Stellar Tidal Disruption Radius
Estimate the Newtonian stellar tidal radius using a point central mass; relativistic capture and stellar structure are not modeled.
Description
A Newtonian tidal-radius estimate compares a star's self-gravity with differential gravity from a central point mass.
A Newtonian tidal-radius estimate compares a star's self-gravity with differential gravity from a central point mass. Its cube-root mass-ratio scaling is a simplified disruption scale rather than a detailed stellar or relativistic calculation.1
Estimate the Newtonian stellar tidal radius using a point central mass; relativistic capture and stellar structure are not modeled.
When to use Stellar Tidal Disruption Radius
Use this tool to estimate the Newtonian stellar tidal radius using a point central mass; relativistic capture and stellar structure are not modeled.
Prepare the orbital state or model parameters in one reference frame. Use compatible distance/time units and the stated angular and gravitational-parameter conventions.
How to use Stellar Tidal Disruption Radius and understand its results
- Prepare the orbital state or model parameters in one reference frame. Use compatible distance/time units and the stated angular and gravitational-parameter conventions.
- Enter stellarRadius, centralMass, stellarMass using the field table and calculation rules, then run the tool.
- Read disruptionRadius. The explanation below defines the units, signs, ordering and any flags or placeholder values.
- If the tool reports an input issue, correct the values and run it again. Apply the stated assumptions when interpreting a successfully returned result.
| Input field | Meaning | Value type; see rules below | Requirement |
|---|---|---|---|
| stellarRadius | Stellar radius | number | Required |
| centralMass | Central mass | number | Required |
| stellarMass | Stellar mass | number | Required |
Enter strictly positive stellar radius, central mass and stellar mass. The two masses must use matching units; the output keeps the radius unit. The tool takes the cube root of the mass ratio and multiplies by the stellar radius. Equal masses return the supplied stellar radius.
disruptionRadius = stellarRadius × (centralMass/stellarMass)^(1/3) Units, indexing, boundary conditions and exceptional cases are defined in the calculation rules above.
| Output field | Meaning | Value type |
|---|---|---|
| disruptionRadius | Disruption radius | number |
{
"input": {
"stellarRadius": 1,
"centralMass": 8000,
"stellarMass": 1
},
"output": {
"disruptionRadius": 20
}
}Limitations and assumptions
Stellar structure, encounter geometry, rotation, relativistic capture and a black hole's horizon are not modeled. It does not supply a disruption probability or verify that a central mass is in the regime where the approximation is useful.
Numeric inputs must be finite. Follow the calculation-specific rules for overflow, underflow and exceptional cases. Missing required fields, extra fields, wrong value types and violations of the calculation rules are input errors.
Alternative or Complementary methods
Use Specific Orbital Energy: Evaluate specific two-body orbital energy v²/2−μ/r in consistent units; this does not determine angular momentum or collision safety. For a complementary task, use Semimajor Axis From Period: Invert Kepler third law for a positive elliptic semimajor axis using total gravitational parameter and period in compatible units.
References
-
Stellar Tidal Disruption Radius — tool.io
Similar or alternative tools
- Specific Orbital Energy
Evaluate specific two-body orbital energy v²/2−μ/r in consistent units; this does not determine angular momentum or collision safety.
- Semimajor Axis From Period
Invert Kepler third law for a positive elliptic semimajor axis using total gravitational parameter and period in compatible units.