Consequences of the non gaussian character of the stochastic excitation for solar-type oscillations

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dc.creatorSamadi, R.
dc.creatorNordlund, A.
dc.creatorStein, R. F.
dc.creatorGoupil, M. J.
dc.creatorRoxburgh, I.
dc.date2002-10-01
dc.date.accessioned2026-07-07T02:05:31Z
dc.date.available2026-07-07T02:05:31Z
dc.descriptionOur recent study, based on a 3D numerical simulation, suggested that the stochastic excitation of solar p-modes has a non gaussian nature and a non gaussian model was proposed which results in a good agreement between the computed rate $P$ at which p-modes are excited and the solar seismic observational constraints. In the present work, we study some consequences of this non-gaussian model on the rate P at which p-modes are excited in intermediate mass stars (1 Mo < M < 2 Mo). The non gaussian model changes substantially the spectrum of P at high frequency compared with the commonly assumed gaussian model. The largest effects on P are found for stars in the mass range ~ 1.5-1.6 Mo. They are found large enough that observatins in solar-like oscillating stars observed with space based seismology missions (e.g. COROT) will be able to confirm or reject the gaussian nature of stochastic excitation.
dc.description4 pages, 1 figure, proceedings of meeting "SF2A-2002: Semaine de l'Astrophysique Francaise", held in Paris, France, June 2002, to be published by EdP-Sciences, Conference Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0210028
dc.identifierhttp://arxiv.org/abs/astro-ph/0210028
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5126
dc.subjectAstrophysics
dc.titleConsequences of the non gaussian character of the stochastic excitation for solar-type oscillations
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