Numerical simulations of hydrodynamics (HD) and magnetohydrodynamics (MHD) are an important part of the CHARMS project. We develop, maintain, and utilize (M)HD codes for this purpose, such as ZeusTW (a locally developed MPI-parallel version of Zeus3D, able to do non-ideal MHD, tuned to study various problems in jet, disk and star formation, detailed below), local versions of Zeus2D (tuned for the study of jets and outflows, see, e.g., Shang et al. 2006), and Pluto (currently utilized with problem sets prepared to study outflows and magnetic reconnections, see, e.g., Čemeljić & Huang 2014).
The Code: ZeusTW
Code Descriptions (Krasnopolsky, Li, & Shang 2010, ApJ)
ZeusTW, written in idiomatic Fortran95, is based on the “Zeus36” code (Krasnopolsky et al. 1999, 2003), itself derived from Zeus3D (LCA version 3.4.2; Clarke et al. 1994); Zeus36 is parallel by domain decomposition and utilizes dynamic memory for its field and grid arrays. A small memory pool of temporary arrays replaces the worker arrays of Zeus3D, increasing programming flexibility at essentially zero runtime cost. ZeusTW adds to Zeus36 the ability to solve many non-ideal MHD problems in an explicit form, covering the ohmic (η), Hall (Q), and ambipolar diffusion (α) terms:
ZeusTW can solve MHD/HD equations in Cartesian, spherical, and cylindrical coordinates with a variety of equations of states, including isothermal, adiabatic, and polytropic. A Poisson solver for self-gravity is included. Recent development includes locally isothermal equations of states on a tracer field, a viscosity module, and a simple Bremsstrahlung cooling module.
Ohmic Resistivity (Krasnopolsky, Li, & Shang 2010, ApJ)
To treat the ohmic term relevant for this paper, we used a resistivity algorithm based on Fleming et al. (2000), which includes subcycling. We tested the code by diffusing an initial Gaussian profile in Cartesian geometry, in one, two, and three dimensions. We also tested slightly different forms of the algorithm (such as changing the operator splitting by calculating the current density J before or after the magnetic field B is updated), and different subcycling prescriptions (such as varying the maximum number of ohmic subcycles from 1 to 100). The code passed all of these tests.
The most resistive model (as in the figure) differs drastically from the lower resistivity cases and produces a rotationally-supported disk (RSD) of radius ~150 AU at the representative time t = 1012 s. The disk has a mass ~0.01 M☉ at t = 1012 s, corresponding to an average accretion rate (from the envelope to the disk) ~5 × 10−7 M☉ yr−1.
Hall Effect (Krasnopolsky, Li, & Shang 2011, ApJ)
Including a Hall term with a coefficient Q ≳ 3 × 1020 cm2 s−1 G−1 in the induction equation enables an RSD of radius ≳ 10 AU to form. The RSD is formed not because the Hall effect has reduced the efficiency of the magnetic braking; rather, it is produced because the Hall effect actively spins up the inner part of the equatorial material to Keplerian speed. The spin-up comes about because the collapsing envelope drags the magnetic field into a highly pinched configuration near the equator, producing a large toroidal electric current density, which forces the field lines to rotate differentially due to the Hall effect. The resulting twist of field lines yields the magnetic torque that spins up the equatorial material, even in the absence of any initial rotation. When the magnetic field orientation is flipped, the direction of disk rotation is reversed as well. The implication is that the Hall effect can in principle produce both regularly rotating and counter-rotating disks around protostars.
Ambipolar Diffusion (Li, Krasnopolsky, & Shang 2011, ApJ)
Ambipolar diffusion (AD) is treated using the explicit method described in Mac Low et al. (1995), as in Mellon & Li (2009). The magnetic field is evolved using a velocity that is the sum of the bulk neutral velocity v and an ion-neutral “drift” velocity ΔvAD.
The equatorial infall is initially slowed down near a relatively large radius. It corresponds to the edge of the magnetic bubble inflated by magnetic braking, where a magnetic barrier forces the collapsing material over a large solid angle into a narrow equatorial channel. Upon passing through the barrier, the material resumes rapid radial infall, spinning up as it collapses, until a second barrier is encountered. This second barrier is induced by AD, which enables the magnetic field lines to decouple from matter and pile up outside the central object as the matter accretes onto the protostar. The piled-up magnetic field drives a C-shock, slowing down the accretion flow to a subsonic speed. The slowdown of infall leads to a high density in the post-shock region. Upon passing through the shock, the equatorial material re-accelerates toward the central object, reaching a highly supersonic infall speed at small radii.
