GEOG 203: Planet Earth - Solar Energy and the Seasons

GEOG 203: Planet Earth - Solar Energy and the Seasons

The Solar System, Sun, and Earth

  • Speed of Light and Cosmic Scale

    • Light travels at approximately 300,000 km/sec300,000 \text{ km/sec} (186,000 miles/sec186,000 \text{ miles/sec}).

    • A light year is the distance light travels in one vacuum year, totaling roughly 9.5 trillion km9.5 \text{ trillion km}. This is a measure of distance, not time.

    • Look-back Time: Observationally, because light takes time to travel, we see celestial objects as they were in the past.

    • Moon: 384,400 km384,400 \text{ km} away (1.28 light-seconds1.28 \text{ light-seconds}).

    • Sun: 150,000,000 km150,000,000 \text{ km} away (8 minutes and 20 light-seconds8 \text{ minutes and 20 light-seconds}).

    • Milky Way Galaxy: Approximately 100,000 light years100,000 \text{ light years} across, containing billions of stars.

Dimensions and Distances

  • Earth’s Orbit and the Plane of the Ecliptic

    • The Plane of the Ecliptic is the imaginary flat surface defined by Earth's orbit around the Sun.

    • The average distance (Earth-Sun) is approximately 150 million km150 \text{ million km}, defined as 1 Astronomical Unit (AU)1 \text{ Astronomical Unit (AU)}.

  • Orbital Variation: Perihelion and Aphelion

    • Earth's orbit is an ellipse, not a perfect circle.

    • Perihelion: Earth is closest to the Sun (147,000,000 km147,000,000 \text{ km}) on January 3rd. Interestingly, this occurs during the Northern Hemisphere winter, proving distance is not the primary cause of seasons.

    • Aphelion: Earth is farthest from the Sun (152,000,000 km152,000,000 \text{ km}) on July 4th.

Solar Activity and Radiation

  1. Sunspots and the Solar Cycle

    • Sunspots are dark, cooler regions on the Sun caused by intense magnetic activity.

    • They follow an approximately 11-year cycle11 \text{-year cycle}. High sunspot activity (Solar Maximum) correlates with increased solar radiation output and potential disruptions to satellite communications on Earth.

  2. Solar Wind and the Magnetosphere

    • The Sun emits a stream of charged particles called Solar Wind.

    • Magnetosphere: Earth's magnetic field acts as a shield, deflecting these particles. Near the poles, particles interact with the atmosphere to create Auroras (Aurora Borealis in the North; Aurora Australis in the South).

  3. Principles of Electromagnetic Radiation

    • Energy is emitted in electromagnetic waves characterized by:

      • Wavelength (λ\lambda): Distance between successive crests.

      • Frequency (ff): Number of waves passing a point per second.

    • Wien’s Displacement Law: Hotter objects emit shorter wavelengths (Sun = high energy shortwave), while cooler objects emit longer wavelengths (Earth = lower energy longwave).

The Electromagnetic Spectrum and Energy Balance

  • Temperature Scales: Absolute zero is 0 K0 \text{ K} (273.15C-273.15^\circ \text{C}).

  • Solar Radiation (Shortwave): The Sun (6000 K6000 \text{ K}) emits energy primarily in the visible light, ultraviolet, and near-infrared spectrums.

  • Terrestrial Radiation (Longwave): The Earth (288 K288 \text{ K}) emits thermal infrared energy.

  • Solar Constant: The average insolation at the top of the atmosphere is 1372 W/m21372 \text{ W/m}^2.

  • Albedo and Absorption:

    • 45%45\% of incoming radiation is reflected or scattered (Albedo).

    • 24%24\% is absorbed in the atmosphere.

    • 47%47\% is absorbed at the surface and later re-radiated as longwave heat.

Insolation and Earth's Curvature

  • Insolation (Incoming Solar Radiation): The amount of solar energy intercepted by Earth.

  • The Sphericity Factor: Because Earth is a sphere, the Sun's rays strike the surface at different angles:

    • Subsolar Point: The specific location where the Sun is directly overhead (9090^\circ angle), receiving maximum energy per unit area.

    • High latitudes receive rays at lower angles, causing the energy to spread over a larger area (Beam Spreading) and pass through more atmosphere (Path Length Tracking), leading to cooler temperatures.

Factors Affecting Seasons

  1. Revolution: The 365.24-day365.24 \text{-day} trip around the Sun determines the annual cycle.

  2. Rotation: The 24-hour24 \text{-hour} turn on Earth's axis creates the day/night cycle and the Circle of Illumination (the line dividing day and night).

  3. Tilt (Obliquity): Earth's axis is tilted at 23.523.5^\circ from a line perpendicular to the plane of the ecliptic.

  4. Axial Parallelism: The axis remains pointed toward the North Star (Polaris) throughout the entire orbit.

Annual March of the Seasons

  • Summer Solstice (June 20-21):

    • Subsolar point is at the Tropic of Cancer (23.5N23.5^\circ \text{N}).

    • 24 hours of daylight at the Arctic Circle (66.5N66.5^\circ \text{N}); 24 hours of darkness at the Antarctic Circle (66.5S66.5^\circ \text{S}).

  • Fall Equinox (September 22-23):

    • Subsolar point is at the Equator (00^\circ).

    • All locations on Earth experience exactly 12 hours12 \text{ hours} of day and night.

  • Winter Solstice (December 21-22):

    • Subsolar point is at the Tropic of Capricorn (23.5S23.5^\circ \text{S}).

    • Arctic Circle experiences 24 hours of darkness; Antarctic Circle experiences 24 hours of daylight (‘Midnight Sun’).

  • Spring Equinox (March 20-21):

    • Subsolar point returns to the Equator (00^\circ), signaling the start of the warming trend in the Northern Hemisphere.