Computer Science – Numerical Analysis
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..607l&link_type=abstract
MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp
Computer Science
Numerical Analysis
Pre-Main-Sequence Stars, Magnetic Fields, Stellar Rotation, Stellar Structure, Stellar Evolution, Numerical Analysis, Main-Sequence: Late-Type Stars, Magnetic And Electric Fields, Polarization Of Starlight, Stellar Rotation, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages
Scientific paper
Magnetic fields are at the heart of the observed stellar activity in late-type stars, and they are presumably generated by a dynamo mechanism at the interface layer (tachocline) between the radiative core and the base of the convective envelope. Since dynamo models are based on the interaction between differential rotation and convective motions, the introduction of rotation in the ATON 2 . 3 stellar evolutionary code gives us the opportunity to begin explorations regarding a physically consistent treatment of magnetic effects in stellar structure and evolution, in spite of the formidable mathematical and numerical challenges involved.
As an example of such explorations, we present theoretical estimates of the convective turnover time τc for rotating pre-main sequence solar-type stars, based on up-to-date input physics for stellar models. Those estimates, as opposed to the use of empirically derived values of τc for such matters, can be used to calculate the Rossby number Ro, which is related to the magnetic activity strength in dynamo theories and, at least for main-sequence stars, shows an observational correlation with stellar activity. More important, they can also contribute for testing stellar models against observations.
Landin Natália R.
Mendes Luiz T. S.
Vaz Luiz Paulo Ribeiro
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