When a satellite reaches a Lagrangian point, it has a non-zero velocity $v_1$ because of the transfer orbit in which it had already been. What burn, say, $\Delta v$, one needs if the satellite is about to be kept at that Lagrangian point? Given velocity $v_2$ after the burn applied to the spacecraft, shall we have $v_2 = 0$, i.e., $\Delta v = -v_1$?

  • $\begingroup$ This will be a little hard to answer because satellites are usually put in orbits that move around Lagrange points (e.g. halo orbits), not exactly at them. Either way these tend to be unstable both because of orbital mechanics and because realistic orbits of the Earth, Moon, and other bodies are elliptical, not circular and so there are always perturbations. Also, satellites can try to approach these halo orbits along manifolds which can require very little delta-v to "slide into" halo orbits. It's a complicated topic. $\endgroup$
    – uhoh
    May 19 '19 at 20:44
  • $\begingroup$ This is a different question but you may find it interesting Rendezvouses in halo or lissajous orbits $\endgroup$
    – uhoh
    May 20 '19 at 0:14

What is the required burn to keep a satellite at a Lagrangian point?

tl;dr: typical station keeping delta-v for a halo orbit around Sun-Earth L1 or L2 points are of the order of 2 to 4 meters/sec per year based on a very old spacecraft (SOHO) and a future spacecraft (JWST).

I'll address the two closest and most used Lagrange points; L1 and L2. Generally spacecraft are put in halo or Lissajous orbits associated with (around) the points, not at the points themselves. This is done both for geometrical reasons (avoid the Sun in the line of sight for antenna-pointing or blockages) but there may be orbital mechanical reasons as well. See the extensive answers to Are large halo orbits around L₁'s and L₂'s preferred over small orbits for reasons other than geometry?

I'll add a quick note, Lagrange points and halo (and other) orbits are mathematical manifestations of mathematics. They exist in a certain theoretical situation called the Circular Restricted Three Body Problem or CR3BP (or CRTBP). These concepts work approximately in the real world where orbits are not circular and there are more than three bodies.

Whether you are at L1 or L2, or in a halo orbit around them, you are really orbiting around the larger body. If you are at or near the Sun - Earth L1 (e.g. DSCOVR, SOHO) you are really in an orbit around the Sun which is in resonance with the Earth. It would normally move around the Sun a little faster than Earth, but Earth pulls it back just enough to keep it orbiting with a period of one year.

There is a subclass of halo orbits around L1 and L2 in the CR3BP model that are actually stable, though the rest aren't. However in the real world due to there being other gravitational bodies around and the orbits not being circular, none of these are really stable.

According to this answer to ** the James Webb Space Telescope (JWST) only needs a station-keeping delta-v budget of 2 to 4 meters/sec per year to stay in its halo orbit around the Sun-Earth L2 point. It accomplishes this though careful planning and construction. JWST sits just in front of the most stable halo orbit so it would ten to wander toward the Earth, but this is balanced by solar photon pressure on its giant solar thermal shield, which tends to hold it there (roughly speaking). It will also execute very tiny delta-v maneuvers ever three weeks so that the errors are tiny and never allowed to grow.

I talk a lot about SOHO (Sun-Earth L1) station keeping in Is this what station keeping maneuvers look like, or just glitches in data? (SOHO via Horizons) and in the exciting report (if you like orbital mechanics) Roberts 2002 The SOHO Mission L1 Halo Orbit Recovery From the Attitude Control Anomalies of 1998 in Table 2 and the paragraph that follows, it says that SOHO originally needed about 2.4 meters/sec per year for station-keeping.

When a satellite reaches a Lagrangian point, it has a non-zero velocity 𝑣1 because of the transfer orbit in which it had already been.

Getting to halo orbits around L1 and L2 does not always require a classical "transfer orbit". You can sneak in with very little delta-v along what is called a "stable manifold" as SOHO did for example. It's not perfectly zero delta-v, but it is very low.

It is a lot like the opposite of what would happen if you started just Earthward of the halo orbit, you would drift out along the unstable manifold. Drifting in is like drifting out but backwards in time.

This is plotted data from Horizons from Is this what station keeping maneuvers look like, or just glitches in data? (SOHO via Horizons) using a script like this: https://pastebin.com/7XULFDea written when I was just starting to learn Python. Still images combined into a GIF using ImageJ. Data from https://ssd.jpl.nasa.gov/horizons small black dots are 1 day intervals, red dot is Sun-Earth L1 and blue blob represents the various places Earth is relative to L1.

SOHO from JPL's Horizons

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    $\begingroup$ That's a very nice visualisation - do you plot it and record the screen as you change the view? $\endgroup$
    – Rory Alsop
    May 20 '19 at 7:54
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    $\begingroup$ Thank you - I hadn't visited the links, I assumed they were just the source of the data. $\endgroup$
    – Rory Alsop
    May 20 '19 at 8:58
  • $\begingroup$ @RoryAlsop yikes that was three years ago, feels like another lifetime. I've added the information for the plot here instead. $\endgroup$
    – uhoh
    May 20 '19 at 12:20

For those Lagrangian points which are unstable, L1, L2 and L3, there is no equilibrium, and any movement off the point will accelerate further away, towards the Sun or Earth. For them, you would need to counteract v1 (and any gravitational forces undergone along the way) in order to reach a rest velocity with respect to the Lagrangian point plus you would have to use thrusters to remain there.

For stable Lagrangian points, L4 and L5, you would need to simply meet the required orbit parameters. There will still be a burn to match the orbit.

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    $\begingroup$ L1, L2 and L3 are equilibria (in the rotating reference frame). They are just unstable in the same direction as the vector connecting the star and planet. So perturbations in the other two directions are not unstable (though the surface that is spanned by this is curved). This is also what enables halo orbits. But in general disturbances like variations in solar pressure or the gravitational pull of other planets do excite this unstable direction so one does indeed need to perform station keeping burns. $\endgroup$
    – fibonatic
    May 20 '19 at 20:20

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