*pyshtools* has dedicated classes for working with gravitational and magnetic field data. These classes extend the functionality of the classes `SHCoeffs`

and `SHGrid`

by adding several standard operations related to potential fields. Specific operations include the computation of the geoid, the computation of the three vector components of the gravitational and magnetic fields, the computation of the gravity and magnetic field tensor and eigenvalues, and the computation of the gravitational potential from relief along an interface.

To start using the gravity and magnetic field classes, first import the standard *matplotlib* package, the *pyshtools* package, and the *pyshtools* subpackage *constant*:

In [1]:

```
import matplotlib.pyplot as plt
import pyshtools as pysh
from pyshtools import constants
```

In [2]:

```
pysh.utils.figstyle(rel_width=0.75)
%config InlineBackend.figure_format = 'retina' # if you are not using a retina display, comment this line
```

Operations on gravity fields are performed using the classes `SHGravCoeffs`

, `SHGravGrid`

, `SHGravTensor`

, and `SHGeoid`

. In gereral, the coefficients are stored in an `SHGravCoeffs`

class instance, and this instance is used to initialize the other classes with global grids.

There are several ways to initialize an `SHGravCoeffs`

class instance:

`SHGravCoeffs.from_zeros()`

- Set the degree 0 term to 1 and all other coefficients to zero.`SHGravCoeffs.from_array()`

- Import a*numpy*array of spherical harmonic coefficients.`SHGravCoeffs.from_file()`

- Read coefficients from a file.`SHGravCoeffs.from_random()`

- Initialize the coefficients as random variables with a given power spectrum.`SHGravCoeffs.from_shape()`

- Compute the gravitational potential coefficients from relief along an interface.

Unlike `SHCoeffs`

, when initializing an `SHGravCoeffs`

class instance, it is necessary to specify the attributes `gm`

, `r0`

, and optionally `omega`

, for the GM, reference radius of the coefficients, and the angular rotation rate of the body.

Alternatively, the `SHGravCoeffs`

class can be initialized using the pyshtools module *datasets*. When accessing a dataset, the file will first be downloaded from the original source and then stored in the pyshtools subdirectory of the userâ€™s cache directory (if it had not been done previously). The file hash will be verified to ensure that it has not been modified, and the file will then be used to initialize the class along with the necessary metadata. Here, we will make use of the GMM-3 gravity model of Genova et al. (2016):

In [3]:

```
clm = pysh.datasets.Mars.GMM3()
```

We can inspect this class instance by using the `info()`

method, by `print(clm)`

, or simply by entering the name of the class instance at the prompt:

In [4]:

```
clm.info()
```

Using the `constants`

submodule, we set the angular rotation rate of the planet, which is necessary when calculating the normal gravity and geoid. We also define variables for the planet's reference ellipsoid, such as the semimajor axis `a`

, the flattening `f`

, and the reference potential `u0`

:

In [5]:

```
clm.set_omega(constants.Mars.omega.value)
a = constants.Mars.a.value
f = constants.Mars.f.value
u0 = constants.Mars.u0.value
```

The spectrum of the function can be plotted using the methods `plot_spectrum()`

and `plot_spectrum2d()`

. Unlike `SHCoeffs`

class instances, we have the option of plotting the power spectrum of the geoid (default), potential, radial gravity, or total gravitational field as specified by the optional parameter `function`

. The total spectrum is analogous to the Lowes-Mauersberger spectrum of magnetic fields.

In [6]:

```
fig1, ax1 = clm.plot_spectrum(function='geoid', show=False)
fig2, ax2 = clm.plot_spectrum2d(function='total', show=False)
```

If the errors of the gravitational potential are set, `plot_spectrum()`

will compute automatically and plot the error spectrum. For `plot_spectrum2d()`

, the errors can be plotted by specifying `errors=True`

. By default, the power associated with the degree 0 and 1 terms will not be plotted, because the degree 0 term is orders of magnitude larger than the others, and the degree-1 terms are zero when in center-of-mass coordinates.

Next, we use the method `expand()`

to calculate grids of the gravitational potential, the three vector components of the gravity field, and the total gravity disturbance. By default, these values are calculated on a sphere whose radius is equal to the reference radius `r0`

. By specifying the parameters `a`

and `f`

, these quantities will instead be calculated on a flattened ellipsoid. In this case, it should be emphasized that the vector components still correspond to the spherical coordinate unit vectors $\hat{r}$, $\hat{\theta}$, and $\hat{\phi}$, and not components that are perpendicular to the reference ellipsoid. By default, the normal gravity is removed from the total gravitational acceleration, yielding the gravity disturbance.

The `expand()`

method returns an `SHGravGrid`

class instance. This class stores each of the five grids, `rad`

, `theta`

, `phi`

, `total`

, and `pot`

as `SHGrid`

class instances. The four gravity grids can be plotted together using the method `plot()`

:

In [7]:

```
grav = clm.expand(lmax=95, a=a, f=f)
fig2, ax2 = grav.plot(show=False)
```

Individual maps can be plotted using the corresponding methods `plot_rad()`

, `plot_theta()`

, `plot_phi()`

, `plot_total()`

, and `plot_pot()`

. Here, we plot the total gravity disturbance, and use the parameters `cmap`

and `cmap_limits`

to set the minimum and maximum values and color scale, respectively:

In [8]:

```
fig3, ax3 = grav.plot_total(cmap='RdBu_r',
cmap_limits=[-400, 600],
show=False)
```