The abundances of the elements in the solar photosphere. VII.
Solar photosphere abundances of various heavy elements from photoelectric spectrometer measurements of equivalent width of known Fraunhofer lines
Lambert, D. L.↗
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Temperature fluctuations in the solar photosphere.
Temperature fluctuations in solar photosphere determined from granulation data, interpreting results in terms of convective and radiative transport of energy
Wilson, P. R.↗
Forbidden lines of Ca II in the photospheric spectrum.
Ca II forbidden lines in photospheric spectrum identified with weak Fraunhofer line by photoelectric spectrometer scans
Lambert, D. L.↗
A comparison of the photospheric and interplanetary magnetic fields during the flight of Mariner IV.
Interplanetary and photospheric magnetic fields polarities observed by Mariner 4 and with solar magnetograph, noting noncorrelated data along latitudinal strip
Ballif, J. R.↗
The photospheric abundance of iron.
Photospheric Fe I abundance variation with excitation potential
Withbroe, G. L.↗
Temperature fluctuations in the solar photosphere. II - The mean limb-darkening and the second maximum
Solar photosphere temperature fluctuations from model consistent with convection hypothesis agreeing with limb darkening data
Wilson, P. R.↗
On the abundance of iron in the solar photosphere
Solar photospheric Fe abundance determined from IR supermultiplet line spectra, considering LTE effects
Rogerson, J. B., Jr.↗
Abundance of iron in the solar photosphere
Fe abundance in solar photosphere, evaluating various determination methods
Ross, J. E.↗
An interference filter for observing the photospheric network
Sun photographs with violet interference filter, determining photospheric magnetic fields position by cospatial network
Chapman, G. A.↗
Differential rotation of the photospheric magnetic field
Photospheric magnetic field differential rotation using synoptic charts for autocorrelation technique
Howard, R.↗
Photospheric magnetic field rotation - Rigid and differential
Photospheric magnetic field direction autocorrelation showing differential and rigid rotation properties at various heliographic latitudes
Howard, R.↗
On the physical conditions in the photospheric network - An improved model of solar faculae
Solar faculae semiempirical models, cospatial with strong photospheric magnetic fields constructed from continuum observations
Chapman, G. A.↗
Comparison of the mean photospheric magnetic field and the interplanetary magnetic field
Photospheric and interplanetary magnetic field polarity and magnitude comparison, using Explorer observations
Colburn, D. S.↗
Interpretation of the solar continuum from 1680 to 600 A - Model of the transition region photosphere-chromosphere and of the chromosphere
Brightness temperature from solar UV continuum in 1680 to 600 A in photosphere-chromosphere transition model
Cuny, Y.↗
Large scale photospheric magnetic field: The diffusion of active region fields
The large-scale phototospheric magnetic field was computed by allowing observed active region fields to diffuse and to be sheared by differential rotation in accordance with the Leighton (1969) magneto-kinematic model of the solar cycle. The differential rotation of the computed field patterns as determined by autocorrelation curves is similar to that of the observed photospheric field, and poleward of 20 deg. latitude both are significantly different from the differential rotation of the long-lived sunspots (Newton and Nunn, 1951) used as an input into the computations.
Schatten, K. H.↗
The mean photospheric magnetic field from solar magnetograms Comparisons with the interplanetary magnetic field.
Large-scale averages of daily solar magnetograms have been compared by cross-correlation with the interplanetary magnetic sector pattern during a 2.5 yr interval. A significant correlation was found at a lag of about 4.5 days, with the amplitude of the correlation depending on the area included in the magnetogram averages. The highest correlation was found when an area of one quarter of the solar disk was used, which is consistent with the idea that the photospheric features which are to be associated with the interplanetary sector pattern are large scale features.
Scherrer, P. H.↗
One- and multi-component models of the upper photosphere based on molecular spectra. I - The violet system of CN /0, 0/
Spectroheliograms taken in the CN (0, 0) violet band near 3883 A show very small scale network and cell structures with high contrast. The bandhead itself, which is a broad feature due to overlap of several CN lines, allows the diagnostic simplicity of a continuum since motions, magnetic fields, and broadening mechanisms are unimportant. We have obtained spectroheliograms in the bandhead and center-to-limb photoelectric spectra of CN (0, 0) at Kitt Peak National Observatory. From the photoelectric spectra and a detailed analysis of the formation of the CN (0, 0) spectrum we derive a best-fit one-component upper photospheric model differing from that of the HSRA and recommend a change in solar carbon abundance from the HSRA value.
Mount, G. H.↗