TY - JOUR
T1 - Let It Go
T2 - Geophysically Driven Ejection of the Haumea Family Members
AU - Noviello, Jessica L.
AU - Desch, Steven J.
AU - Neveu, Marc
AU - Proudfoot, Benjamin C.N.
AU - Sonnett, Sarah
N1 - Funding Information:
We thank Emilie Dunham for a useful conversation that sparked many of the ideas presented here. We thank Sue Selkirk, who made the art of Haumea’s formation. We thank the anonymous reviewers for their thoughtful comments and feedback, as well as the journal managers and editor, Dr. Edgard Rivera-Valentín. Finally, we thank Darin Ragozzine for the discussions about Haumea’s formation and the light-curve analyses. This work was supported by grant 80NSSC19K0028 from NASA Solar System Workings (PI: Steve Desch). M.N. acknowledges support from NASA under the CRESST II Cooperative Agreement (award No. 80GSFC21M0002). J.L. N.’s research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. The views and conclusions contained in this document are those of the authors and should not be interpreted as representing the official policies, either expressed or implied, of the National Aeronautics and Space Administration (NASA) or the US Government. The US Government is authorized to reproduce and distribute reprints for government purposes notwithstanding any copyright notation herein.
Funding Information:
We thank Emilie Dunham for a useful conversation that sparked many of the ideas presented here. We thank Sue Selkirk, who made the art of Haumea’s formation. We thank the anonymous reviewers for their thoughtful comments and feedback, as well as the journal managers and editor, Dr. Edgard Rivera-Valentín. Finally, we thank Darin Ragozzine for the discussions about Haumea’s formation and the light-curve analyses. This work was supported by grant 80NSSC19K0028 from NASA Solar System Workings (PI: Steve Desch). M.N.
Funding Information:
acknowledges support from NASA under the CRESST II Cooperative Agreement (award No. 80GSFC21M0002). J.L. N.’s research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. The views and conclusions contained in this document are those of the authors and should not be interpreted as representing the official policies, either expressed or implied, of the National Aeronautics and Space Administration (NASA) or the US Government. The US Government is authorized to reproduce and distribute reprints for government purposes notwithstanding any copyright notation herein.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/9/1
Y1 - 2022/9/1
N2 - We present a new model for Haumea’s formation and evolution that relies on geophysical and geochemical data informed from observations of Haumea and meteorites to explain the characteristics of Haumea and its dynamical family. We hypothesize that after the impact of two partially differentiated Kuiper Belt objects, Haumea’s rocky core grew, decreasing its moment of inertia (MOI), spinning it up to the point that icy material was ejected from its surface. This ice, carrying about 3% of Haumea’s mass and 14% of its initial angular momentum, comprises the Haumean dynamical family and the ring system and moons observed today. Later, melted ice hydrated Haumea’s core and it grew, increasing Haumea’s MOI and spinning it down to the modern value. We use the geophysical code kyushu to demonstrate that solutions exist for a Haumea in hydrostatic equilibrium at each of these hypothesized stages. Geochemical modeling using the IcyDwarf code constrains the formation of Haumea’s core and the creation of the collision family to have occurred after roughly 150–160 Myr of solar system evolution (4.41 ± 0.01 Gyr ago). Hydration of the core was complete by about 0.20 Gyr, but a substantial subsurface ocean with half the mass of Earth’s oceans persisted until it froze at about 0.45 Gyr, making Haumea the solar system’s most distant potential relict ocean world.
AB - We present a new model for Haumea’s formation and evolution that relies on geophysical and geochemical data informed from observations of Haumea and meteorites to explain the characteristics of Haumea and its dynamical family. We hypothesize that after the impact of two partially differentiated Kuiper Belt objects, Haumea’s rocky core grew, decreasing its moment of inertia (MOI), spinning it up to the point that icy material was ejected from its surface. This ice, carrying about 3% of Haumea’s mass and 14% of its initial angular momentum, comprises the Haumean dynamical family and the ring system and moons observed today. Later, melted ice hydrated Haumea’s core and it grew, increasing Haumea’s MOI and spinning it down to the modern value. We use the geophysical code kyushu to demonstrate that solutions exist for a Haumea in hydrostatic equilibrium at each of these hypothesized stages. Geochemical modeling using the IcyDwarf code constrains the formation of Haumea’s core and the creation of the collision family to have occurred after roughly 150–160 Myr of solar system evolution (4.41 ± 0.01 Gyr ago). Hydration of the core was complete by about 0.20 Gyr, but a substantial subsurface ocean with half the mass of Earth’s oceans persisted until it froze at about 0.45 Gyr, making Haumea the solar system’s most distant potential relict ocean world.
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U2 - 10.3847/PSJ/ac8e03
DO - 10.3847/PSJ/ac8e03
M3 - Article
AN - SCOPUS:85142232335
SN - 2632-3338
VL - 3
JO - Planetary Science Journal
JF - Planetary Science Journal
IS - 9
M1 - 225
ER -