Solar structure from global studies of the 5-minute oscillation

  title={Solar structure from global studies of the 5-minute oscillation},
  author={A. Claverie and G. R. Isaak and C. McLeod and H. V. Raay and T. R. Cort{\'e}s},
High sensitivity Doppier spectroscopy of integral sunlight in the 769.9 nm line of neutral potassium reveals several equally spaced lines of Q > 1,000 centred on the well known period of 5 min. These lines are interpreted as low l, high n overtones of the entire Sun and, if viewed in terms of current solar models, appear to imply a low heavy element abundance and a consequent low solar neutrino flux. Previous workers1–3 have used spatial resolution to study the 5-min oscillation of the solar… Expand
Rapid rotation of the solar interior
The observation of line-of-sight velocities of the solar surface by means of Doppler shift measurements of the Fraunhofer absorption lines, using optical resonance scattering, has proved a usefulExpand
Contribution of Low-l p Modes to the Solar Equatorial Rotation Profile
The solar equatorial velocity profile is known down to the base of the convection zone with high precision (≤1%); from here downward until approximately 0.5 R☉, it seems to be constant, independentExpand
Evidence from solar seismology against non-standard solar-core models
GLOBAL oscillations of the Sun1 have been used to test solar models2, but modelling the oscillation frequencies to their measured accuracies of a few microhertz has proved difficult, mostly owing toExpand
Variation of low-order acoustic solar oscillations over the solar cycle
GLOBAL acoustic oscillation modes of the Sun were discovered eleven years ago1. The possibility of temporal variations in the oscillation frequencies was suggested by fluctuations in the flux ofExpand
Observation of additional low-degree 5-min modes of solar oscillation
By measuring the difference between the shifts in the Fe 5,124 spectrum line from light integrated from a central circular portion of the solar disk and from an annular portion exterior to it, weExpand
Solar core rotation
In the continuing study of solar oscillation by means of optical resonant scattering1, two sets of data were obtained between June and August 1981. The first of these was at Haleakala on the islandExpand
The Mark-I helioseismic experiment – I. Measurements of the solar gravitational redshift (1976–2013)
The resonant scattering solar spectrophotometer 'Mark-I', designed and build at the University of Birmingham (UK) and located at the Observatorio del Teide (Spain), has been continuously in operationExpand
Nonparametric and Parametric Methods for Solar Oscillation Spectra
The study of the systematic oscillations of the Sun has led to better understanding of the Sun’s inner structure and dynamics, and may help to resolve inconsistencies between observations and theExpand
Present state of the study of 160-minutes solar oscillation
Global oscillation of the Sun with a period of 160 rain were first discovered in 1974 and since observed in Crimea during the last 6 years; they were confirmed, in 1976–1979, by Doppler measurementsExpand
Global Oscillations at Low Frequency from the SOHO mission (GOLF)
The GOLF experiment on the SOHO mission aims to study the internal structure of the sun by measuring the spectrum of global oscillations in the frequency range 10−7 to 10−2 Hz. Bothp andg modeExpand


On the sun's acoustical spectrum.
Theoretical acoustical spectra for complete solar models have been obtained. Both radial modes and nonradial modes (with l=1,2,3,4,5, and 6) have been calculated for as many as 20 nodes in theExpand
Observations of nonradial p-mode oscillations on the sun
Observations of the solar velocity field with a diode array attached to the echelle spectrograph of a vacuum tower telescope are described which resolve the solar five-minute oscillatory motion intoExpand
The sensitivity of nonradial p mode eigenfrequencies to solar envelope structure.
Eigenfrequencies are calculated for nonradial p mode oscillations in the Sun. These frequencies are shown to depend on the adiabat of the solar convective envelope. The frequency dependence isExpand
The Zeeman broadening of high n solar recombination lines
The Zeeman broadening of high n lines is derived. While in areas of the quiet Sun with field strengths of ≈1 G the upper boundary of the observable frequency region of recombination lines is definedExpand
Observation of free oscillations of the Sun
The Fraunhofer absorption lines for potassium and sodium on the Sun are compared with the corresponding lines in the laboratory using a resonant optical scattering method. The observed shifts betweenExpand
What is the horizontal scale of the 5-min oscillations?
If wrong, all the early reports of a small horizontal scale (≈ 2000 km) for the 5-min oscillations may be due to unfortunate similarities between the velocity and overturning time of the solarExpand
Störungstheoretische Erfassung des Schwingungs- und Resonanzverhaltens nichtlinearer n-Freiheitsgrad-Systeme
ÜbersichtDie Beurteilung der bei Anwendung der Störungstheorie auftretenden Säkularglieder erschwerte bisher in erheblichem Maße die Lösung nichtlinearer n-Freiheitsgrad-Systeme (n > 1). Am BeispielExpand
Nonradial and nonlinear stellar pulsation
The New Solar Physics