Solar XUV limb brightening observations. II - Lines formed in the chromospheric- coronal transition region
Solar limb brightening of XUV lines of carbon, nitrogen, oxygen and silicon ions in chromospheric-coronal transition region
Withbroe, G. L.↗
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Extreme ultraviolet observations of active regions in the chromosphere and the corona
Solar active regions in chromosphere and corona observed by EUV spectroheliometer aboard OSO-4 spacecraft, discussing ion formation and temperatures
Kirshner, R. P.↗
The chromospheric magnetograph
Chromospheric photoelectric magnetograms with high resolution H alpha pictures for deriving magnetic field directly from filtergrams
Veeder, G. J.↗
Solar XUV limb brightening observations. II - Lines formed in the chromospheric- coronal transition region
Solar far UV limb brightening of C III, N III, N IV, O III, O IV and Si IV lines in chromospheric-corona transition region, correcting coronal model for spicule effects
Withbroe, G. L.↗
Extreme ultraviolet observations of active regions in the chromosphere and the corona
Oso-4 far UV observations of solar chromosphere and corona active regions
Kirshner, R. P.↗
The effect of the density scale height on shock-wave heating in the low solar chromosphere
Lower chromosphere shock wave heating, analyzing density scale height effects
Jordan, S.↗
Structure of the chromosphere-corona transition region
Structure and energy distribution of chromosphere-corona transition region
Fung, P. C. W.↗
The heating of the chromosphere
Collisional processes for determining kinetic temperature distribution and heating of chromosphere
Jordan, S.↗
A note on chromospheric fine structure at active region polarity boundaries
High resolution H-alpha photographs for studying chromospheric fine structure at active region polarity boundaries
Prata, S. W.↗
The solar Lyman continuum and the structure of the solar chromosphere
Solar chromosphere structure and Lyman continuum, examining brightness and kinetic temperatures, limb variations, radiative transfer and models
Kalkofen, W.↗
Mass motion in the solar chromosphere
Solar chromosphere mass motion, studying macroturbulence influences on visible spectrum lines high resolution profiles from rocket spectrograms
Jones, R. A.↗
The manifold structure of the chromosphere and corona
Solar chromosphere and corona manifold structure data, using high resolution filter photography
Zirin, H.↗
Observations of stellar chromospheres
Stellar chromosphere detection through H, K and metastable He lines observation, noting importance for solar physics
Zirin, H.↗
Morphological relationships in the chromospheric H alpha fine structure
Morphological relationships in solar chromospheric H alpha fine structure involving bushes, fibrils, threads and filaments
Foukal, P.↗
Variations of cosmic rays associated with chromospheric flares on the sun
Features of the cosmic-ray variations in the geomagnetic pole region and a smooth decrease in the cosmic rays intensity as a result of increased solar activity are reported. A 66-day variation of the cosmic rays was registered, in agreement with the maximum frequency and power of solar chromospheric flares.
Kozin, I. D.↗
H alpha fine structure and the chromospheric field.
Study of the physical characteristics of the H alpha structures previously defined as fibrils and threads. The interpretation of the fibrils as ends of flux tubes is useful in tracing the behavior of the transverse field component over the solar surface. The observed properties of fibrils and threads are consistent with the hypothesis that they are produced by a shock wave mechanism similar to that advanced by Parker (1963) to explain spicules. It is suggested that the undisturbed magnetic field in the chromosphere of an active region is confined to a thin sheath, while the field of the quiet regions extends into the corona.
Foukal, P.↗
Structure of the chromosphere-corona transition region.
The structure and energy balance of the chromosphere-corona transition region is investigated by means of a static, planar model which is compared with the results of XUV-resonance-line observations. In this model, the transition region is heated by thermal conduction from the corona and cooled by radiative losses. Comparison of the model with observational results implies that this is the dominant process in the energy balance of the transition region, and that the base of the transition region is inherently nonstatic and/or nonplanar. The model explains the observational finding of Noyes et al. (1970) that the number density and the downward heat flux both increase by the same factor from quiet regions to active regions.
Moore, R. L.↗
High resolution spectroscopy of the disk chromosphere. I - Observing procedures.
Review of some of the main features of a high resolution spectroscopy program aimed at the precise photometric observation of chromospheric fine structures using the Sacramento Peak vacuum telescope. The observing procedures are described, and a sample of the first observational results is presented.
Beckers, J. M.↗