Determination of physical parameters of prominences using steady-state equations

Details Determination of physical parameters of prominences using steady-state equations Determination of physical parameters of prominences using steady-state equations

Jun 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975azh....52..572t&link_type=abstract

Astronomicheskii Zhurnal, vol. 52, May-June 1975, p. 572-578. In Russian.

Physics

Continuous Spectra, H Lines, Solar Prominences, Solar Spectra, Astronomical Models, Electron Density (Concentration), Electron Energy, Fraunhofer Lines, H Alpha Line, Hydrogen Atoms, Integral Equations, Solar Physics, Statistical Analysis, Steady State

Scientific paper

A system of steady-state equations is formulated for the continuum and first ten levels of hydrogen atoms in solar prominences. A method and several variants are outlined for simultaneously determining the basic physical parameters of prominences. These parameters include the optical thickness of a prominence in the H-alpha line center, its electron density, electron temperature, and effective extent.

Affiliated with

Also associated with

No associations

Rating

Determination of physical parameters of prominences using steady-state equations does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Determination of physical parameters of prominences using steady-state equations, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Determination of physical parameters of prominences using steady-state equations will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-748616