What is it about?
Effects of radiation pressure and oblateness of primaries on various parameters of halo orbits are studied. Due to increase in oblateness of the first primary, halo orbits around L1 and L2 enlarge, move towards the second primary and their period decreases. Due to increase in oblateness of the second primary, halo orbits around L1 shrink, move towards the first primary and their period decreases while halo orbits around L2 enlarge, move away from the second primary and their period decreases. Numerical solution for halo orbits around L1 and L2 in the Sun–Earth system is obtained by using the differential correction method for different values of radiation pressure and oblateness.
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Why is it important?
It has been observed that as we consider higher order solution using the Lindstedt–Poincaré method, we get more precise halo orbits. So, considering the fifth order solution as an initial guess for obtaining halo orbits using the differential correction or other numerical method provides better approximation than the third or fourth order solution.
Read the Original
This page is a summary of: Fifth order solution of halo orbits via Lindstedt–Poincaré technique and differential correction method, New Astronomy, August 2021, Elsevier, DOI: 10.1016/j.newast.2021.101585.
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