Other
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23r.133s&link_type=abstract
Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 133-134
Other
Scientific paper
Classical T Tauri stars (CTTSs) are young stars that exhibit emission lines, together with excess continuum emission that ranges from the infrared to the ultraviolet. According to current models of CTTSs, the steady migration of the gas in a circumstellar accretion disk is suddenly halted at a few stellar radii by the stellar magnetic field (Uchida & Shibata 1984; Camenzind 1990; Königl 1991; Shu et al. 1994). Material then free falls onto the star, guided by stellar magnetic field lines. The permitted emission lines are thought to be produced in the magnetic funnel flow. When the accretion material hits the stellar surface, the strong continuum excess (veiling) is produced. We present veiling and emission lines fluxes measurements for the T Tauri GQ Lupi, observed during eighteen consecutive nights in February of 1999 at ESOs 1.52m telescope and with Boller & Chivens spectrograph, in the ESO-ON agreement. The veiling showed a variation through the nights with period of about twelve days, the same result found in Batalha, Lopes, Batalha (2001), BLB. The emission line fluxes correlate each other, indicating that they are forming in a common region. The inverse P Cygni profile, which was very strength in BLB, disappeared in our observations. Muzerolle, Calvet & Hartmann (2001), MCH, reported theoretical lines profiles for different values of spot temperature, accretion rate and the disk inclination. We compare our observed profiles with MCH theoretical profiles to obtain the better configuration of GQ Lupi star and try to explain the cyclic behavior of the veiling.
Batalha C. C.
Lopes Denivaldo
Seperuelo E.
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