Raquel M. G. Albuquerque
IA

Abstract
Classical T Tauri stars (CCTS) are young solar-type stars that have been known by their enigmatic angular momentum evolution. In order for a young Stellar Object (YSO) grow-up and maintain its equilibrium simultaneously, besides accreting matter, it also needs to eject part of it in the form of outflows (stellar winds, jets, magnetospheric ejections,...). By knowing how these accretion/outflow mechanisms occur and evolve, it will possible to better understand the origins of the Solar System. CTTS have been studied both observationally and theoretically. Observations allow astronomers to characterize these stars through mass, temperature, radius, accretion/outflow velocities and accretion rates that are encoded in their emission lines. On the other hand, theoretical studies provide analytical models through magnetohydrodynamics (MHD), which is the fundamental structure to develop steady and time-dependent numerical simulations. By figuring out the relevance of some physical quantities involved, it will be possible to replicate the observations made so far. In this Cookie seminar, I will focus both on observational and theoretical perspectives. Firstly, I will explore some of the spectral features present in a sample of CTTS and infer about mass accretion rates and characterize their outflow dynamics. Secondly, I will show some of the results regarding the structure modelling of magnetospheres made with PLUTO code, in collaboration with researchers from the Observatory of Paris - LUTH.

2015 October 28, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Classroom)
Rua das Estrelas, 4150-762 Porto