Helioseismology and the solar age

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dc.creatorDziembowski, W. A.
dc.creatorFiorentini, G.
dc.creatorRicci, B.
dc.creatorSienkiewicz, R.
dc.date1998-09-28
dc.date.accessioned2026-07-07T02:28:06Z
dc.date.available2026-07-07T02:28:06Z
dc.descriptionThe problem of measuring the solar age by means of helioseismology hasbeen recently revisited by Guenther & Demarque (1997) and by Weiss & Schlattl (1998). Different best values for $t_{\rm seis}$ and different assessment of the uncertainty resulted from these two works. We show that depending on the way seismic data are used, one may obtain the value $t_{\rm seis}\approx 4.6$ Gy, close to the age of the oldest meteorites, $t_{\rm met}=4.57$ Gy, like in the first paper, or above 5 Gy like in the second paper. The discrepancy in the seismic estimates of the solar age may be eliminated by assuming higher than the standard metal abundance and/or an upward revision of the opacities in the solar radiative interior.We argue that the most accurate and robust seismic measure of the solar age are the small frequency separations, $D_{\ell,n}=ν_{l,n}-ν_{\ell+1,n-1}$, for spherical harmonic degrees $\ell=0,2$ and radial orders $n\gg\ell$.The seismic age inferred by minimization of the sum of squared differences between the model and the solar small separations is $t_{\rm seis}=4.66\pm0.11$, a number consistent with meteoritic data.Our analysis supports earlier suggestions of using small frequency separations as stellar age indicators.
dc.description8 pages + 4 ps figures included, LaTeX file with l-aa.sty, submitted to Astronomy and Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/9809361
dc.identifierhttp://arxiv.org/abs/astro-ph/9809361
dc.identifierAstron.Astrophys. 343 (1999) 990
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/12976
dc.subjectAstrophysics
dc.titleHelioseismology and the solar age
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