Coupled photoionization, cooling and planetary escape
Research context
research method · conditional · As of 2026-10-10
A photoheated atmosphere couples fluid transport, ionization/recombination, absorption and radiative cooling.
Key knowledge
A photoheated atmosphere couples fluid transport, ionization/recombination, absorption and radiative cooling. An energy-limited estimate applies only when a specified absorbed fraction drives escape; recombination/radiative losses or external wind confinement can change the regime.
Values and equations
Mdot≈ε π R_abs^2 F_UV /(G M_p/R_base)
- Mdot
- Mass escape rate kg s^-1
- ε
- Fraction of incident energy driving escape 1
- R_abs,R_base
- Absorption and bound-base radius m
- F_UV
- Incident UV energy flux W m^-2
- M_p
- Planet mass kg
- G
- Gravitational constant m^3 kg^-1 s^-2
Conditions and scope
- Declare incident-flux geometry, absorption radius, composition and boundary pressure.
- The hot-Jupiter model is not transferable unchanged to a terrestrial conductive atmosphere.
- Energy-limited approximation, stated irradiation averaging; ignores Roche correction and strong external confinement.
Sources · 1
References
Sources retain their recorded scope. A source link alone does not establish verification of every statement.
Evidence and review
Atmospheric escape from hot Jupiters: Sections 2–4: photoionization, cooling, hydrodynamic escape and wind confinement (selected source body inspected).
2026-10-10 · Bounded source check of the recorded statement and conditions. This does not certify a unique physical model, reproduce the cited study or replace independent branch review.
Entry details
Permanent link to this entry ↗- Record identity
- research-earth-planet-escape
- Revision
- research.1
- Structured reference record
- Postgraduate & research reference