Solving the discrepancy between the seismic and photospheric solar radius

M. Haberreiter, W. Schmutz, A. G. Kosovichev

Research output: Contribution to journalArticlepeer-review

47 Scopus citations

Abstract

Two methods are used to observationally determine the solar radius: One is the observation of the intensity profile at the limb; the other one uses f-mode frequencies to derive a "seismic" solar radius which is then corrected to optical depth unity. The two methods are inconsistent and lead to a difference in the solar radius of ∼0.3 Mm. Because of the geometrical extension of the solar photosphere and the increased path lengths of tangential rays the Sun appears to be larger to an observer who measures the extent of the solar disk. Based on radiative transfer calculations we show that this discrepancy can be explained by the difference between the height at disk center where τ5000 = 1 (τRoss = 2/3) and the inflection point of the intensity profile on the limb. We calculate the intensity profile of the limb for the MDI continuum and the continuum at 5000 Å for two atmosphere structures and compare the position of the inflection points with the radius at τ5000 = 1 (τRoss =2/3). The calculated difference between the seismic radius and the inflection point is 0.347 ± 0.006 Mm with respect to τ5000 = 1, and 0.333 ± 0.008 Mm with respect to τRoss =. We conclude that the standard solar radius in evolutionary models has to be lowered by 0.333 ± 0.008 Mm and is 695.66 Mm. Furthermore, this correction reconciles inflection point measurements and the seismic radii within the uncertainties.

Original languageEnglish (US)
Pages (from-to)L53-L56
JournalAstrophysical Journal
Volume675
Issue number1 PART 2
DOIs
StatePublished - 2008
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Astrometry
  • Radiative transfer
  • Sun: fundamental parameters
  • Sun: photosphere

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