A statistical analysis of NA I D1 profile fluctuations at the center of the solar disk. I - Data reduction and resolvable velocities

Details A statistical analysis of NA I D1 profile fluctuations at the center of the solar disk. I - Data reduction and resolvable velocities A statistical analysis of NA I D1 profile fluctuations at the center of the solar disk. I - Data reduction and resolvable velocities

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...83..217e&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 83, March 1983, p. 217-232. Research supported by the University of Texas and NSF.

Physics

1

Deuterium Compounds, Line Shape, Radial Velocity, Sodium Hydrides, Solar Spectra, Statistical Analysis, Fluctuation Theory, Molecular Spectra, Photosphere, Power Spectra, Root-Mean-Square Errors, Solar Granulation, Solar Observatories, Spectroheliographs, Velocity Errors, Weighting Functions

Scientific paper

A statistical analysis is presented of three radial-velocity fluctuation arrays V(Delta lambda, Y) and line-formation fluctuation arrays, where Delta lambda is wavelength displacement from the center of Na I D1 and Y is displacement on the sun's surface along the spectrograph slit, which were obtained from Sacramento Peak Observatory spectrograms. The variations of these line profile fluctuations are examined, and the radial-velocity rms values, coherences, and power spectra shapes for V(Delta lambda, Y) fluctuations are analyzed at different Delta lambda values with the corresponding effective heights of formation calculated with Mein weighting functions. Among other results, it is found that a possible anticorrelation exists between continuum fluctuations and those near the line center. The radial velocity corrected rms values, which are the root-mean-square values of the radial velocity corrected for instrumental and atmospheric blurring, are shown to be large (1.5-4.0 km/s) primarily due to large corrections for atmospheric blurring. The radial velocity corrected rms minima at effective heights of formation above 350 km indicate the penetration of granulation velocities into the upper photosphere, while the power spectra shapes reflect decreasing average fluctuation scales above the temperature minimum and in the low and middle photosphere.

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