Static model of chromospheric heating in solar flares

Journal Article · Thu Sep 15 04:00:00 EDT 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/161336· OSTI ID:5401636

Ricchiazzi, P J; Canfield, R C

We have modeled the response of the solar chromosphere to several flare processes: nonthermal electrons, thermal conduction, and coronal pressure. The equations of steady state energy balance, hydrostatic equilibrium, radiative transfer, and atomic statistical equilibrium are solved simultaneously by finite difference methods, using linearization and iteration. It is assumed that the atmospheric response is confined to one dimension by a strong vertical magnetic field. The radiative transfer equation is solved for the most important optically thick transitions of hydrogen magnesium, and calcium. Radiative loss due to H/sup -/, the EUV and X-ray lines of heavier ions, and free-free bremsstrahlung is included in an optically thin manner.

• Research Organization: Center for Astrophysics and Space Sciences, University of California, San Diego
• OSTI ID: 5401636
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 272:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CHROMOSPHERE
ELECTRONS
ELEMENTARY PARTICLES
ENERGY BALANCE
ENERGY TRANSFER
FERMIONS
FLUID MECHANICS
HEAT TRANSFER
HEATING
HYDRODYNAMICS
IONIZATION
LEPTONS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
RADIATION TRANSPORT
RADIATIONS
SOLAR ACTIVITY
SOLAR ATMOSPHERE
SOLAR ELECTRONS
SOLAR FLARES
SOLAR PARTICLES
SOLAR RADIATION
STAR MODELS
STEADY-STATE CONDITIONS
STELLAR RADIATION
THERMAL CONDUCTION