The trans-Neptunian dwarf planet Eris is tidally locked to its small moon Dysnomia. Recently obtained bounds on the mass of Dysnomia demonstrate that Eris must be unexpectedly dissipative (‘squishy’) for it to have despun over the age of the Solar System. New research shows that Eris must have differentiated into an ice shell and rocky core to explain the dissipation.
Eris was discovered in January 2005 by Caltech astronomer Michael Brown and colleagues at Palomar Observatory.
The dwarf planet is roughly 2,300 km (1,445 miles) in diameter, has a mass of 0.28% that of Earth and 27% greater than that of Pluto.
Eris has an orbital period of 559 years. Its maximum possible distance from the Sun is 97.5 AU (astronomical units), and its closest is 38 AU.
Unlike its cousin Pluto, which was explored by NASA’s New Horizons spacecraft and revealed a dynamic and variegated world, only these basic characteristics of Eris are available.
In particular, its internal structure, for instance, whether it consists of a homogeneous rock-ice mixture or not, is unknown.
“The first important clue is that Eris and its moon, Dysnomia, always face the same way toward each other,” said University of California, Santa Cruz Professor Francis Nimmo.
“That happens because the big planet gets spun down by the tides that the little moon raises on it. The bigger the moon is, the faster the planet spins down.”
Researchers can use the spin and orbital characteristics of planets and their moons to infer properties of their internal structures. But until recently, they did not have an estimate for the size of Dysnomia.
The new data from the Atacama Large Millimeter/Submillimeter Array (ALMA) changed that by revealing that Eris’ moon must be below a certain mass (mass ratio 0.0084 at 1-σ and 0.015 at 3-σ). This upper limit on mass provided the second crucial piece of information.
“And so as soon as you know that, then you can actually start to do real calculations,”…
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