<p>Icy planetesimals are thought to contribute to the volatile inventory of terrestrial planets and serve as building blocks of icy bodies in the outer Solar System. Samples from the C-type asteroid Ryugu, collected by the Hayabusa-2 spacecraft, indicate a low-temperature history with aqueous alteration and organic materials. In contrast, iron meteorites with isotopic ratios similar to those of carbonaceous chondrites suggest exposure to higher temperatures. These findings imply that the thermal evolution of icy planetesimals is highly diverse. Since direct exploration provides only localized data, understanding this diversity requires comparing observational results with model calculations that incorporate key evolutionary processes. We develop a model, including radial growth, impact heating, water phase changes, aqueous alteration, and structural differentiation, to re-evaluate the thermal evolution of icy planetesimals during the first 100 Myr after the formation of calcium–aluminum-rich inclusions (CAIs). The model considers final radius (10–1000 km), timing of growth onset (1.0 or 2.0 Myr after CAI), growth duration (0.4 or 4.0 Myr), and growth mode (linear or runaway). Our results show that larger planetesimals generally reach higher temperatures, but growth timing and mode significantly affect thermal evolution. Early accretion leads to higher temperatures, with some bodies reaching the Fe–FeS eutectic (1250 K), while delayed or prolonged growth reduces heating. Our results show that the constituent materials of Ryugu, which kept below 40<InlineEquation ID="IEq1"> <EquationSource Format="TEX">$^{\circ }$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mo>∘</mo> </mmultiscripts> </math></EquationSource> </InlineEquation>C, likely formed near the surface of a hydrated mineral layer. This is possible even in planetesimals several hundred kilometers in size due to efficient heat transport via convection. If accretion begins 2.0 Myr after CAI and completes in 0.4 Myr, a wide region in such a body could yield Ryugu’s material. Evolution into a 250 km body with a 170–200 km hydrous core and overlying liquid water layer may resemble Saturnian icy moon Enceladus. For a later onset and longer duration of growth, even aqueous alteration could be prevented. In contrast, metal melting in the deep regions of rapidly formed icy planetesimals larger than 200 km could originate iron meteorites with isotopic signatures similar to those of carbonaceous chondrites.</p> Graphical Abstract <p></p>

Growth and thermal evolution of icy planetesimals

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2026年1月13日

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Jun Kimura,
Ryusei Sato,
Kentaro Terada,
Sho Sasaki

摘要

Icy planetesimals are thought to contribute to the volatile inventory of terrestrial planets and serve as building blocks of icy bodies in the outer Solar System. Samples from the C-type asteroid Ryugu, collected by the Hayabusa-2 spacecraft, indicate a low-temperature history with aqueous alteration and organic materials. In contrast, iron meteorites with isotopic ratios similar to those of carbonaceous chondrites suggest exposure to higher temperatures. These findings imply that the thermal evolution of icy planetesimals is highly diverse. Since direct exploration provides only localized data, understanding this diversity requires comparing observational results with model calculations that incorporate key evolutionary processes. We develop a model, including radial growth, impact heating, water phase changes, aqueous alteration, and structural differentiation, to re-evaluate the thermal evolution of icy planetesimals during the first 100 Myr after the formation of calcium–aluminum-rich inclusions (CAIs). The model considers final radius (10–1000 km), timing of growth onset (1.0 or 2.0 Myr after CAI), growth duration (0.4 or 4.0 Myr), and growth mode (linear or runaway). Our results show that larger planetesimals generally reach higher temperatures, but growth timing and mode significantly affect thermal evolution. Early accretion leads to higher temperatures, with some bodies reaching the Fe–FeS eutectic (1250 K), while delayed or prolonged growth reduces heating. Our results show that the constituent materials of Ryugu, which kept below 40 $^{\circ }$ $^{\circ}$ C, likely formed near the surface of a hydrated mineral layer. This is possible even in planetesimals several hundred kilometers in size due to efficient heat transport via convection. If accretion begins 2.0 Myr after CAI and completes in 0.4 Myr, a wide region in such a body could yield Ryugu’s material. Evolution into a 250 km body with a 170–200 km hydrous core and overlying liquid water layer may resemble Saturnian icy moon Enceladus. For a later onset and longer duration of growth, even aqueous alteration could be prevented. In contrast, metal melting in the deep regions of rapidly formed icy planetesimals larger than 200 km could originate iron meteorites with isotopic signatures similar to those of carbonaceous chondrites.

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