Intensity Of Radiation Emitted By Black Body At Absolute Temperature Calculator

Formula Used:

\[ I_b = \frac{[\text{Stefan-BoltZ}] \times T^4}{\pi} \]

Radiation Intensity Of Black Body:

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1. What Is The Radiation Intensity Of Black Body?

The radiation intensity of a black body refers to the amount of electromagnetic radiation emitted per unit solid angle per unit area by a perfect black body at a given temperature. It describes how intensely a black body radiates energy in different directions.

2. How Does The Calculator Work?

The calculator uses the Stefan-Boltzmann law for radiation intensity:

\[ I_b = \frac{\sigma \times T^4}{\pi} \]

Where:

\( I_b \) — Radiation intensity of black body (W/m²·sr)
\( \sigma \) — Stefan-Boltzmann constant (5.670367 × 10⁻⁸ W/m²·K⁴)
\( T \) — Absolute temperature (K)
\( \pi \) — Mathematical constant pi (≈3.14159)

Explanation: This formula calculates the radiation intensity emitted by a perfect black body based on its absolute temperature, following the principles of black body radiation.

3. Importance Of Radiation Intensity Calculation

Details: Calculating radiation intensity is crucial in thermodynamics, astrophysics, and engineering applications. It helps understand energy emission patterns, design thermal systems, and analyze stellar radiation characteristics.

4. Using The Calculator

Tips: Enter the absolute temperature in Kelvin. The temperature must be greater than 0 K for valid calculation results.

5. Frequently Asked Questions (FAQ)

Q1: What is a black body in physics?
A: A black body is an idealized physical object that absorbs all incident electromagnetic radiation, regardless of frequency or angle of incidence, and emits radiation according to its temperature.

Q2: How does temperature affect radiation intensity?
A: Radiation intensity increases with the fourth power of absolute temperature (T⁴). Doubling the temperature increases radiation intensity by a factor of 16.

Q3: What are typical radiation intensity values?
A: Radiation intensity values vary widely with temperature. At room temperature (300K), it's approximately 0.000146 W/m²·sr, while at the sun's surface temperature (5778K), it's about 6.33 × 10⁷ W/m²·sr.

Q4: How is this different from total radiated power?
A: Radiation intensity is directional (per steradian), while total radiated power is integrated over all directions. The total power per unit area is given by σT⁴.

Q5: What are real-world applications of this calculation?
A: This calculation is used in thermal imaging, infrared spectroscopy, climate science, designing radiant heaters, and analyzing stellar properties in astronomy.