There is significant interest in monitoring the instantaneous magnetic configurations and dynamic states of the magnetotail and understanding what controls them. A unique and attractive opportunity is provided by remote sensing of the radial profile of the equatorial magnetic field curvature based on low‐latitude energetic particle measurements of isotropy boundaries (IBs), providing that you can determine the origin of isotropic precipitation. To validate the magnetic field line curvature scattering (FLCS) as the main mechanism of the isotropy boundary formation, we compare coarse energy versus latitude IB profiles (in 3 + 3 energy channels) measured during a few dozen passes of POES and ELFIN spacecraft with the theoretical predictions of the adapted (AM03) magnetospheric model. Two studied intervals in August 2022 include substorm events of various intensities for which good spacecraft coverage in the near magnetotail helps reconstruct the adaptive model in the areas where the IBs are formed. We find a general agreement between the predicted and observed coarse IB profiles' shape and latitude, validating the FLCS hypothesis. Deviations are also observed, and we discuss the factors that can influence identification of the true FLCS profiles in observations and predictions, including limitations of adaptive modeling, non‐monotonic radial structure of the tail magnetic field, and interference of FLCS with other precipitation mechanisms related to wave‐particle interactions. Most can be avoided by improving the sensitivity, energy coverage, and resolution in future instruments. The global radial structure of the equatorial magnetotail magnetic field can regulate the character and strength of convection in the tail plasma sheet, which is driven by the dayside merging process. It is impossible to monitor it in situ with a few magnetospheric spacecraft; however, snapshots of this magnetic terrain can be reconstructed by observing boundaries of isotropic precipitations (Isotropy Boundaries, IBs) at low‐altitude, polar‐orbiting spacecraft when they cross the nightside auroral zone. Caution must be exercised to distinguish magnetic curvature‐controlled precipitation (FLCS) from wave‐particle interaction types of precipitation (WPI). To validate the mechanism, we analyze two intervals in August 2022 with good spacecraft coverage in the near magnetotail. We constrain the magnetic field in the area where the IBs originate from using the adaptive (AM03) magnetospheric model. We compare FLCS‐based model‐predicted IBs at 6 energies (coarse IB profile) with the profiles observed by POES and ELFIN polar spacecraft for a few dozen of their near‐midnight crossings of the auroral zone. The observed coarse IB profiles agree with adaptive model predictions concerning their shape and latitude, except in situations when no magnetic measurements are available in the region of IB formation. Although this validates the preponderance of the FLCS mechanism to explain the observations, various factors are also discussed that could lead to some systematic deviations of compared IB latitudes. Adapted magnetospheric model is used to predict energy versus latitude Isotropy Boundary profiles based on current sheet scattering mechanism Observed and predicted coarse IB profiles show general agreement in shape and latitude, supporting their FLCS origin Inconsistencies between observed and predicted profiles reflect the complexity of tail configurations and interference from wave‐particle scattering