Starting point
For a bright gibbous or full Moon, try ISO 100–400, f/5.6–f/8 and roughly 1/125–1/500 s for the lunar disk. A thin crescent or earthshine can need much longer exposures or bracketing. These are starting ranges, not fixed recipes.
Moon lesson
Why do Moon phases change, and why does moonrise get later each day?
Move lunar age. The left view shows sunlight and the Moon’s orbit; the right view simultaneously shows the phase and daily Moon path an observer on Earth sees. Hover on desktop or tap on mobile for more detail.
Space view: sunlight, Earth and MoonYellow = direct sunlight · blue = reflected light toward Earth
Moon orbit / ecliptic5.145°
Earth view: visible phase and daily Moon pathLeft is the illuminated lunar disk; right is the daily rise/set path
Ground view: the Moon’s daily path
Go deeper: open the full phase, orbit and eclipse explanationUnderstand light and viewpoint first; expand details when useful
What is moonlight?
The Moon does not produce visible light like the Sun. Sunlight strikes the lunar regolith and is diffusely reflected in many directions; some of that reflected light reaches Earth.
Why are ordinary phases not Earth’s shadow?
Ordinary lunar phases are mainly caused by the changing Sun–Moon–Earth viewing geometry. Near new Moon the lit side faces mostly away from Earth; near full Moon it faces mostly toward Earth. Earth’s shadow is central only during a lunar eclipse.
Why is the synodic month 29.53 days if the Moon orbits in about 27.32 days?
27.32 days is the sidereal month relative to distant stars. During that time Earth has also moved along its solar orbit, so the Moon must travel farther to recover the same Sun–Earth geometry. That phase cycle takes about 29.53 days.
Why is there not an eclipse every new and full Moon?
The Moon’s orbit is tilted about 5.1° to the ecliptic. Most new and full Moons pass above or below exact alignment. Eclipses occur only when phase and orbital-node geometry line up closely enough.
FROM ORBIT TO CAMERA
Turn the Moon model into a shooting decision
Phase controls contrast and sky illumination; altitude and azimuth control composition; focal length controls scale. Treat the settings below as starting ranges, then meter the real sky.
Choose scale
16–35 mm places the Moon in a landscape; 70–200 mm begins to emphasize it; 300–600 mm and beyond make the disk dominant. Dramatic Moon-to-foreground scale comes from shooting position and focal length, not from the Moon physically becoming huge.
In the field
Use Planner for moonrise or moonset azimuth and your foreground bearing. Arrive early enough to move the camera position: a small lateral change can matter more to alignment than changing focal length.
What to look for
Check lunar highlight clipping, atmospheric softness near the horizon, foreground silhouette, and whether the Moon clears terrain or buildings. For earthshine, watch both the bright crescent and the much darker lunar night side.
Common mistakes
Do not expose the Moon like a dark star field, assume moonrise is the same time every day, or treat every large-looking Moon as a special physical enlargement. Long lenses magnify framing; camera-to-foreground geometry creates the dramatic scale relationship.
Related tools
Plan direction & timing · Check the live Moon · Compare focal length · Test exposure
Try it
Set the model near a thin crescent, first quarter and full Moon. For each state, decide whether you would expose for lunar detail, foreground illumination or earthshine, then open Planner and choose a foreground whose bearing matches the Moon near rise or set.
Next lesson
Sources & model limitsWhat is physical fact, and what is simplified here?
Sources
Phase, reflected moonlight, synodic-month context and eclipse geometry follow NASA Moon references. NASA Moon Phases · NASA Eclipses and the Moon
Limits
The scene enlarges bodies and compresses distances for teaching. The “about 49 minutes later” moonrise shift is an average, not a daily guarantee; exact rise/set time and direction depend on date, observer location and lunar declination.
Real size comparisonOpen real-scale comparison
Real size comparison
If Earth’s diameter = 1, how large are the Sun and Moon?
This compares mean diameters at a true size ratio, not distances. The Sun is about 109.2 Earth diameters and the Moon about 0.273 Earth diameters. Orbital distances remain compressed in the 3D teaching scenes, while the lunar orbit is drawn at about 5.145° to the ecliptic.
Sun109.2
Earth1.000
Moon0.273
Mean diameters: Sun ≈ 1,392,700 km · Earth ≈ 12,742 km · Moon ≈ 3,475 km. The diagrams preserve diameter ratios; orbital distances are compressed separately.
The 3D scene compresses distances and enlarges bodies for legibility, but the lunar orbital inclination is drawn at about 5.145°. See the size comparison below for true diameter ratios.