Chandrasekhar–Friedman–Schutz instability
E7942
astrophysical instability
gravitational-radiation-driven instability
rotational instability in stars
The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
All labels observed (1)
| Label | Occurrences |
|---|---|
| Chandrasekhar–Friedman–Schutz instability canonical | 1 |
Statements (45)
| Predicate | Object |
|---|---|
| instanceOf |
astrophysical instability
ⓘ
gravitational-radiation-driven instability ⓘ rotational instability in stars ⓘ |
| affects |
neutron stars
ⓘ
rotating stars ⓘ |
| alsoKnownAs | CFS instability ⓘ |
| appliesTo |
f-modes
ⓘ
g-modes ⓘ non-axisymmetric modes ⓘ r-modes ⓘ |
| causes |
growth of non-axisymmetric oscillation modes
ⓘ
secular instability in rotating stars ⓘ |
| consequence |
emission of continuous gravitational waves
ⓘ
spin-down of rapidly rotating neutron stars ⓘ |
| criterion | mode pattern speed changes sign between rotating and inertial frames ⓘ |
| dependsOn |
equation of state of dense matter
ⓘ
gravitational radiation reaction ⓘ stellar rotation rate ⓘ |
| describedIn | general relativistic perturbation theory ⓘ |
| drivenBy | emission of gravitational waves ⓘ |
| energySource | rotational kinetic energy of the star ⓘ |
| field |
general relativity
ⓘ
gravitational-wave astrophysics ⓘ relativistic astrophysics ⓘ |
| mathematicalDescription | eigenmode analysis of rotating relativistic stars ⓘ |
| mechanism |
gravitational radiation removes angular momentum from the star
ⓘ
gravitational-wave backreaction amplifies certain oscillation modes ⓘ retrograde modes in the rotating frame can appear prograde in the inertial frame ⓘ |
| namedAfter |
Bernard F. Schutz
ⓘ
John L. Friedman ⓘ Subrahmanyan Chandrasekhar ⓘ |
| observationalSignature | narrow-band continuous gravitational-wave emission ⓘ |
| originatesFrom |
work of John L. Friedman and Bernard F. Schutz on gravitational radiation instabilities
ⓘ
work of Subrahmanyan Chandrasekhar on rotating stars ⓘ |
| relatedTo |
Chandrasekhar limit
ⓘ
non-radial stellar oscillations ⓘ r-mode instability ⓘ |
| relevantFor |
gravitational-wave detection by ground-based interferometers
ⓘ
young rapidly rotating neutron stars ⓘ |
| stabilizedBy |
bulk viscosity
ⓘ
shear viscosity ⓘ viscosity in stellar matter ⓘ |
| studiedIn |
numerical relativity
ⓘ
theory of compact objects ⓘ |
| timescale | secular timescale ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.