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Eclipses and orbital inclination

By changing the inclination of the moon's orbit and the direction of intersection, we look at the eclipses of the moon and the number of eclipses in a year.

    E11 · Eclipses and orbital inclinationReady
    You can also experiment with the numbers and controls below the scene.

    Earth Science, Astronomy, Space / Principles and Exploration

    Eclipses and orbital inclination — principles and investigation

    Sun and moon occur every month, but solar and lunar eclipses do not occur every month. Examine the alignment conditions of the Sun, Earth, and Moon by changing the inclination, intersection direction, and observation point of the Moon's orbit. Check the location of the shadow to see why the phase condition and the spatial condition of being near the intersection must meet together.

    How does it work?

    A ceremony can only be created when the conditions of arrangement of sac and net and that it is near the intersection meet together.

    Key relationship

    Line: |β|≤about 1.5° · Network: |β|≤about 1.0°

    Try this investigation

    1. Change the direction of the slope and intersection and run for one year. The time slider previews the scene before execution. Compare the shadows from the side and above views.
    2. We inspect all moons and moons of the year at inclinations of 5.1° and 0° and record the number of solar and lunar eclipses.
    3. Maintain the slope of 5.1° and change the intersection direction to 90° to compare when the equation occurs.

    Interpreting your results

    With zero orbital inclination, how often do eclipses occur in this simplified model?

    A solar eclipse is possible in a eclipse when the moon blocks the sun, and a lunar eclipse is possible in a eclipse when the moon passes through the Earth's shadow. If there is an inclination, most of the time it deviates above or below the ecliptic.

    Assumptions and limitations

    The equation limits of 1.5°·1.0° are approximations for educational purposes. Assume a lunar month of 29.53059 days, a year of 365.25 days, a fixed intersection, and a circular orbit. A year has 0≤t<365.25 days, including the starting sun. The size and distance of the true shadow and penumbral shadow are scales for explanation purposes only. We do not predict the actual date, visible area on the ground, or whether there will be a total eclipse.