Magnetohydrodynamic Simulations of Disk-Magnetized Star Interactions in the Quiescent Regime: Funnel Flows and Angular Momentum Transport

By M. Romanova, G. V. Ustyugova, Alexander V. Koldoba, R. Lovelace. 2002

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Magnetohydrodynamic (MHD) simulations have been used to study disk accretion to a rotating magnetized star with an aligned dipole moment. Quiescent initial conditions were developed in order to avoid the fast initial evolution seen in earlier studies. A set of simulations was performed for different stellar magnetic moments and rotation rates. Simulations have shown that the disk structure is significantly changed inside a radius rbr where magnetic braking is significant. In this region the disk is strongly inhomogeneous. Radial accretion of matter slows as it approaches the area of strong magnetic field, and a dense ring and funnel flow (FF) form at the magnetospheric radius rm, where the magnetic pressure is equal to the total, kinetic plus thermal, pressure of the matter. FFs, where the disk matter moves away from the disk plane and flows along the stellar magnetic field, are found to be stable features during many rotations of the disk. The dominant force driving matter into the FF is the pressure gradient force, while gravitational force accelerates it as it approaches the star. The magnetic force is much smaller than the other forces. The FF is found to be strongly sub-Alfvénic everywhere. The FF is subsonic close to the disk, but it becomes supersonic well above the disk. Matter reaches the star with a velocity close to that of free fall. Angular momentum is transported to the star dominantly by the magnetic field. In the disk the transport of angular momentum is mainly by the matter, but closer to the star the matter transfers its angular momentum to the magnetic field, and the magnetic field is dominant in transporting angular momentum to the surface of the star. For slowly rotating stars we observed that magnetic braking leads to the deceleration of the inner regions of the disk, and the star spins up. For a rapidly rotating star, the inner regions of the disk rotate with a super-Keplerian velocity, and the star spins down. The average torque is found to be zero when the corotation radius rcor ≈ 1.5rm. The evolution of the magnetic field in the corona of the disk depends on the ratio of magnetic to matter energies in the corona and in the disk. Most of the simulations were performed in the regime of a relatively dense corona where the matter energy-density was larger than the magnetic energy-density. In this case the coronal magnetic field gradually opens, but the velocity and density of outflowing matter are small. In a test case where a significant part of the corona was in the field-dominated regime, more dramatic opening of the magnetic field was observed with the formation of magnetocentrifugally driven outflows. Numerical applications of our simulation results are made to T Tauri stars. We conclude that our quasi-stationary simulations correspond to the classical T Tauri stage of evolution. Our results are also relevant to cataclysmic variables and magnetized neutron stars in X-ray binaries.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e5bb98be5a089467f9daa580b95d68edcba1a107

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Citations in the corpus

Locking of the Rotation of Disk-Accreting Magnetized Stars (2005, background): “…the innermost field lines reconnect to form a closed magnetosphere, and some of them open and close again in a recurrent manner (Goodson & Winglee 1997; Goodson, Winglee & Böhm 1999; Romanova et al. 2002, hereafter RUKL; Romanova et al. 2004; Kato et al. 2004, Von Rekowski & Brandenburg 2004).”
Magnetospheric accretion-ejection processes in the classical T Tauri star AA Tauri (2006, background): “–3396 CCD V S. Hodgkin Canarias 28 magnetic fields, leading to a magnetospheric cavity extending over a few stellar radii (e.g. Romanova et al. 2002, 2003).”
“Propeller” Regime of Disk Accretion to Rapidly Rotating Stars (2006, methodology): “Nevertheless, we have found it efficacious to start with the poloidal dipole field, and let the system evolution open the field lines (see also Romanova et al. 2002).”
Which jet launching mechanism(s) in T Tauri stars (2006, background): “As observed by Romanova et al. (2002), when plasma inertia is important (full MHD equations), this violent opening of the field lines is not obtained.”
Launching of conical winds and axial jets from the disc–magnetosphere boundary: axisymmetric and 3D simulations (2009, background): “…reconnection has been discussed theoretically (Aly & Kuijpers 1990; Uzdensky, Königl & Litwin 2002) and has been observed in a number of axisymmetrtic simulations (Hirose et al. 1997; Goodson et al. 1997, 1999; Matt et al. 2002; Romanova et al. 2002 hereafter R02; von Rekowski & Brandenburg 2004).”
Magnetic Fields of Nondegenerate Stars (2009, background): “…observations, in particular the typical sizes of magnetospheric gaps and rotation periods of cTTSs. Initially restricted to dipolar magnetospheres (Romanova et al. 2002; von Rekowski & Brandenburg 2004; Bessolaz et al. 2008), simulations and models now incorporate more complex fields resembling…”
Accretion to magnetized stars through the Rayleigh–Taylor instability: global 3D simulations (2008, methodology): “To model stationary accretion, the disk is chosen to initially be in a quasi-equilibrium state, where the gravitational, centrifugal and pressure gradient forces are in balance (Romanova et al. 2002).”
Accretion-powered Stellar Winds as a Solution to the Stellar Angular Momentum Problem (2005, unknown): “…of Figure 1, as well as the possibility that the most significant spin-down torques on the star originate from open stellar field lines, is well-supported by the numerical MHD simulations of Goodson & Winglee (1999) and von Rekowski & Brandenburg (2004, 2005, but see Romanova et al. 2002).”
On the formation of Hα line emission around classical T Tauri stars (2006, methodology): “Journal compilation C© 2006 RAS Downloaded from https://academic.oup.com/mnras/article-abstract/370/2/580/967210 by guest on 30 July 2018 Romanova et al. 2002).”