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Transcript of Mancinelli Et Al 2014
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8/11/2019 Mancinelli Et Al 2014
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Pure and Applied Geophysics
pageoph
ISSN 0033-4553
Pure Appl. Geophys.
DOI 10.1007/s00024-014-0906-8
Fractal Dimension of GeologicallyConstrained Crater Populations of Mercury
Paolo Mancinelli, Cristina Pauselli,
Diego Perugini, Andrea Lupattelli &
Costanzo Federico
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Fractal Dimension of Geologically Constrained Crater Populations of Mercury
PAOLO MANCINELLI,1 CRISTINAPAUSELLI,1 DIEGO PERUGINI,1 ANDREA LUPATTELLI,1 and COSTANZOFEDERICO1
AbstractData gathered during the Mariner10 and MES-
SENGER missions are collated in this paper to classify craters into
four geo-chronological units constrained to the geological map
produced after MESSENGERs flybys. From the global catalogue,
we classify craters, constraining them to the geological information
derived from the map. We produce a size frequency distribution
(SFD) finding that all crater classes show fractal behaviour: with
the number of craters inversely proportional to their diameter, the
exponent of the SFD (i.e., the fractal dimension of each class)
shows a variation among classes. We discuss this observation aspossibly being caused by endogenic and/or exogenic phenomena.
Finally, we produce an interpretative scenario where, assuming a
constant flux of impactors, the slope variation could be represen-
tative of rheological changes in the target materials.
Key words: Mercurys geology, impact processes, primary
and secondary crust.
1. Introduction
Over the last few years, new data from the
MESSENGER spacecraft (NASA mission) have shed
new light on the geological history of Mercury.
Endogenic phenomena such as contractional tectonics
and volcanism extensively affected the surface of the
planet, defining the morphologies observed by Mar-
iner10 and MESSENGER. Exogenic processes such
as asteroid impact-induced cratering also altered
Mercurys surface, and may have contributed to
volcanic activity on the planet, at least in the larger
basins.Data from both Mars and the Moon indicate that
the inner solar system is characterised by two popu-
lations of impactors: one resulting from the Late
Heavy Bombardment (LHB) (GOMES et al. 2005;
HARTMANN et al. 1981; NEUKUM et al. 2001; MARCHI
et al. 2009; MINTON and MALHOTRA 2010) which
ended about 3.8 Ga ago and was caused by migration
of the giant planets (MORBIDELLI et al. 2001; MOR-
BIDELLIet al. 2002; GOMES et al. 2005; MARCHIet al.
2012), and another due to Near Earth Asteroids
(NEA) (BOTTKE et al. 2002; MORBIDELLI et al. 2002;STROM et al. 2005; STROM et al. 2008; STROM et al.
2011). Considering that the analysis from STROM
et al.(2005) obtained the same results for Mercurys
highlands and Caloris plains and because of its
location in the inner solar system, we expected
Mercurys crater population to show the same
behaviour on a global-scale analysis. The decay rate
from LHB is still considered controversial, but most
authors believe that the cratering projectile flux has
been more or less constant for the last 3.5 Ga, at least
for those impactors with diameters of less than 10 km
(HARTMANN et al. 1981; NEUKUM et al. 2001; BOTTKE
et al. 2002; MARCHI et al. 2009; MINTON and MAL-
HOTRA 2010). The effects of the LHB on a planetary
body can also be constructive. In fact, LHB impactors
have been hypothesized as providers of volatiles that
could have contributed to the enrichment of the ter-
restrial planets (TRIGO-RODRIGUEZand MARTINTORRES
2012; TRIGO-RODRIGUEZ 2013).
The crater represents the sum of the effects of
three impact phases: coupling, excavation and mod-ification (e.g., MELOSH 1989; XIAO et al. 2014). The
first two phases represents the transmission and
propagation of the energy of the projectile to the
target body, first producing melt and vaporization,
then immediately after, the target material is
deformed and ejected. Deformation is proportional to
the energy of the projectile, is dependent on the target
and projectile materials, and decreases with increas-
ing distance from the impact. The result of these two
1Dipartimento di Fisica e Geologia, Universitadegli Studi di
Perugia, Via A. Pascoli, 06123 Perugia, Italy. E-mail: pamancinel-
[email protected]; [email protected];[email protected];
[email protected]; [email protected]
Pure Appl. Geophys.
2014 Springer Basel
DOI 10.1007/s00024-014-0906-8 Pure and Applied Geophysics
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phases is the transient crater. The last phase may last
longer than the previous two, and involves the col-
lapse of both the ejected material and the unstable
portions of the crater rim, which will partially fill the
crater basin. At the end of this phase, the final
diameter of the crater is achieved.
Products and morphologies resulting from an
impact on the surface of a planet can be used as a
proxy to infer the structure and rheology of the pla-
nets upper crust (MASSIRONIet al.2009; MARCHIet al.
2011), and therefore to verify whether outcropping
material is made of primary crust or of stratified
igneous bodies and volcanic deposits.
Since the first data produced by the Mariner10,
geological mapping of planet Mercury was one of the
main goals to achieve in order to understand Mer-
curys surface evolution. Resolution of mappingincreased with the quantity and resolution of data
gathered by MESSENGER spacecraft (DENEVI et al.
