Maintaining the proper current density profile, for example, can help to maintain stability to tearing modes.

To visualise instantaneous density profiles, a short duration flash (rather than continuous illumination) may be used.

If there is a range of masses, each component will have a different density profile.

If this is the case, the observed stars would be expected to attain the shallower density profile, .

I still haven't been able to write a function that describes the observed density profiles.

What is the morphology of the density profiles in this difficult to probe region?

In order to accommodate a flat rotation curve, a density profile for galactic environs must be different than one that is centrally concentrated.

The deviations can then be analyzed to obtain the density profile of the interface normal to the surface.

The pulsation frequencies give the information about the density profile of the region where the waves originate and travel.

For example, gravity measurements are used to obtain a model of the density profile under the surface.