《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
: Y& |1 L0 u; h1 S/ F0 I" Xa lower density of craters smaller than about 100 km in diameter than on the & L* ^, [5 B7 E
Moon, a deficit that has been attributed to resurfacing by formation of ancient ! f3 Q" n' `( j+ S( f/ B9 _
intercrater plains. Simone Marchi et al. used a crater areal density map 9 U3 X: Q/ ^, F6 A
based on data from the MESSENGER spacecraft (the colour-coded foreground on / T2 d" E  b- a. Q- q: F1 E* g7 W0 d
cover, with a global surface mosaic in the background) to locate the oldest # {" e" n2 f* N8 P* h
surfaces on Mercury and interpret the crater populations in the framework of a , j5 `  @; l4 v) s! \
recent lunar crater chronology. They conclude that the oldest surfaces were 9 g7 W- z6 n5 m) M
emplaced just after the start of the Late Heavy Bombardment 4.0 to 4.1 billion
8 G7 d* C# O, t( E- S/ |( l1 X7 m; Pyears ago. The large impact basins, not previously dated, yield a similar # q  G/ k0 _5 L
surface age. This agreement implies that resurfacing was global and due to
3 U% P: M8 T! Y6 _% @volcanism, perhaps aided by heavy bombardment as previously suggested. Cover: 3 ]# a# D  F0 ^9 p4 z0 p% E1 }! B
Simone Marchi/MESSENGER data: NASA/JHUAPL/Carnegie Institution of Washington, p- ]1 U8 N, b  T9 _  u. x. N

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