*pyshtools* has dedicated classes for working with gravitational and magnetic fields. 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]:

```
%matplotlib inline
import matplotlib.pyplot as plt
import pyshtools
from pyshtools import constant
```

In [2]:

```
pyshtools.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.

We start by reading the gravitational potential coefficients and errors for the planet Mars. We make use of the model GMM-3 of Genova et al. (2016), where `r0`

and `gm`

are set by the first two elements of the file's header line. If the file didn't contain a header with this information, these parameters could be specified explicitly by using the keywords `gm`

and `r0`

. We note that the header line of this file uses units of kilometers instead of meters, so we convert the values in the header to meters by specifiying `header_units='km'`

:

In [3]:

```
clm = pyshtools.SHGravCoeffs.from_file('../ExampleDataFiles/gmm3_120_sha.tab', errors=True, header_units='km')
```

Immediately, we receive a warning message because the file did not set the degree-0 spherical harmonic coefficient: when this occurs, *pyshtools* will automatically sets this value to unity. 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 `constant`

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(constant.omega_mars.value)
a = constant.a_mars.value
f = constant.f_mars.value
u0 = constant.u0_mars.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 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 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 `vmin`

, `vmax`

, and `cmap`

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

In [8]:

```
fig3, ax3 = grav.plot_total(vmin=-400, vmax=600, cmap='RdYlBu_r', show=False)
```

Remember, you should **never** use the 'rainbow' and 'jet' colormaps!

The geoid is computed using the `geoid()`

method. By specifying the reference potential (in m$^2$/s$^2$), the height is calculted with respect to a sphere of reference radius `r0`

. This method returns an `SHGeoid`

class instance, where the geoid map is stored internally as an `SHGrid`

class instance. Here, we compute the geoid on a grid that has a finer resolution than the potential coefficients by specifying the optional variable `lmax`

. The reason for doing so is to compare this map directly to a higher resolution map of the shape of the planet later:

In [9]:

```
mars_geoid = clm.geoid(u0, lmax=719)
fig4, ax4 = mars_geoid.plot(cmap='RdYlBu_r', show=False)
```

In this image, the geoid height largely reflects the rotational flattening of the planet. To calculate the geoid height with respect to a flattened ellipsoid, it is only necessary to specify the optional parameters `a`

and `f`

:

In [10]:

```
mars_geoid_ellipsoid = clm.geoid(u0, a=a, f=f, lmax=719)
fig5, ax5 = mars_geoid_ellipsoid.plot(vmin=-750, vmax=1200, cmap='RdYlBu_r', show=False)
```