Molecular Jets and Outflows from Earliest Phases
Based on the unified wind model of Shang et al. (2006), kinematics and structures of molecular outflows from low-mass young stars are studied with various levels of magnetization and temperature of the outflows propagating into a cold isothermal toroid. Toroidal field pinches and collimates the inner part of the outflow into axially concentrated jet, while higher temperature along with lower field strength operates the opposite. Moreover, the poloidal field in the toroid helps to prevent corrugation in wind-ambient interaction regions and produces a thicker swept-up shell. Synthetic properties of protostellar outflows in the youngest phases are investigated by the two-temperature unified outflow models with toroidal and poloidal fields including mass–velocity profiles, position–velocity profiles, intensity–velocity profiles of important molecular lines from CO and SiO. The Class 0 source IRAS 04166+2706, as an archetypical case of possessing molecular jets and outflows in CO and SiO, serves as a case study of the ejection history under the framework of the unified wind model.
Magnetized Gravitational Collapse and Formation of Earliest Disks
Disk formation in magnetized cloud cores is largely hindered by magnetic braking. Additional effects are needed to weaken the magnetic braking and enable the formation of persistent, rotationally supported, protostellar disks. A series of papers were published to investigate the effects of non-ideal MHD effects, including the first attempts to investigate the effect of enhanced ohmic dissipation and that of the Hall effect. Besides non-ideal MHD effects, the misalignment between the magnetic field axis and rotational axis may help to form a rotationally supported disk. Moreover, turbulence can be an important way to bypass the magnetic breaking catastrophe by inducing magnetic reconnections and thus reducing the magnetic flux threading the collapsing cloud core. An alternative interpretation is advanced, based on magnetic decoupling-triggered reconnection of severely pinched field lines close to the central protostar and turbulence-induced warping of the pseudodisk.
Ring and Gap Formation in Wind-Launching Disks
State-of-the-art observational facilities are providing increasingly stringent constraints on the physical properties of circumstellar discs. Specifically, the Atacama Large Millimeter/submillimeter Array (ALMA) has shown that a large number of circumstellar discs have detailed radial and azimuthal substructures. How the various observed structures form remains undetermined, though a number of promising physical mechanisms have been proposed. Previous axisymmetric investigations in two dimensions (2D) have shown that rings and gaps develop naturally in non-ideal magnetohydrodynamic disc–wind systems, especially in the presence of ambipolar diffusion. These 2D simulations were extended to three dimensions (3D) and the rings and gaps are still formed in the presence of a moderately strong ambipolar diffusion from the same basic mechanism that was identified in the 2D simulations, namely, the redistribution of the poloidal magnetic flux relative to the disc material as a result of the reconnection of a sharply pinched poloidal magnetic field lines. As the ambipolar diffusivity decreases, both the disc and the wind become increasingly turbulent, driven by the magnetorotational instability, with tightly wound spiral arms becoming more prominent in the disc.
