/

T = 355 s = 5 min 55 s


Moon Transit Culmination 2012
Vertical axis: Difference T = tTrans - tCulm (minutes) at 50N
horizontal axis: day in May-Jun 2012
computed by my Planet applet



Urs Klaeger pointed out to me:
With increasing declinations AND at geo-latitudes north of the subsolar/sublunar point, Culmination is after Transit. Vice versa south of the Sun/Moon.


Jean Meeus writes:
If culmination occurs south of the zenith and
δ is positive, the highest altitude is reached after the meridian passage; if the culmination occurs between the pole and the zenith, the situation is reversed.
(More Mathematical Astronomy Morsels, page 320)

Moon Transit
                                            Culmination
Moon
at 50N, May-Jun 2012: daily change of declination (δ),
and ∆T = tTrans - tCulm (minutes)

e.g. on May 10:
δ>0, and ∆T<0: culmination is after transit,

Moon
                              transit culmination difference time 2012
horizontal axis: day of the year 2012
vertical axis: time difference in seconds between culmination and transit
latitude Φ = 50
computed by my Planet applet

Transit Culmination 2015 lunar
                              standstill
Vertical axis: Difference tTrans - tCulm (minutes) at 50N 0E
horizontal axis: day in Sep-Oct 2015
computed by my Planet applet


lunar standstill 2024
Vertical axis: Difference tTrans - tCulm (minutes) at 50N 0E
horizontal axis: day in Sep-Oct 2024
computed by my Planet Applet


It seems that the variation of T is dominated by the 18.6-year cycle of lunar standstills:
small values of T (up to 4 minutes) are occuring in years of minor lunar standstills (1996, 2015), and large values (more than 6 minutes) in years of major lunar standstills (2006, 2024/2025).

Max. declination in 2024 on Sep 24 at 17 UT:    28.70
Min.  declination in 2024 on Oct 09  at 12 UT:   -28.70
Change in declination: 
-14.22 arcmin/h < deltapunkt< 18.21 arcmin/h

Max. declination in 2015 on Jan 03 at 18 UT:    18.65
Min. declination  in 2015 on Jan 18 at 06 UT:    -18.58
Change in declination:  -9.42 arcmin/h < deltapunkt< 11.64 arcmin/h


2006 (major lunar standstill) Aug 10, 50N, 0E
    transit            00:40:34 UT
    culmination     00:46:48 UT
       ∆T = 6 min 14 s
Planet Applet:
    transit            00:40:34 UT
    culmination     00:46:49 UT
       ∆T = 6 min 15 s
calsky:
    transit:             00h 40m 34.2s UT
    culmination:      00h 46.9m UT
      ∆T = 6 min 20 s
StarryNight SN7 CSAP
    transit:             00h 40m 34.2s UT  
    culmination:      00h 46.8m UT
     T = 6 min 15 s

The altitude at culmination is only 0.81' more than at transit.

by formula (3) and MICA:
    deltapunkt = dδ/dt = -0,2585/hour
    dH/dt = 14.45/hour
    δ = -15.55
     ∆T = 6 min 02 s


delta
                                            Declination
Vertical axis: hourly change of Declination (degrees)
horizontal axis: day in Sep-Oct 2015
minor lunar standstill


declination
Vertical axis: hourly change of Declination (degrees)
horizontal axis: day in Sep-Oct 2024
major lunar standstill


The result by formula (3) or formula (8) will be large for northern latitudes, if δ<0,
and if |
deltapunkt|is large. dH/dt is nearly constant (14.38/hour to 14.61/hour).


The Planets

As an example transit and culmination of Mars at 50N, 0E:

Mars, 2012 May 25 (computed by MICA):
    Transit            18:41:50 UT, 18:41:51.2 UT
    Culmination     18:41:43 UT, 18:41:45 UT
 
      ∆T = 7 s

Mars, 2012 May 25 (computed by StarryNight):
    Transit            18:41:50 UT, 18:41:51.2 UT
    Culmination     18:41:43 UT, 18:41:44.5 UT
 
      ∆T = 6,7 s

 
Mars, 2012 Aug 01 (computed by MICA):
    Transit            16:17:38 UT
    Culmination     16:17:26 UT
      ∆T = 12 s

Mars, 2012 Aug 01 (computed by StarryNight):
    Transit            16:17:38 UT, 16:17:40.7 UT
    Culmination     16:17:26 UT, 16:17:28.5 UT
      ∆T = 12.2 s
 
Mars, 2013 Apr 01 (computed by MICA):
    Transit            12:18:20 UT
    Culmination     12:18:34 UT
      ∆T = 14 s

Mars, 2013 Apr 01 (computed by StarryNight):
    Transit            12:18:20 UT, 12:18:22.9 UT
    Culmination     12:18:34 UT, 12:18:36 UT
      ∆T = 13.1 s


Body dH/dt in /hour
10800/(dH/dt)2 in hour2/
Sun 15 48
Planets 15 + deltapunkt 47.89
Stars 15.04 47.73
Moon 14.32 + deltapunkt 50.74 - 52.07

Table from Wilson


factor

Using the diagram above to get T for the Sun, look up the value of F (depending on latitude and declination), and multiply F by the hourly declination change deltapunkt in arcminutes per hour:
Φ = 50, δ = 0, F = 18, deltapunkt= 1 arcmin/h, T = 18 s


***

A paper by Pio (1899) describes the determination of the longitude (at known latitude) from the culmination of the Moon: The instants of two equal altitudes are measured by a chronometer and a sextant, and the time of culmination is "reduced to the meridian". The practical advantage of the method is that it does not require any transit instruments.



Links
D. A. Pio: Longitude from the Moon Culminations, Monthly Notices of the Royal Astronomical Society, from November 1998 to November 1999, Volume LIX, London 1899.

[NavList 9938] Re: Time of meridian passage accuracy

James N. Wilson: Position from Observation of a Single Body (Appendix I)
Books
Jrg Meyer: Die Sonnenuhr und ihre Theorie, Verlag Harry Deutsch, Frankfurt 20

Jean Meeus: More Mathematical Astronomy Morsels, Willmann-Bell, 2002.
Software
MICA Multiyear Interactive Computer Almanac 1800-2050 by U.S. Naval Observatory

StarryNight 7 CSAP

(c) 2012-2017 J. Giesen

Last update: 2017, Jan 13