A small spherical meteor is at a distance from the Sun of 50 Sun radï. Estimate its temperature,

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A small spherical meteor is at a distance from the Sun of 50...

Key Concepts

Thermal Equilibrium

Thermal equilibrium occurs when an object absorbs energy at the same rate as it radiates energy, leading to a stable temperature. For a small spherical meteor, this concept is applied by setting the absorbed solar energy equal to the energy radiated, thereby allowing the calculation of its equilibrium temperature.

Geometric Considerations in Radiation

For a spherical body, the effective area that intercepts solar radiation (its cross-sectional area) is different from its total surface area over which it radiates energy. This difference is fundamental when deriving the temperature of the body, as it affects the balance between the incoming solar flux and the emitted thermal radiation.

Stefan?Boltzmann Law

This law relates the power radiated per unit area of a black body to the fourth power of its temperature (F = ?T?), and it is crucial for determining how much energy the Sun emits per area. It underpins the calculation of temperature based on the radiation received and emitted, as seen in the equilibrium condition between absorption and emission.

Inverse Square Law

The inverse square law explains that the intensity of radiation from a point source diminishes as the square of the distance from the source. This means that as an object moves away from the Sun, the flux it receives decreases by a factor of 1/(distance)², which is key to estimating how much solar energy is incident on a meteor at a given distance.

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