Physics
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23r.126p&link_type=abstract
Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 126-127
Physics
Scientific paper
Low mass stars as the Sun, have had during their first million years of life a large interaction with the accretion disk resulting in the star formation. This interaction which consists in a magnetic connection between the central star and the disk results in an important braking of the star rotation. Later, the disk is disintegrated and a spin up process appears. Much later, magnetic winds will again produce a spin down which will result in the more or less slow Main Sequence (MS) rotations. Despite the tremendous increase of measured periods of rotation in Pre Main Sequence Stars (PMS) during these recent years and theoretical advances, the physics at the end of the disk lifetime remains obscure. We are tackling this problem by considering first, which will be the response of the star rotation when a disk has decreased its accretion rate to a minimum value; this is expected to happen at the end of disk lifetime, observationally inferred to happen at an age of near 10 Myr. For this, we have used the model of Cameron and Campbell (1993) which enable to change the accretion rate with the time. After reproducing the rotation rates of Cameron and Campbell we have introduced an emerging radiative core in the star expected to be produced at this age, by means of two polytropes, one representing this core and the second, the convective envelope. A new distribution of internal energy of the star is formed that produces a linear decrease (independently of the values of initial accretion rates) of the stellar moment of inertia. Nevertheless always maintaining the global virialized equilibria. We have detected a new spin up process due to this internal stellar effect. Future studies will consider which will be the effect when a clearing mass of the disk is considered.
de La Reza Ramiro
Pinzon Giovanni
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