Making the Moon from a Fast-Spinning Earth: A Giant Impact Followed by Resonant Despinning

Forming the Moon from Earth It is thought that the Moon formed after a Mars-sized planet hit Earth about 4.5 billion years ago. Computer simulations of this event predict that the Moon was produced primarily from material from the impacting planet. However, the Moon has a similar composition to that of Earth, and the impacting planet would likely have had a different composition. Prior models assumed that the impact left the Earth-Moon system with the same angular momentum as it has today (see the Perspective by Halliday). Ćuk and Stewart (p. 1047, published online 17 October; see the cover) show that the angular momentum of the Earth-Moon system could have decreased by half after the Moon-forming impact, opening the door to new impact models. For example, simulations suggest that high-velocity impacts onto a fast-spinning early Earth can lead to a Moon formed primarily from Earth's mantle. Canup (p. 1052, published online 17 October) considered instead lower-velocity impacts by planets comparable in mass to the proto-Earth, which could generate a Moon and an Earth with similar compositions. Computer simulations show that a giant impact on early Earth could lead to a Moon with a composition similar to Earth’s. A common origin for the Moon and Earth is required by their identical isotopic composition. However, simulations of the current giant impact hypothesis for Moon formation find that most lunar material originated from the impactor, which should have had a different isotopic signature. Previous Moon-formation studies assumed that the angular momentum after the impact was similar to that of the present day; however, Earth-mass planets are expected to have higher spin rates at the end of accretion. Here, we show that typical last giant impacts onto a fast-spinning proto-Earth can produce a Moon-forming disk derived primarily from Earth’s mantle. Furthermore, we find that a faster-spinning early Earth-Moon system can lose angular momentum and reach the present state through an orbital resonance between the Sun and Moon.

[1]  On the Precession of a Viscous Spheroid, and on the Remote History of the Earth. [Abstract] , 2017 .

[2]  P. Goldreich,et al.  The history of the lunar orbit , 1966 .

[3]  William K. Hartmann,et al.  Satellite-Sized Planetesimals and Lunar Origin , 1975 .

[4]  David J. Stevenson,et al.  Origin of the Moon-The Collision Hypothesis , 1987 .

[5]  D. Stevenson,et al.  Gravitational instability in two-phase disks and the origin of the moon , 1988 .

[6]  A. .. Ringwood Flaws in the giant impact hypothesis of lunar origin , 1989 .

[7]  Hans-Peter Schertl,et al.  Geochim. cosmochim. acta , 1989 .

[8]  J. Wisdom,et al.  Symplectic maps for the N-body problem. , 1991 .

[9]  Jack Wisdom,et al.  Evolution of the Earth-Moon System , 1994 .

[10]  S. Ida,et al.  Lunar accretion from an impact-generated disk , 1997, Nature.

[11]  R. Canup,et al.  Evolution of a Terrestrial Multiple-Moon System , 1998 .

[12]  J. Wisdom,et al.  Resonances in the Early Evolution of the Earth-Moon System , 1998 .

[13]  G. Lugmair,et al.  Early solar system timescales according to 53Mn-53Cr systematics , 1998 .

[14]  C. Murray,et al.  Solar System Dynamics: Expansion of the Disturbing Function , 1999 .

[15]  J. Makino,et al.  Evolution of a Circumterrestrial Disk and Formation of a Single Moon , 1999 .

[16]  R. Ray,et al.  Lunar orbital evolution: A synthesis of recent results , 1999 .

[17]  Harold F. Levison,et al.  On the Character and Consequences of Large Impacts in the Late Stage of Terrestrial Planet Formation , 1999 .

[18]  R. Canup,et al.  Origin of the Moon's orbital inclination from resonant disk interactions , 2000, Nature.

[19]  L. Taylor,et al.  Oxygen Isotopes and the Moon-Forming Giant Impact , 2001, Science.

