B-V Color Index Temperature Estimator
Ballesteros 2012 approximate temperature from independently dereddened Johnson B−V, bounded−0.4..2 for stellar-color proxy; not reddening inference. Model only, not an ephemeris, measured stellar identity or observational guarantee.
Description
A dereddened B−V index can support an empirical temperature estimate.
A dereddened B−V index can support an empirical temperature estimate.1
Its calibration does not remove extinction or model every stellar atmosphere. Use B-V Color Index Temperature Estimator to evaluate the supplied inputs under the model explained below.
When to use B-V Color Index Temperature Estimator
Use B-V Color Index Temperature Estimator to evaluate the supplied inputs under the model explained below. Establish the units, measurement scope and model assumptions before entering values.
How to use B-V Color Index Temperature Estimator and understand its results
- Establish the units, measurement scope and model assumptions before entering values.
- Enter Dereddened b minus v using the field table and validation rules below, then run the tool.
- Read Ballesteros temperature kelvin; interpret the units, signs, ordering and unknown-value placeholders described below.
- Correct reported input errors and rerun. Apply successful results according to their specific meanings and check the assumptions before using them in a decision.
| Input field | Meaning | Value type | Requirement |
|---|---|---|---|
| dereddenedBMinusV | Dereddened b minus v | number | Required; constraints below |
Enter finite independently dereddened B−V from −0.4 to 2 inclusively. Apply the committed Ballesteros relation 4600×[1/(0.92×color+1.7)+1/(0.92×color+0.62)] for K. No reddening removal, luminosity-class fit or uncertainty estimate is supplied.
temperatureK=4600×(1/(0.92×BV+1.7)+1/(0.92×BV+0.62)) Use the field order, units and branch conditions described above.
| Output field | Meaning | Value type |
|---|---|---|
| ballesterosTemperatureKelvin | Ballesteros temperature kelvin | number |
{
"input": {
"dereddenedBMinusV": 0
},
"output": {
"ballesterosTemperatureKelvin": 10125.237191650855
}
}Limitations and assumptions
Its calibration does not remove extinction or model every stellar atmosphere. Apply the exact scope and assumptions explained above.
All listed fields require explicit values. Unexpected fields, incorrect types, nonfinite numbers and sparse arrays fail validation. Domain-specific bounds, alignments and supported tokens are explained above; extremely large inputs or outputs can also be rejected. Input errors differ from successful false results, empty match lists and unknown-evidence placeholders.
Alternative or Complementary methods
Use Stefan-Boltzmann Luminosity Calculator for a related task: Stefan–Boltzmann emission combines surface area and temperature to the fourth power.
Use Main Sequence Lifetime Calculator for a related task: A power-law lifetime model combines mass with a reference lifetime and luminosity exponent.
References
-
B-V Color Index Temperature Estimator — tool.io
Similar or alternative tools
- Stefan-Boltzmann Luminosity Calculator
Stefan–Boltzmann emission combines surface area and temperature to the fourth power.
- Main Sequence Lifetime Calculator
A power-law lifetime model combines mass with a reference lifetime and luminosity exponent.