Star-disk alignment in the protoplanetary disks: SPH simulation of the collapse of turbulent molecular cloud cores

Abstract

We perform a series of three-dimensional smoothed particle hydrodynamics (SPH) simulations to study the evolution of the angle between the protostellar spin and the protoplanetary disk rotation axes (the star-disk angle ${\psi }_{\mathrm{sd}}$) in turbulent molecular cloud cores. While ${\psi }_{\mathrm{sd}}$ at the protostar formation epoch exhibits broad distribution up to $\sim 130^{\circ }$, ${\psi }_{\mathrm{sd}}$ decreases ($\lesssim 20^{\circ }$) in a timescale of $\sim 10^4$ yr. This timescale of the star-disk alignment, $t_{\mathrm{alignment}}$, corresponds basically to the mass doubling time of the central protostar, in which the protostar forgets its initial spin direction due to the mass accretion from the disk. Values of ${\psi }_{\mathrm{sd}}$ both at $t=10^2$ yr and $t=10^5$ yr after the protostar formation are independent of the ratios of thermal and turbulent energies to gravitational energy of the initial cloud cores: $\alpha =E_{\mathrm{thermal}}/|E_{\mathrm{gravity}}|$ and ${\gamma }_{\mathrm{turb}}=E_{\mathrm{turbulence}}/|E_{\mathrm{gravity}}|$. We also find that a warped disk is possibly formed by the turbulent accretion flow from the circumstellar envelope.

Accepted for publication in MNRAS (16 pages, 16 figures, 2 tables)

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