Radiation Energy Emitted By Black Body In Time Interval Given Temperature Calculator

Stefan-Boltzmann Law:

\[ E = \sigma \times T^4 \times A \times \Delta t \]

Energy Emitted (E):

Unit Converter ▲

Unit Converter ▼

From:	To:

1. What is the Stefan-Boltzmann Law?

The Stefan-Boltzmann Law describes the power radiated from a black body in terms of its temperature. It states that the total energy radiated per unit surface area of a black body is directly proportional to the fourth power of the black body's thermodynamic temperature.

2. How Does the Calculator Work?

The calculator uses the Stefan-Boltzmann Law:

\[ E = \sigma \times T^4 \times A \times \Delta t \]

Where:

\( E \) — Energy emitted (Joules)
\( \sigma \) — Stefan-Boltzmann constant (5.670367 × 10⁻⁸ W/m²K⁴)
\( T \) — Temperature (Kelvin)
\( A \) — Total surface area (m²)
\( \Delta t \) — Time interval (seconds)

Explanation: The formula calculates the total energy radiated by a black body over a given time period based on its temperature and surface area.

3. Importance of Radiation Energy Calculation

Details: This calculation is crucial in thermodynamics, astrophysics, and engineering for understanding heat transfer, stellar radiation, and designing thermal systems.

4. Using the Calculator

Tips: Enter temperature in Kelvin, surface area in square meters, and time interval in seconds. All values must be positive.

5. Frequently Asked Questions (FAQ)

Q1: What is a black body?
A: A black body is an idealized physical body that absorbs all incident electromagnetic radiation, regardless of frequency or angle of incidence.

Q2: Why is temperature raised to the fourth power?
A: The fourth power relationship comes from the integration of Planck's law over all wavelengths and solid angles.

Q3: What are typical applications of this law?
A: Applications include calculating stellar radiation, designing thermal insulation systems, and understanding global warming mechanisms.

Q4: How accurate is this calculation for real objects?
A: Real objects are not perfect black bodies, so the calculation gives the maximum possible radiation. Real objects emit less radiation, described by their emissivity.

Q5: What are the limitations of this equation?
A: The equation assumes a perfect black body and uniform temperature distribution. It doesn't account for wavelength-dependent emission or non-uniform surfaces.