PhysicsGrade 7Earth in Space

Astronomy Lab: Seasons, Moon Phase, and Daylight

Rotate Earth around the Sun, change axial tilt and latitude, then observe season, daylight length, solar angle, and Moon phase.

SimulationsLab index
Textbook unitEarth in SpaceGrade 7 Science Unit 6
Keywordsearth, space, orbit, season, moonMapped to available textbook headings
Practice modeManipulate, measure, explainUse the controls, then read the live evidence

Earth Science · Grade 8

Connect Earth's tilt, orbit, and Moon phase

Move Earth around the Sun, change latitude and axial tilt, then observe daylight length, solar angle, seasonal heating, and Moon phase.

SeasonNorthern summer
1

Equinox baseline: set day 80 (spring equinox) at 9°N (Addis Ababa). Record daylight. Why is it near 12 h everywhere?

2

Solstice contrast: advance to day 172 (June solstice). Compare 9°N vs 50°N daylight. Which latitude changes more and why?

3

Moon cycle: advance moon age from 0 (new) to 14.8 (full) and record each phase. Explain illumination % vs observed shape.

Sun
9°
Solar angle76 °88% heating
Declination23.5 °
Daylight12.5 h
Moon phaseFull moon
Astronomy insight

Near-equatorial latitude (9°): axial tilt has minimal effect — daylight stays close to 12 h year-round. Solar angle 76° is high, giving strong direct heating. Month: Jun.

Daylight12.5 h
Solar angle76 °
Moon illumination100%
Orbit angle170 °
Heating index88%

Lab task

Compare daylight at 9°N (Addis Ababa) and 51°N (London) on day 172 and day 355. Record all four cases and explain why the difference is larger at higher latitudes.

Key principle

Seasons are caused by Earth's axial tilt, not its distance from the Sun. When the Northern Hemisphere tilts toward the Sun, it receives more direct rays and longer days — the definition of summer.

Mission

What to prove in this lab

  1. Explain how Earth's tilt and orbit produce seasonal daylight changes.
  2. Relate latitude and solar angle to day length and heating.
  3. Use Moon position to identify visible lunar phase.