Filamentary structure and helical magnetic fields in the environment of a starless dense core

The environment of L1512, a starless dense core, has been mapped at high an gular resolution in the (CO)-C-12 (J = 2-1) line over more than 1 pc, with a few positions observed in the (CO)-C-12 (J = 3-2) and (J = 4-3) lines. Th e gas outside the dense core is structured in several filaments, roughly 1 pc long and similar to0.1 pc thick, converging at the dense core position. Small longitudinal (similar to1 km s(-1) pc(-1)) but large transverse (up t o 8 km s(-1) pc(-1)) velocity gradients are observed. Remarkably, the trans verse gradients can be seen to change sign periodically, along at least one of the filaments. Thus, there are oscillations in the toroidal velocity wi thin the filaments, which may be a signature of a magnetohydrodynamic insta bility developing in filaments permeated by a helical magnetic field. In th e case of L1512, according to the analysis of Fiege & Pudritz, the growth r ate of the instability is low, corresponding to a timescale of the order of 1 Myr. We deduce from the wavelength of the oscillations that the toroidal component of the magnetic field dominates the poloidal component. The toro idal component helps confine the filaments, which are not otherwise confine d by self-gravity (m/m(vir) similar to 0.2), by the pressure of the galacti c H I layer, or by external turbulent pressure. We find that the velocity g radients in the vicinity of the dense core provide an estimate for an upper limit to the accretion rate onto the dense core of (M) over dot = 4 x 10(- 6) M-. yr(-1). For the gas characteristics in the filaments, we find that a broad range of density and temperature is allowed for the gas, from n(H2) = 2 x 10(3) cm(-3) for the coldest case (T-k = 20 K) down to n(H2) = 180 cm (-3) for the warmest (T-k = 250 K).