The red dwarf Rothie AA-A h389 2, the gas giant 2 g, and the close binary pair 2
h and 2 i, computed from their recorded orbital elements. Dates are real (UTC); the in-universe year
is shown alongside.
Around the red dwarf. The two orbits are only about 168,000 km apart, so they almost overlap
at this scale. The square marks the close-up.Following the pair. Centred on the pair's barycentre with the red dwarf always below. Bodies
are to scale; the dashed line is 2 g's path over the next and previous three days.Edge on.The two orbital planes, all the way round. Height of each plane above the reference plane at
its orbital distance, plotted against direction from the red dwarf. Both planes pass through the red dwarf, so
they cross each other on one line. They are tilted ° relative to each other, so at
the pair's distance they are never more than about km apart. The vertical line marks
where 2 g and the pair's barycentre are now; the small dots are 2 h and 2 i, which swing around the barycentre
fast enough to make or break contact with 2 g even while the barycentre itself is moving apart from it.
2 g to 2 h, surface to surface–
2 g to 2 i, surface to surface–
2 g to the pair's barycentre–
Encounters, 2026 to 2048
Contact start
Contact end
Closest to 2 h
Closest to 2 i
Result
Each encounter is the moment 2 g overtakes the pair, roughly every 354.5 days. Distances are
surface to surface, so a negative figure means the bodies overlap. Select a row to jump to its closest moment.
These positions use Elite Dangerous's orbital-element convention (ascending node and argument of periapsis are
mirrored from the standard astronomical one), matching the Canonn signals page. Positions of bodies orbiting a
barycentre, like 2 h and 2 i, have not been verified against observations, so treat margins of a few
thousand kilometres as uncertain.
