TY - JOUR
T1 - Ceres
T2 - Astrobiological Target and Possible Ocean World
AU - Castillo-Rogez, Julie C.
AU - Neveu, Marc
AU - Scully, Jennifer E.C.
AU - House, Christopher H.
AU - Quick, Lynnae C.
AU - Bouquet, Alexis
AU - Miller, Kelly
AU - Bland, Michael
AU - De Sanctis, Maria Cristina
AU - Ermakov, Anton
AU - Hendrix, Amanda R.
AU - Prettyman, Thomas H.
AU - Raymond, Carol A.
AU - Russell, Christopher T.
AU - Sherwood, Brent E.
AU - Young, Edward
N1 - Funding Information:
J.C.C., J.E.C.S., M.B., A.E., T.H.P., C.A.R., C.T.R. acknowledge support from NASA’s Dawn Project. M.N. was supported by a NASA Postdoctoral Management Program Fellowship. C.H.H. was supported by NASA Exobiology grant NNX16AT71G and NSF Emerging Frontiers award 1724099. A.B. acknowledges support from CNES.
Publisher Copyright:
© Copyright 2020, Mary Ann Liebert, Inc., publishers 2020.
PY - 2020/2
Y1 - 2020/2
N2 - Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system's only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres' internal evolution.
AB - Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system's only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres' internal evolution.
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U2 - 10.1089/ast.2018.1999
DO - 10.1089/ast.2018.1999
M3 - Article
C2 - 31904989
AN - SCOPUS:85079021981
SN - 1531-1074
VL - 20
SP - 269
EP - 291
JO - Astrobiology
JF - Astrobiology
IS - 2
ER -