Differences between revisions 3 and 5 (spanning 2 versions)
 ⇤ ← Revision 3 as of 2013-02-27 06:39:40 → Size: 1035 Editor: KeithLofstrom Comment: ← Revision 5 as of 2013-02-27 06:52:17 → ⇥ Size: 2129 Editor: KeithLofstrom Comment: Deletions are marked like this. Additions are marked like this. Line 1: Line 1: #format jsmath Line 7: Line 8: {{attachment:incline1.png:width=512}} Line 8: Line 10: If the displacement of the unconstrained orbit differs from the equatorial orbit by $d = D \sin{ \omega t }$, then the acceleration is $a = - \omega^2 D \sin{ \omega t }$. Since $\omega^2 = \mu / R^3$ for a circular orbit without the $J_2$ perturbation, the peak acceleration is \mu D / R^3 . For μ = 398600.44 km^3^/s^2^, the acceleration at maximum displacement is given for various altitudes in the table below, as well as the accumulated $\Delta V$ over a 10 year mission:|| Altitude || Radius || Acceleration || 10 year $\Delta V$ |||| km || km || μm/s^2^ || m/s |||| 200 || 6578 || || |||| 600 || 6978 || || |||| 1000 || 7378 || || |||| 2000 || 8378 || || |||| 6411 || 12789 || || || m288 |||| 35786 || 42164 || || || GEO ||

# Displacement and Acceleration

Arrays of satellites cannot maintain a constant displacement above or below the orbital plane without a constant (and significant) acceleration keeping them there. The ΔV needed over the lifetime of a satellite is beyond the range of high Isp engines. Further, it is unnecessary; by using constellations that evolve and rotate in three dimensions along the orbit, the same results (high gain main lobe, suppressed sidelobes) can be achieved. It is important to work with orbital mechanics, not fight nature and physics.

Imagine an attempt to permanently "hover" on the "north" side of a circular equatorial orbit. All Kepler earth orbits are mapped onto planes which intersect the center of the earth, and our hovering object is actually on a different, slightly inclined orbit. If the object is free to follow the orbital mechanics without an external force, it will follow a slightly different inclination circular orbit that intersects the original orbital plane.

If the displacement of the unconstrained orbit differs from the equatorial orbit by d = D \sin{ \omega t } , then the acceleration is a = - \omega^2 D \sin{ \omega t } . Since \omega^2 = \mu / R^3 for a circular orbit without the J_2 perturbation, the peak acceleration is \mu D / R3 . For &mu; = 398600.44 km3/s2^, the acceleration at maximum displacement is given for various altitudes in the table below, as well as the accumulated \Delta V over a 10 year mission:

 Altitude Radius Acceleration 10 year \Delta V km km μm/s2 m/s 200 6578 600 6978 1000 7378 2000 8378 6411 12789 m288 35786 42164 GEO

DisplacementAcceleration (last edited 2021-06-19 03:55:33 by KeithLofstrom)