Wavelength shifts converted to velocities between solar lines observed at disc center and laboratory wavelengths of Fe i, Fe ii, Ti i, Ni i, and Fe i lines in the near infrared are plotted as a function of the logarithm of their solar equivalent width in milliångstroms. The need for wavelengths based on the wavelength standards is stressed. A comparison of photographic Fe i solar wavelength is shown to agree, on the average, with Fourier Transform Spectrometer solar wavelengths within less than 0.5 milliångstroms. Using Balthasar's limb effect tables we convert the disc center velocities to limb velocities and find, though the scatter is large, that there is little evidence for a super-gravitational red shift.

In this paper the absolute limb effect for a number of Fraunhofer lines observed at the McMath Solar Observatory is given. Results, uncorrected for scattered light, are given for the following lines: Feiλ37334.9, λ3735.3, λ5123.7, λ5250.2, λ5434.5, λ6678.0, and λ8886.6. Additional lines observed are five lines of CN λλ3876.3–3880.0, two lines of Caiλ6161.3 and λ6162.2, one line of Nai, λ6160.7, and one CN line (λ7957.0) of the red system.

Solar granules are classified into four groups according to their shapes and splitting by sharp rifts crossing them. The appearance and evolution of ‘white-light dark networks’ is described.

The center-to-limb wavelength shifts of the cores of faint, medium and strong Fraunhofer lines are presented: Fei 3767, Caii 3968, Ceii 4222, Cai 4227, Nai 5896, Baii 6497, and Ki 7699.

Solar differential rotation for 1982–83 obtained at the double pass spectrograph of the McMath telescope at Kitt Peak, are presented for lines of Fe, Mg, Na, K, Si, and O in the wavelength interval λλ3820–10827. The results are analyzed by representations in Legendre polynominals and a power series. The differential rotation is very close to the result obtained by Howard and Harvey in 1966–68 at Mt. Wilson but with a slightly greater amplititude. We find a mean equatorial rate of rotation of 1.977 km s-1. Day to day variations are observed in the equatorial zone; a stable rate of rotation is observed outside of the sunspot zone.

It is shown that comparing an observed Fraunhofer profile to a fitted gaussian yields more information on shape and asymmetry of the solar line than the simple bisector method.

view Abstract Citations (9) References (14) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Center to limb observations of sodium lines in the solar spectrum Pierce, A. K. ; Slaughter, C. Abstract Center to limb (cos theta = 1.0 to 0.1) intensities are given for the profiles of 25 sodium lines distributed at wavelengths from 3302 to 22083 A in the solar spectrum. Central intensities and half-widths are tabulated for five additional sodium lines. Publication: The Astrophysical Journal Supplement Series Pub Date: January 1982 DOI: 10.1086/190768 Bibcode: 1982ApJS...48...73P Keywords: Line Spectra; Sodium; Solar Spectra; Ultraviolet Spectra; Luminous Intensity; Solar Limb; Spectral Line Width; Tables (Data); Solar Physics full text sources ADS |

The coefficients of several polynomial representations of the limb darkening at 62 wavelengths in the UV and visible portions of the solar spectrum obtained at the McMath Solar Telescope are presented in tabular form. Full corrections for scattered light and seeing have been included in the reductions.

view Abstract Citations (9) References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Thorium Comparison Spectrum Breckinridge, James B. ; Pierce, A. Keith ; Stoll, Clifford P. Abstract Wavelengths for approximately 1850 thorium emission lines between 2720 and 8805 A are given. The accuracy of these measures appears to be better than ::i:: 0.001 A. These measures, made from photographic plates taken with the 13 .7-m focal length grating spectrograph at the McMath Solar Telescope at Kitt Peak, are part of work done for the solar wavelength atlas program (Pierce and Breckirridge, Kitt Peak Contributions 559, 1973). We suggest they be used for general stellar and solar comparison wavelengths. Subject headings: line identifications - spectra, laboratory Publication: The Astrophysical Journal Supplement Series Pub Date: February 1975 DOI: 10.1086/190335 Bibcode: 1975ApJS...29...97B full text sources ADS |