Knowledge of the solar core dynamics through g modes

Details Knowledge of the solar core dynamics through g modes Knowledge of the solar core dynamics through g modes

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..17e...8g&link_type=abstract

Highlights of Recent Progress in the Seismology of the Sun and Sun-Like Stars, 26th meeting of the IAU, Joint Discussion 17, 23

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Helioseismology is able to study the solar interior through the observation of the solar oscillation modes propagating inside the Sun. Pressure-driven modes (p modes) provide a very detailed picture of the external convective zone above 0.7 R[&sun;]and the radiative zone down to ~0.2 R[&sun;] where only a few of such modes penetrate so far. To study deeper layers, still containing more than 40% of the totals mass, another type of oscillations are needed: the gravity-driven modes (g modes). Since the early 19 80s, this type of mode has been looked for. Only very recently have we have found some structures that are compatible with some global properties of these modes in the GOLF/ SOHO data. In this contribution we will show these signals. By explaining them as the signature of the asymptotic properties of the ℓ = 1 g modes, we could start constraining the solar core dynamics.

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