TY - JOUR
T1 - Thermal evolution of icy planetesimals in the solar nebula
AU - Wakita, Shigeru
AU - Sekiya, Minoru
N1 - Funding Information:
Acknowledgments. We thank Drs. Tomoki Nakamura, Tomoaki Kubo, Ryuji Okazaki, Hiizu Nakanishi and Saburo Miyahara for their comments and discussions. We also thank Dr. Motoo Ito and an anonymous reviewer for their helpful reviews. Numerical simulations were in part performed on the general-purpose PC farm at the Center for Computational Astrophysics, CfCA, of the National Astronomical Observatory of Japan. This work is supported by Grant-in-Aid for JSPS Fellows (21-2143) from the Ministry of Education, Culture, Sports, Science and Technology.
PY - 2011
Y1 - 2011
N2 - The thermal histories and time evolutions of icy planetesimals are numerically solved with various parameters (the time of formation that corresponds to the ratio of 26Al/27Al, the size of the planetesimals and their initial temperature). We consider the formation of a rocky core due to the settling of rocks after the melting of ice. We also take into account two chemical reactions, aqueous alteration and a dehydration reaction, between rocks and water. Results of numerical simulations show that a key factor is the initial ratio of 26Al/27Al. Our results indicate that icy planetesimals, formed at 2.4 Myr after CAI formation, may not reach the melting temperature of ice, regardless of their sizes and initial temperature.
AB - The thermal histories and time evolutions of icy planetesimals are numerically solved with various parameters (the time of formation that corresponds to the ratio of 26Al/27Al, the size of the planetesimals and their initial temperature). We consider the formation of a rocky core due to the settling of rocks after the melting of ice. We also take into account two chemical reactions, aqueous alteration and a dehydration reaction, between rocks and water. Results of numerical simulations show that a key factor is the initial ratio of 26Al/27Al. Our results indicate that icy planetesimals, formed at 2.4 Myr after CAI formation, may not reach the melting temperature of ice, regardless of their sizes and initial temperature.
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U2 - 10.5047/eps.2011.08.012
DO - 10.5047/eps.2011.08.012
M3 - Article
AN - SCOPUS:84861395604
SN - 1343-8832
VL - 63
SP - 1193
EP - 1206
JO - earth, planets and space
JF - earth, planets and space
IS - 12
ER -