Jonathan Carroll-Nellenback University of Rochester

Actively developed at the University of Rochester Written primarily using Fortran Parallelized with MPI Grid-based AMR with arbitrary sized grids Conserves mass, momentum, energy and  B Implements various Riemann solvers, reconstruction methods, etc… Supports thermal conduction, self-gravity, sink particles, resistivity, viscosity, and various cooling functions. Integrated trac-wiki system with extensive documentation, ticketing system, blog posts, etc…

Parallelization of AMR code AstroBEAR Threaded AMR Scaling Results Examples of Multi-Physics with AstroBEAR Interaction between magnetized clumps and radiative shocks. Anistropic heat conduction Magnetic Towers Disk formation around binaries Effect of inhomogeneities within Colliding flows

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A S P OA S A S R OA S P OA S A S R A S P OA S A S R A S P OA S A S R A S P R O O P A S R A S P R O Level 0 Threads Level 1 Threads Level 2 Threads Control Thread

A S P OA S A S R OA S P OA S A S R A S P OA S A S R A S P OA S A S R A S P R O O P A S R A S P R O Serial Execution Good performance requires load balancing every step Threaded Execution Good performance requires global load balancing across AMR levels

Balancing each level requires having enough grids to distribute among all of the processors – or artificially fragmenting grids into smaller pieces.

Global load balancing allows for greater parallelization and allows processors to have a few larger grids instead of multiple small grids.

For some problems, time derivatives from coarse grids are needed to update fields on finer grids (ie Gravitational Potential) If we want to thread the various level advances there are two options. Use old time derivatives from the previous coarse step. Should work fine as long as value of derivatives at boundaries between levels has a “small” 2 nd time derivative. Lag lower level advances by 1 level time step (ie Advance level 0 from 2  t to 3  t while advancing level 1 from 1  t to 2  t, level 2 from.5  t to 1.5  t. Level 3 from.25  t to 1.25  t and so on. Results in postponed restriction.

Problems involving magnetized clouds and clumps, especially their interaction with shocks are common in astrophysical environments and have been a topic of research in the past decade. Using AstroBEAR, we set up an initial state with magnetized clumps of different contained magnetic field configurations and drive strong shocks through them. In the simulations… Clump density contrast is 100, Wind Mach is 10. The clump is magnetic dominated. Radiative cooling is strong.

The poloidal contained case opens up quickly with a shaft shaped core. Smaller clumps are formed after shock with a very turbulent downstream.

The toroidal contained case collapses onto the axis, making the shocked clump resembles a “nose cone”.

Interfaces between hot and cold magnetized plasmas exist in various astrophysical contexts. It is of interest to understand how the structure of the magnetic field spanning the interface affects the temporal evolution of the temperature gradient. We explore the relation between the magnetic field topology and the heat transfer rate by adding various fractions of tangled versus ordered field across a hot–cold interface that allows the system to evolve to a steady state. In the simulations… We set up a sharp hot-cold gradient with helical magnetic field surrounding the interface. The rest of the box is filled with magnetic field aligned with the temperature gradient. The anisotropic heat conduction only conducts heat along field lines. Li, S., Frank, A., Blackman, E. ApJ

What we observe… Initially, the heat transport only happens locally around the interface, since it is confined by the small scale field loops. As the simulation goes on, the helical field loops begin to open up and reconnect, which serve as channels for heat transport from hot region to cold region. By adding straight field components to the helical field loops, the heat transfer rate of the interface can be speeded up.

z r inj Stellar jets. Density = 100 cm-3 Temperature = K γ =5/3 V = 0 km s-1 Magnetic fields only within the central region. Jet only develops because of magnetic pressure gradients. Continuous Poynting flux injection. r

primary secondary c. of mass co-rotating grid 3D, cubic co-rotating grid with cartesian coordinates AMR only about the secondary Inflow wind solution BC (-x,+y,+-z) to simulate the primary’s AGB with spherical wind (v ~ 10km/s, mass loss ~ M sun /yr) and M 1 =1.5M sun Outflow boundary conditions (+x,-y) Bound circular orbit Sink particle to simulate the Secondary: accretor with M 2 =M sun Separations within 10-40AU gamma= ; isothermal

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