《自然》[Nature]13年7月4日出版pdf全文

nero1981

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The most heavily cratered terrains on Mercury exhibit $ \4 T, B" M) N9 P  _
a lower density of craters smaller than about 100 km in diameter than on the 7 s! q6 k. v& u* _- ^' ?
Moon, a deficit that has been attributed to resurfacing by formation of ancient
  m3 Q0 u+ Z) \0 ]; A, z& d! |intercrater plains. Simone Marchi et al. used a crater areal density map 2 Z1 C+ M& ~, f$ ^; D' Q
based on data from the MESSENGER spacecraft (the colour-coded foreground on ' e8 _8 q- |& t* y7 \4 q9 o
cover, with a global surface mosaic in the background) to locate the oldest
, q) c( Z) \9 L( [8 k$ Xsurfaces on Mercury and interpret the crater populations in the framework of a
' Z2 c/ b" ]+ s8 g) grecent lunar crater chronology. They conclude that the oldest surfaces were
/ H8 g5 o; X. c' n5 ^emplaced just after the start of the Late Heavy Bombardment 4.0 to 4.1 billion , W9 e6 X3 G" m( ?
years ago. The large impact basins, not previously dated, yield a similar ( C4 F% W4 U4 x: ]# M' T
surface age. This agreement implies that resurfacing was global and due to
; R/ R. P  i1 U2 H" Jvolcanism, perhaps aided by heavy bombardment as previously suggested. Cover:
6 b. g5 h, S: t# k& D- d2 W" ZSimone Marchi/MESSENGER data: NASA/JHUAPL/Carnegie Institution of Washington1 f7 S' f7 U1 V3 Z1 J& O' G

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