# Preliminary orbits with line-of-sight correction for LEO satellites observed with radar

## TL;DR

This paper introduces a method for preliminary orbit determination of LEO satellites using radar data that accounts for Earth's oblateness, improving initial orbit estimates by incorporating the J2 perturbation into the dynamical model.

## Contribution

It extends previous Keplerian models by including Earth's oblateness (J2 effect) for more accurate orbit determination from radar observations.

## Key findings

- Enhanced initial orbit accuracy for low Earth orbit satellites.
- Improved convergence rates in orbit determination algorithms.
- Effective correction of line-of-sight measurements considering Earth's oblateness.

## Abstract

We propose a method to account for the Earth oblateness effect in preliminary orbit determination of satellites in low orbits with radar observations. This method is an improvement of the one described in (Gronchi et al 2015), which uses a pure Keplerian dynamical model. Since the effect of the Earth oblateness is strong at low altitudes, its inclusion in the model can sensibly improve the initial orbit, giving a better starting guess for differential corrections and increasing the chances to obtain their convergence. The input set consists of two tracks of radar observations, each one composed of at least 4 observations taken during the same pass of the satellite. A single observation gives the topocentric position of the satellite, where the range is very accurate, while the line of sight direction is poorly determined. From these data we can compute by a polynomial fit the values of the range and range rate at the mean epochs of the two tracks. In order to obtain a preliminary orbit we wish to compute the angular velocities, that is the rate of change of the line of sight. In the same spirit of (Gronchi et al 2015), we also wish to correct the values of the angular measurements, so that they fit the selected dynamical model if the same holds for the radial distance and velocity. The selected model is a perturbed Keplerian dynamics, where the only perturbation included is the secular effect of the $J_2$ term of the geopotential. The proposed algorithm models this problem with 8 equations in 8 unknowns.