Planets and Moons
ID: 12739
# 100 Lunar Days - Parts I and II

In October of 2017, Lunar Reconnaissance Orbiter (LRO) celebrates one hundred days of collecting scientific data at the Moon. One hundred *Moon* days. That's 100 opportunities to observe changes from night to day, photograph the surface at different Sun angles, measure rising and falling temperatures, and study the way certain chemicals react to the daily light and temperature cycle, among other things. But you might be wondering...

#### What is a lunar day?

What do we mean when we say that LRO has been at the Moon for 100 lunar days? The short answer is this: A day is the length of time between two noons or sunsets. That's 24 hours on Earth, 708.7 hours (29.53 Earth days) on the Moon. We can see a day passing on the Moon by watching its month-long cycle of phases, and as of October 16, 2017, LRO has watched this cycle 100 times since the start of its exploration and science mission on September 15, 2009.

But as often happens in astronomy, the situation's actually a little more complicated. The trouble starts with merely nailing down a definition of the word

At any given location on the Earth, a**local solar day** is the time it takes the Sun to return to the same point in the sky. To be more precise, we define a line in the sky, the meridian, which runs between due north and due south and passes through the zenith (the straight-up point). Local noon is the time when the Sun is centered on the meridian, and a local solar day is the time between two successive local noons.

The length of this kind of day varies throughout the year. Currently, it can be as much as 21 seconds shorter or 29 seconds longer than 24 hours. This variation is due to the**eccentricity** of the Earth's orbit (the orbit is an ellipse, not a circle), and the **obliquity** of the ecliptic (the Earth's axis is tilted relative to its orbit).

So that we don't have to reset our clocks all the time, it's convenient to define a**mean solar day**, the average of the local solar day over a full year. A mean solar day is exactly 24 hours long. In fact, we *define* an hour as 1/24 of a mean solar day.

The mean solar day can't be the average over any arbitrary year. The eccentricity and obliquity vary over time, and because of precession of the equinoxes, the effect of obliquity slides through the calendar, alternately reinforcing and canceling the effect of eccentricity over tens of thousands of years. The Earth is also slowing down, primarily due to tidal interactions with the Moon.

The mean solar day is the theoretical average local solar day, calculated by fixing the eccentricity, obliquity, precession, and rotation rate to the values at noon in Greenwich, England, on December 31, 1899, using the theory of the Sun's apparent motion developed by Simon Newcomb in the 1890's.

We now have extremely accurate atomic clocks. We define the length of a second as a certain number of waves in the radiation from a cesium atom, and we say that a mean solar day is 86400 of these seconds. For historical continuity, the number of waves was chosen so that this second is 1/86400 of the mean solar day defined by Newcomb's theory.

The concept of a solar day can be extended to other bodies in the solar system, including our Moon. A mean solar day on the Moon, a**lunar day** for short, is 29.5306 Earth days. Local lunar days can vary even more than solar days on Earth, over 6 hours shorter or 7 hours longer than the mean. The 100 lunar days celebrated by LRO in October of 2017 are *mean* lunar days.

Because the Moon is tidally locked to the Earth, it always shows the Earth the same face. This also means that it rotates at the same rate that it orbits. A lunar day takes exactly as long as one complete orbit relative to the Sun. A lunar day also corresponds to one complete cycle of the phases visible from Earth, so a lunar day is the same as a synodic month.

At this point, it shouldn't surprise you that there are other kinds of days (sidereal, for example) and months (anomalistic and draconic, to name two). But that's a story for another time.

#### Source Material

#### Credits

**David Ladd** (USRA): Lead Producer

**David Ladd** (USRA): Lead Video Editor

**David Ladd** (USRA): Lead Animator

**Noah Petro** (NASA/GSFC): Lead Scientist

**Ernie Wright** (USRA): Lead Visualizer

**Please give credit for this item to:**

NASA's Goddard Space Flight Center

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But as often happens in astronomy, the situation's actually a little more complicated. The trouble starts with merely nailing down a definition of the word

day.

At any given location on the Earth, a

The length of this kind of day varies throughout the year. Currently, it can be as much as 21 seconds shorter or 29 seconds longer than 24 hours. This variation is due to the

So that we don't have to reset our clocks all the time, it's convenient to define a

The mean solar day can't be the average over any arbitrary year. The eccentricity and obliquity vary over time, and because of precession of the equinoxes, the effect of obliquity slides through the calendar, alternately reinforcing and canceling the effect of eccentricity over tens of thousands of years. The Earth is also slowing down, primarily due to tidal interactions with the Moon.

The mean solar day is the theoretical average local solar day, calculated by fixing the eccentricity, obliquity, precession, and rotation rate to the values at noon in Greenwich, England, on December 31, 1899, using the theory of the Sun's apparent motion developed by Simon Newcomb in the 1890's.

We now have extremely accurate atomic clocks. We define the length of a second as a certain number of waves in the radiation from a cesium atom, and we say that a mean solar day is 86400 of these seconds. For historical continuity, the number of waves was chosen so that this second is 1/86400 of the mean solar day defined by Newcomb's theory.

The concept of a solar day can be extended to other bodies in the solar system, including our Moon. A mean solar day on the Moon, a

Because the Moon is tidally locked to the Earth, it always shows the Earth the same face. This also means that it rotates at the same rate that it orbits. A lunar day takes exactly as long as one complete orbit relative to the Sun. A lunar day also corresponds to one complete cycle of the phases visible from Earth, so a lunar day is the same as a synodic month.

At this point, it shouldn't surprise you that there are other kinds of days (sidereal, for example) and months (anomalistic and draconic, to name two). But that's a story for another time.

NASA's Goddard Space Flight Center

http://svs.gsfc.nasa.gov/12739

SVS >> HDTV

SVS >> Moon

SVS >> LRO

SVS >> Lunar Reconnaissance Orbiter

SVS >> Planetary Science

NASA Science >> Planets and Moons