Low-frequency, low-degree solar p-mode properties from 22 years of birmingham solar oscillations network data

Guy Davies*, A. M. Broomhall, W. J. Chaplin, Y. Elsworth, Steven Hale

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

30 Citations (Scopus)
118 Downloads (Pure)


The solar low-degree low-frequency modes of oscillation are of particular interest as their frequencies can be measured with very high precision and hence provide good constraints on seismic models. Here we detect and characterize these valuable measures of the solar interior from a 22 yr Birmingham Solar Oscillations Network data set. We report mode frequencies, line widths, heights, amplitudes, and rotational splitting, all with robust uncertainties. The new values of frequency, rotational splitting, amplitude, and line width we provide will help place new constraints on hydrostatic and rotational structure, plus diagnostics of near-surface convection. Further to this, by assuming simple power laws, we extrapolate mode properties to lower frequencies.We demonstrate that the low-l low-frequency p modes have a low signalto-noise ratio and that this cannot be overcome simply by continued observation. It will be necessary to observe the Sun in novel ways to 'beat' the intrinsic granulation noise.

Original languageEnglish
Pages (from-to)2025-2032
Number of pages8
JournalRoyal Astronomical Society. Monthly Notices
Issue number2
Early online date7 Feb 2014
Publication statusPublished - 1 Apr 2014


  • Methods: data analysis
  • Sun: helioseismology
  • Sun: oscillations

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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