Secondary Eclipse Planet Brightness Temperature Solver
Monochromatic blackbody brightness temperature from planet/star eclipse flux ratio; stellar spectrum, passband integration/reflection and limb effects omitted.
Description
Secondary Eclipse Planet Brightness Temperature Solver: return monochromatic brightness temperature k.
Brightness temperature is the blackbody temperature that reproduces a measured radiance at a chosen wavelength. It need not equal a planet's physical surface temperature.
This tool returns monochromatic brightness temperature k. Use the stated units and model convention when interpreting these fields.
When to use this tool
Use this tool when the supplied inputs match the specific operation described above and you need a repeatable result under its stated convention.
- Check the supported input and output contract against an existing calculation or observation.
- Use the complete example to confirm units, selector spelling and result interpretation.
How to use the tool and how it works
- Enter every field in the input table using the stated units and the exact supported selector spelling where applicable.
- Run the tool. Correct input errors before interpreting an output.
- Read the result fields below; use accompanying flags and the stated sign, boundary or model convention when interpreting a number.
Use the stellar blackbody temperature, wavelength, squared planet/star radius ratio and eclipse depth to invert the monochromatic Planck-ratio expression. The hc/k constant used is 0.014387768775039337 m K.1
| Input field | Meaning and units | Accepted input |
|---|---|---|
| starTemperatureK | Star temperature k. Kelvin. | Finite number; greater than zero |
| wavelengthM | Wavelength m. Meters. | Finite number; greater than zero |
| planetToStarRadius | Planet to star radius. | Finite number; greater than zero; from zero to one inclusive |
| eclipseDepthFraction | Eclipse depth fraction. Fractional units; 0.2 means 20%. | Finite number; greater than zero; from zero to one inclusive |
| Output field | Interpretation |
|---|---|
| result | Object containing the following named result fields. |
| result.monochromaticBrightnessTemperatureK | Monochromatic brightness temperature k; use the stated units and sign convention. |
{
"input": {
"starTemperatureK": 1000,
"wavelengthM": 0.000014387768775039337,
"planetToStarRadius": 0.1,
"eclipseDepthFraction": 0.01
},
"output": {
"result": {
"monochromaticBrightnessTemperatureK": 1000
}
}
}Limitations and assumptions
- The model neglects reflected light and band integration. Positive inputs, bounded fractions and a bounded stellar Planck exponent are required.
- Every declared field is required and unexpected fields are rejected. Numeric inputs must be finite; input errors are distinct from a valid false result or an explicitly qualified output.
- Extremely large inputs and nonfinite or excessively large outputs are rejected. List positions reported by the tool use zero-based indices unless stated otherwise.
Alternative or Complementary methods
Check the underlying observations, units and conventions independently before using the result in a larger workflow. The tools listed below address nearby tasks; compare their inputs and scope before substituting one for this operation.
References
Similar or alternative tools
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An ideal gray atmosphere represents infrared opacity using discrete layers.