This is a live calculation of the time on Mars including mission times for MSL Curiosity and MER-B Opportunity.

JD_{UT} =

JD_{TT} =

M = °

α_{FMS} = °

PBS = °

ν - M = °

ν = °
EOT = ° =

137.4°E longitude

Mouse over a number on the left to get an explanation below

(in progress)

Unix Epoch

This is the number of milliseconds since

1 January 1970 00:00:00 UTC.

We get this straight from your browser.

This is the number of days (rather than milliseconds) since a much older epoch than Unix time.

Rather than an elaborate conversion from the Gregorian date to the Julian date, we just divide
*millis* by 86,400,000 to get the number of days since the Unix epoch and add that number
to 2,440,587.5, the Julian Date at the Unix epoch.

JD_{UT} = 2,440,587.5 + (*millis* / 8.64 × 10^{7} ms/day)

We actually need the Terrestrial Time (TT) Julian Date rather than the UTC-based one. This means we basically just add the leap seconds which, since ? are ? + 32.184.

JD_{TT} = JD_{UT} + (? + 32.184) / 86,400

This is the number we're going to use as the input to many of our Mars calculations.
It's the number of (fractional) days since

12:00 on 1 January 2000

in Terrestrial Time.

We know what JD_{TT} was at the J2000 epoch (2,451,545.0) so it's trivial to convert.

Δt_{J2000} = JD_{TT} - 2,451,545.0

The equivalent of the Julian Date for Mars is the Mars Sol Date.

At midnight on the 6th January 2000 (Δt_{J2000} = 4.5) it was midnight at the Martian
prime meridian, so our starting point for Mars Sol Date is Δt_{J2000} − 4.5.

The length of a Martian day and Earth (Julian) day differ by a ratio of 1.027491252 so we divide by that.

By convention, to keep the MSD positive going back to midday December 29th 1873, we add 44,796.

There is a slight adjustment as the midnights weren't perfectly aligned. Allison, M., and M. McEwen 2000 has −0.00072 but the Mars24 site gives a more up-to-date −0.00096.

MSD = ([(Δt_{J2000} − 4.5) / 1.027491252] + 44,796.0 − 0.00096)

*Coordinated Mars Time* (or MTC) is like UTC but for Mars. Because it is just a mean time,
it can be calculated directly from the Mars Sol Date as follows:

MTC = (24 h × MSD) mod 24

The mean anomaly is a measure of where an orbiting body is in its orbit. More precisely, it's a measure of how far into the full orbit the body is since its last periapsis (the point in the ellipse closest to the focus).

The mean anomaly is the ratio (time-wise) into the full orbit, multiplied by 2π (radians) or 360° although the value doesn't truly correspond to any angle. The mean anomaly is proportional to time (and
hence area swept) rather that the actual angle of the body from the
focus (which would be the *true anomaly*).

So the mean anomaly can be calculated from Δt_{J2000} if we know the mean
anomaly at the J2000 epoch (19.3870°) and the mean daily motion (360° / length of anomalistic orbit in days).

This gives us:

M = 19.3870° + 0.52402075°Δt_{J2000}

for Mars.

Mars goes around the Sun, but viewed from Mars's point of view, the Sun goes around Mars. I'm not talking about the daily motion of the Sun caused by Mars's rotation, but the year-long motion of the Sun viewed from Mars.

Because the orbit is an ellipse, the Sun will go faster some times than others. Imagine a
fictitious Sun, though, that took the same Martian year to go around Mars but which orbited at a
constant angular velocity (the mean of the real Sun). This is the *fictitious mean Sun*
and it's easier to calculate its angle first because, like the mean anomaly, it is proportional
to time.

Based on observations, Allison and McEwen give the angle at J2000 and the daily change (based on tropical orbit period) as 270.3863° and 0.52403840° / day respectively.

This gives us:

α_{FMS} = 270.3863° + 0.52403840°Δt_{J2000}

The eccentricity is the deviation of the orbit's ellipse from being a perfect circle. It varies
ever so slightly over time and for Mars is given by *e* = 0.09340 + 2.477 × 10^{-9} / day Δt_{J2000} = .

The difference between the actual position of the Sun and the fictitious mean Sun is the same as
the difference between the true anomaly and mean anomaly. This is called the *Equation of Center*.

For a two-body Kepler orbit, this difference can be approximated using a Fourier-Bessel series given
the mean anomaly M and eccentricity *e*. This results in:

(10.691° + 3° × 10^{-7} Δ*t*_{J2000}) sin *M*

+ 0.623° sin 2*M*

+ 0.050° sin 3*M*

+ 0.005° sin 4*M*

+ 0.0005° sin 5*M*

We're not quite done yet as the above assumes a two-body Kepler motion and we need to include the perturbations caused by other planets previously calculated.

Once they have been added, we have our equation of center.

By adding this to our mean anomaly, M, we also get our true anomaly ν = °

We can now calculate the actual position of the Sun as follows:

*L*_{S} = α_{FMS} + (ν − M)

Remember, this is not the daily motion of the Sun caused by Mars's rotation, but the year-long motion of the Sun viewed from Mars. Think of it as where Mars is in its orbit around the Sun, flipped around to be from Mars's perspective (hence "areocentric").

Formulae from
Allison, M., and M. McEwen 2000. A post-Pathfinder evaluation of aerocentric solar coordinates with improved timing recipes for Mars seasonal/diurnal climate studies. *Planet. Space Sci.* **48**, 215-235.
and Mars24 Algorithm and Worked Examples