README.md

---
language:
- en
license: cc-by-4.0
tags:
- physics

task_categories:
- time-series-forecasting
- other
task_ids:
- multivariate-time-series-forecasting
---

# How To Load from HuggingFace Hub

1. Be sure to have `the_well` installed (`pip install the_well`)
2. Use the `WellDataModule` to retrieve data as follows:

```python
from the_well.benchmark.data import WellDataModule

# The following line may take a couple of minutes to instantiate the datamodule
datamodule = WellDataModule(
    "hf://datasets/polymathic-ai/",
    "MHD_64",
)
train_dataloader = datamodule.train_dataloader()

for batch in dataloader:
    # Process training batch
    ...
```

# Magnetohydrodynamics (MHD) compressible turbulence

**NOTE:** This dataset is available in two different resolutions \\(256^3\\) for `MHD_256` and \\(64^3\\) for `MHD_64`. The data was first generated at \\(256^3\\) and then downsampled to \\(64^3\\) after anti-aliasing with an ideal low-pass filter. The data is available in both resolutions.

**One line description of the data:** This is an MHD fluid flows in the compressible limit (subsonic, supersonic, sub-Alfvenic, super-Alfvenic).

**Longer description of the data:** An essential component of the solar wind, galaxy formation, and of interstellar medium (ISM) dynamics is magnetohydrodynamic (MHD) turbulence. This dataset consists of isothermal MHD simulations without self-gravity (such as found in the diffuse ISM) initially generated with resolution \\(256^3\\) and then downsampled to \\(64^3\\) after anti-aliasing with an ideal low-pass filter. This dataset is the downsampled version.

**Associated paper**: [Paper](https://iopscience.iop.org/article/10.3847/1538-4357/abc484/pdf)

**Domain expert**: [Blakesley Burkhart](https://www.bburkhart.com/), CCA, Flatiron Institute & Rutgers University.

**Code or software used to generate the data**: Fortran + MPI.

**Equation**:
```math
\begin{align}
\frac{\partial \rho}{\partial t} + \nabla \cdot (\rho \mathbf{v}) &= 0 \nonumber\\
\frac{\partial \rho \mathbf{v}}{\partial t} + \nabla \cdot (\rho \mathbf{v} \mathbf{v} - \mathbf{B} \mathbf{B}) + \nabla p &= 0 \nonumber\\
\frac{\partial \mathbf{B}}{\partial t} - \nabla \times (\mathbf{v} \times \mathbf{B}) &= 0 \nonumber\\
\end{align}
```
where \\(\rho\\) is the density, \\(\mathbf{v}\\) is the velocity, \\(\mathbf{B}\\) is the magnetic field, \\(\mathbf{I}\\) the identity matrix and \\(p\\) is the gas pressure.

![Gif](https://users.flatironinstitute.org/~polymathic/data/the_well/datasets/MHD_64/gif/density_unnormalized.gif)

| Dataset    | FNO | TFNO  | Unet | CNextU-net
|:-:|:-:|:-:|:-:|:-:|
| `MHD_64`  | 0.3605 | 3561 |0.1798|\\(\mathbf{0.1633}\\)|

Table: VRMSE metrics on test sets (lower is better). Best results are shown in bold. VRMSE is scaled such that predicting the mean value of the target field results in a score of 1.

# About the data

**Dimension of discretized data:** 100 timesteps of 64 \\(\times\\) 64 \\(\times\\) 64 cubes.

**Fields available in the data:** Density (scalar field), velocity (vector field), magnetic field (vector field).

**Number of trajectories:** 10 Initial conditions x 10 combination of parameters = 100 trajectories.

**Estimated size of the ensemble of all simulations:** 71.6 GB.

**Grid type:** uniform grid, cartesian coordinates.

**Initial conditions:** uniform IC.

**Boundary conditions:** periodic boundary conditions.

**Data are stored separated by (\\(\Delta t\\)):** 0.01 (arbitrary units).

**Total time range (\\(t\_{min}\\) to \\(t\_{max}\\)):** \\(t\_{min} = 0\\), \\(t\_{max} = 1\\).

**Spatial domain size (\\(L_x\\), \\(L_y\\), \\(L_z\\)):** dimensionless so 64 pixels.

**Set of coefficients or non-dimensional parameters evaluated:** all combinations of \\(\mathcal{M}_s=\\){0.5, 0.7, 1.5, 2.0 7.0} and \\(\mathcal{M}_A =\\){0.7, 2.0}.

**Approximate time and hardware used to generate the data:** Downsampled from `MHD_256` after applying ideal low-pass filter.

# What is interesting and challenging about the data:

**What phenomena of physical interest are catpured in the data:** MHD fluid flows in the compressible limit (sub and super sonic, sub and super Alfvenic).

**How to evaluate a new simulator operating in this space:** Check metrics such as Power spectrum, two-points correlation function.

Please cite the associated paper if you use this data in your research:

```
@article{burkhart2020catalogue,
  title={The catalogue for astrophysical turbulence simulations (cats)},
  author={Burkhart, B and Appel, SM and Bialy, S and Cho, J and Christensen, AJ and Collins, D and Federrath, Christoph and Fielding, DB and Finkbeiner, D and Hill, AS and others},
  journal={The Astrophysical Journal},
  volume={905},
  number={1},
  pages={14},
  year={2020},
  publisher={IOP Publishing}
}
```