- Shang H; Liu C-F; Krasnopolsky R; Wang L-Y, “A Unified Model for Bipolar Outflows from Young Stars: Kinematic Signatures of Jets, Winds, and Their Magnetic Interplay with the Ambient Toroids”, ApJ, submitted, 2022 [SCI]
- Wang W; Väisälä MS; Shang H; Krasnopolsky R; Li Z-Y; Lam KH; Yuan F, “Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Fields” , ApJ: 928(1), id.85 (23pp), Mar, 2022 [SCI]
- Zhao B; Caselli P; Li Z-Y; Krasnopolsky R; Shang H; Lam KH, “The Interplay between Ambipolar Diffusion and Hall Effect on Magnetic Field Decoupling and Protostellar Disc Formation” , MNRAS: 505(4), 5142-5163, Aug, 2021 [SCI]
- Shang H; Krasnopolsky R; Liu C-F; Wang L-Y, “A Unified Model for Bipolar Outflows from Young Stars: the Interplay of Magnetized Wide-Angle Winds and Isothermal Toroids”, ApJ: 905(2), id.116 (52pp.), Dec, 2020 [SCI]
- Väisälä MS; Shang H; Krasnopolsky R; Liu S-Y; et al., “Time Evolution of 3D Disk Formation with Misaligned Magnetic Field and Rotation Axes” , ApJ: 873(2), id. 114 (22 pp.), Mar, 2019 [SCI]
- Wang L-Y; Shang H; Chiang T-Y, “Ejection History of the IRAS 04166+2706 Molecular Jet”, ApJ: 874, id. 31 (12 pp.), Mar, 2019 [SCI]
- Yen H-W; Zhao B; Hsieh I-T; Koch P; Krasnopolsky R; Lee C-F; Li Z-Y; Liu S-Y; Ohashi N; Takakuwa S; Tang Y-W; et al., “JCMT POL-2 and ALMA Polarimetric Observations of 6000─100 au Scales in the Protostar B335: Linking Magnetic Field and Gas Kinematics in Observations and MHD Simulations”, ApJ: 871(2), id. 243 (18 pp.), Feb, 2019 [SCI]
- Suriano SS; Li Z-Y; Krasnopolsky R; Suzuki TK; Shang H, “The formation of rings and gaps in wind-launching non-ideal MHD discs: three-dimensional simulations”, MNRAS: 484(1), 107-124, March, 2019 [SCI]
- Suriano SS; Li Z-Y; Krasnopolsky R; Shang H, “The formation of rings and gaps in magnetically coupled disk-wind systems: ambipolar diffusion and reconnection”, MNRAS: 477(1), 1239-1257, June, 2018 [SCI]
- Zhao B; Caselli P; Li Z-Y; Krasnopolsky R, “Decoupling of magnetic fields in collapsing protostellar envelopes and disc formation and fragmentation”, MNRAS: 473(4), 4868-4889, Feb 1, 2018 [SCI]
- Suriano SS; Li Z-Y; Krasnopolsky R; Shang H, “Rings and gaps produced by variable magnetic disc winds and avalanche accretion streams – I. Axisymmetric resistive MHD simulations”, MNRAS: 468(4), 3850-3868, July 11, 2017 [SCI]
- Zhao B; Caselli P; Li Z-Y; Krasnopolsky R; Shang H; Nakamura F, “Protostellar disc formation enabled by removal of small dust grains”, MNRAS: 460(2), 2050-2076, Aug 1, 2016 [SCI]
- Wang L-Y; Shang H; Krasnopolsky R; Chiang T-Y, “A Two-Temperature Model of Magnetized Protostellar Outflows”, ApJ: 815(1), 39, Dec 10, 2015 [SCI]
- Li Z-Y; Krasnopolsky R; Shang H; Zhao B, “On the Role of Pseudodisk Warping and Reconnection in Protostellar Disk Formation in Turbulent Magnetized Cores”, ApJ: 793(2), 130, Oct 1, 2014 [SCI]
- Li Z-Y; Krasnopolsky R; Shang H, “Does Magnetic-field-Rotation Misalignment Solve the Magnetic Braking Catastrophe in Protostellar Disk Formation?”, ApJ: 774(1), 82, Sep 1, 2013 [SCI] ( ADS | Fulltext )
- Krasnopolsky R; Li Z-Y; Shang H; Zhao B, “Protostellar Accretion Flows Destabilized by Magnetic Flux Redistribution”, ApJ: 757(1), 77, Sep 20, 2012 [SCI]
- Li Z-Y; Krasnopolsky R; Shang H, “Non-ideal MHD Effects and Magnetic Braking Catastrophe in Protostellar Disk Formation”, ApJ: 738(2), 180, Sep 10, 2011 [SCI]
- Krasnopolsky R; Li Z-Y; Shang H, “Disk Formation in Magnetized Clouds Enabled by the Hall Effect”, ApJ: 733(1), 54, May 20, 2011 [SCI]
- Krasnopolsky R; Li Z-Y; Shang H, “Disk Formation Enabled by Enhanced Resistivity”, ApJ: 716(2), 1541-1550, Jun 20, 2010 [SCI]
- Shang H; Allen A; Li Z-Y; Liu C-F; Chou M-Y; Anderson J, “A Unified Model for Bipolar Outflows from Young Stars”, ApJ: 649(2), 845-855, Oct 1, 2006 [SCI]