[20]  Erik Asphaug,et al.  Origin of the Moon in a giant impact near the end of the Earth's formation , 2001, Nature.

[21]  Y. Abe,et al.  The Evolution of an Impact-generated Partially Vaporized Circumplanetary Disk , 2004 .

[22]  R. Canup,et al.  Simulations of a late lunar-forming impact , 2004 .

[23]  宁北芳,et al.  疟原虫var基因转换速率变化导致抗原变异[英]/Paul H, Robert P, Christodoulou Z, et al//Proc Natl Acad Sci U S A , 2005 .

[24]  V. Springel The Cosmological simulation code GADGET-2 , 2005, astro-ph/0505010.

[25]  Matthew E. Pritchard,et al.  The Constitution and Structure of the Lunar Interior , 2006 .

[26]  Equilibration in the aftermath of the lunar-forming giant impact , 2007, 1012.5323.

[27]  M. Ćuk Excitation of Lunar Eccentricity by Planetary Resonances , 2007, Science.

[28]  E. Kokubo,et al.  Formation of Terrestrial Planets from Protoplanets. II. Statistics of Planetary Spin , 2007 .

[29]  R. Wieler,et al.  Late formation and prolonged differentiation of the Moon inferred from W isotopes in lunar metals , 2007, Nature.

[30]  R. Canup Lunar-forming collisions with pre-impact rotation , 2007 .

[31]  H. J. Melosh,et al.  A hydrocode equation of state for SiO2 , 2007 .

[32]  E. Kokubo Formation of Terrestrial Planets from Protoplanets , 2008 .

[33]  R. Rosenfeld Nature , 2009, Otolaryngology--head and neck surgery : official journal of American Academy of Otolaryngology-Head and Neck Surgery.

[34]  Lars Hernquist,et al.  COLLISIONAL STRIPPING AND DISRUPTION OF SUPER-EARTHS , 2009, 0907.0234.

[35]  Lars Hernquist,et al.  WATER/ICY SUPER-EARTHS: GIANT IMPACTS AND MAXIMUM WATER CONTENT , 2010, 1007.3212.

[36]  Eiichiro Kokubo,et al.  FORMATION OF TERRESTRIAL PLANETS FROM PROTOPLANETS UNDER A REALISTIC ACCRETION CONDITION , 2010, 1003.4384.

[37]  Robert A. Marcus,et al.  THE FORMATION OF THE COLLISIONAL FAMILY AROUND THE DWARF PLANET HAUMEA , 2010, 1003.5822.

[38]  Renee C. Weber,et al.  Seismic Detection of the Lunar Core , 2011, Science.

[39]  S. Jacobsen,et al.  Fast accretion of the Earth with a late Moon-forming giant impact , 2011, Proceedings of the National Academy of Sciences.

[40]  David L. Valentine,et al.  Seismic Detection of the Lunar Core , 2011 .

[41]  Sarah T. Stewart,et al.  COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS , 2011, 1106.6084.

[42]  Chemical fractionation in the silicate vapor atmosphere of the Earth , 2011 .

[43]  Andrew M. Davis,et al.  The proto-Earth as a significant source of lunar material , 2012 .

[44]  MOON FORMATION Earth's titanium twin , 2012 .

[45]  Gilbert W. Collins,et al.  Shock vaporization of silica and the thermodynamics of planetary impact events , 2012 .

[46]  R. Walker,et al.  182W Evidence for Long-Term Preservation of Early Mantle Differentiation Products , 2012, Science.

[47]  W. Ward ON THE VERTICAL STRUCTURE OF THE PROTOLUNAR DISK , 2012 .

[48]  S. Mukhopadhyay Early differentiation and volatile accretion recorded in deep-mantle neon and xenon , 2012, Nature.

[49]  Sarah T. Stewart,et al.  COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION , 2012 .

[50]  W. Benz,et al.  A hit-and-run giant impact scenario , 2012, 1207.5224.