A fast bow shock location predictor-estimator from 2D and 3D analytical models: Application to Mars and the MAVEN mission

TL;DR

This paper introduces fast algorithms for predicting the bow shock location around planets using analytical models, validated on Mars data from the MAVEN mission, enabling quick and accurate shock crossing estimations.

Contribution

The paper develops new predictor-corrector algorithms for bow shock location estimation from spacecraft data, applicable across planetary environments, with demonstrated accuracy on Mars using MAVEN data.

Findings

Predicted shock position within 0.15 Rₚ of actual crossing

Refined estimate within 0.05 Rₚ using predictor-corrector method

Detected 14,929 bow shock crossings from 2014 to 2021

Abstract

We present fast algorithms to automatically estimate the statistical position of the bow shock from spacecraft data, using existing analytical two-dimensional (2D) and three-dimensional (3D) models of the shock surface. We derive expressions of the standoff distances in 2D and 3D and of the normal to the bow shock at any given point on it. Two simple bow shock detection algorithms are constructed, one solely based on a geometrical predictor from existing models, the other using this predicted position to further refine it with the help of magnetometer data, an instrument flown on many planetary missions. Both empirical techniques are applicable to any planetary environment with a defined shock structure. Applied to the Martian environment and the NASA/MAVEN mission, the predicted shock position is on average within 0.15 planetary radius $R_p$ of the bow shock crossing. Using the predictor-corrector algorithm, this estimate is further refined to within a few minutes of the true crossing $\approx$0.05 $R_p$). Between 2014 and 2021, we detect 14,929 clear bow shock crossings, predominantly quasi-perpendicular. Thanks to 2D conic and 3D quadratic fits, we investigate the variability of the shock surface with respect to Mars Years (MY), solar longitude (Ls) and solar EUV flux levels. Although asymmetry in $Y$ and $Z$ Mars Solar Orbital coordinates is on average small, we show that for MY32 and MY35, Ls = [135-225$^\circ$] and high solar flux, it can become particularly noticeable, and is superimposed to the usual North-South asymmetry due in part to the presence of crustal magnetic fields.