Chandrasekhar Limit Checker
Ideal zero-temperature relativistic electron-degenerate Chandrasekhar 5.83/μe²mass proxy; not exp los ion, rotation or actual stability prediction. Model only, not an ephemeris, measured stellar identity or observational guarantee.
Description
The ideal Chandrasekhar mass depends on the mean molecular weight per electron.
The ideal Chandrasekhar mass depends on the mean molecular weight per electron.1
A signed mass reserve is conditional on that idealization rather than a stability diagnosis. Use Chandrasekhar Limit Checker to evaluate the supplied inputs under the model explained below.
When to use Chandrasekhar Limit Checker
Use Chandrasekhar Limit Checker to evaluate the supplied inputs under the model explained below. Establish the units, measurement scope and model assumptions before entering values.
How to use Chandrasekhar Limit Checker and understand its results
- Establish the units, measurement scope and model assumptions before entering values.
- Enter White dwarf mass solar, Caller electron molecular weight using the field table and validation rules below, then run the tool.
- Read Ideal chandrasekhar mass solar, Signed ideal mass reserve solar; 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 |
|---|---|---|---|
| whiteDwarfMassSolar | White dwarf mass solar | number | Required; constraints below |
| callerElectronMolecularWeight | Caller electron molecular weight | number | Required; constraints below |
Enter nonnegative white-dwarf mass in solar units and positive caller mean molecular weight per electron. Compute ideal limit 5.83/μe² and return limit minus observed mass as signed solar-unit reserve. Negative reserve is allowed. No default electron weight, rotation, finite-temperature correction or stability verdict is installed.
idealLimitSolar=5.83/electronMolecularWeight²; reserveSolar=limit−mass Use the field order, units and branch conditions described above.
| Output field | Meaning | Value type |
|---|---|---|
| idealChandrasekharMassSolar | Ideal chandrasekhar mass solar | number |
| signedIdealMassReserveSolar | Signed ideal mass reserve solar | number |
{
"input": {
"whiteDwarfMassSolar": 1,
"callerElectronMolecularWeight": 2
},
"output": {
"idealChandrasekharMassSolar": 1.4575,
"signedIdealMassReserveSolar": 0.4575
}
}Limitations and assumptions
A signed mass reserve is conditional on that idealization rather than a stability diagnosis. 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 Main Sequence Lifetime Calculator for a related task: A power-law lifetime model combines mass with a reference lifetime and luminosity exponent.
Use Eddington Luminosity Limit Calculator for a related task: An ideal Eddington luminosity compares radiative acceleration with gravitational attraction.
References
-
Chandrasekhar Limit Checker — tool.io
Similar or alternative tools
- Main Sequence Lifetime Calculator
A power-law lifetime model combines mass with a reference lifetime and luminosity exponent.
- Eddington Luminosity Limit Calculator
An ideal Eddington luminosity compares radiative acceleration with gravitational attraction.