2009). Crater statistics followed and constrained
geological mapping, and were produced by many
authors for different purposes (e.g. STROMand NEUKUM
1988; STROMet al.2005; MARCHIet al.2011). Despite
crater statistics certainly being a valid method to
gather information about a planetary surface, and its
temporal evolution both in a relative and an absolute
sense, global scale statistics were never produced for
Mercury. The aim of this work is to present a first
analysis of crater statistics on a global scale for the
planet Mercury, and to test fractal behaviour of geo-
logically constrained crater populations. In particular,
we will present a size frequency distribution (SFD)
constrained to geological observations, and discuss
possible interpretations of the data, considering the
variables that affect impact cratering.
2. Material, Methods and Preliminary Results
The basemap of this work (Fig.1A) covers the
whole planet and contains both new geological
information acquired during MESSENGERs third
flyby and orbital insertion, and more recently pub-
lished data on outcropping geology (DENEVI et al.
2009). To achieve the maximum possible coverage,
we started from that map and enlarged it in order to
cover regions observed after MESSENGERs third
flyby and orbital insertion. To map these areas, we
used the same parameters and unit classification as
defined by DENEVI et al. 2009. The term geological
units will be used in the text to indicate outcropping
formation grouped on the base of the reflectance that
can be representative of a true mineralogical, and thus
geological, change between units. The map was
constructed in a GIS environment, by establishing a
geological formation and a relative age value (geo-
chronological information) for each deposit, as
shown by DENEVI et al.2009, who classified materials
on the basis of reflectance and cratering, and attrib-
uted a relative timing of deposition to each unit.
The older unit, called Intermediate Terrains (IT),
is representative of heavily cratered old regions.
Above these terrains, Low Reflectance Material
(LRM) encompasses low reflectance deposits, com-prising of craters and basin ejecta. Within these LRM
deposits there are a few darker outcrops, containing
crater ejecta and which are defined as centres of LRM
(LRM_C). The younger units, which are represented
by smooth plains ranging from low to high reflec-
tance, are subdivided into two deposits: 1) High
Reflectance Plains (HRP) and Intermediate Plains
(IP), with intermediate to high reflectance; and 2)
Low Reflectance Blue Plains (LBP), which include
later volcanic, low reflectance smooth plains. Within
the HRP ? IP unit, according to the new data from
Flyby 3 and orbit insertion (HEAD et al. 2011), some
fresh deposits are also introduced. These have been
mapped around and inside the Rachmaninoff Basin
(Fig.1A). This new subunit (hereafter referred to as
Late Volcanic Deposits; LVD) displays typical
reflectance and cratering with respect to all the other
units and is made up of smooth deposits. LVD fill
topographic depressions, and are considered to be the
products of volcanic activity that occurred in the
Rachmaninoff region (PROCKTER et al. 2010), whereLVD also registered in an anomalous secondary
cratering (CHAPMAN et al. 2012). Other than in the
South Rachmaninoff basin, other LVD have been
mapped in the Firdousi Plains region. The recently
observed volcanic floods that occurred in the northern
polar region (HEAD et al. 2011) have also been
mapped as LVD, in view of their morphological
characteristics and of their spectral properties similar
to the Firdousi Plains (Fig. 1A, B). However, on a
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global scale, we consider LVD as part of the
HRP ? IP plains, according to previous work that
classified the northern plains as similar to the HRP
unit (HEADet al. 2011).
Although the validity of this kind of geological
mapping may be up for debate, particularly when
terrains are classified primarily according to
reflectance data, this classification (i.e., units HRP,
IP, LBP, LRM, LRM_C and IT) was made by DENEVI
et al. 2009 according to colour and spectroscopic
variations observed and described by previous works
using images from the Mercury Dual Imaging System
(MDIS) (ROBINSON et al. 2008) and data from the
Mercury Atmospheric and Surface Composition
Spectrometer (MASCS) (MCCLINTOCK et al. 2008),
respectively. This approach is further supported when
the geologic map is compared to the mosaic of
MASCS observations (Fig.1A, B).
We assumed that terrains encompassed in the
same unit were deposited in a brief time period (i.e.,
each unit is representative of a time step of the glo-
bal-scale geological evolution of Mercury). This
assumption is supported by the work of MARCHI et al.
(2013), who found that the planet-scale resurfacing ofMercury was produced between 4.1 and 3.55 Ga ago
and was related to LHB, which possibly triggered
global-scale volcanic activity. This indicates that all
global-scale units as mapped in Fig.1A were rap-
idly deposited within this time interval, and thus that
all deposits encompassed in the same unit were pro-
duced in a short time interval.
Figure 2Overlay of geological map, planetary mosaic and crater catalogue from the region west of Rembrandt basin. T4 older fourth-order craters,T3
third-order craters, T2 second-order craters, T1 younger first-order craters
Figure 1A Geological map, modified after DENEVI et al. 2009, and picture
mosaic after Mariner10 and MESSENGER flybys. IT: Intermediate
Terrains, relative Age: IV. LRM: Low Reflectance Material,
relative Age: III. LRM_C: Low Reflectance Material Centre,
relative Age: III. HRP ? IP: Low Reflectance Plains and Interme-
diate Plains, relative Age: II. LBP: Low reflectance Blue Plains,
relative Age: I. LVD: Late Volcanic Deposits, relative age: I [1-
0.7 Ga for Rachmaninoff infill (MASSIRONI et al. 2009)]. White
arrow: Rachmaninoff Basin. B Ultraviolet to near-infrared spectral
variations mapped by Mercury Atmospheric and Surface Compo-
sition Spectrometer (MASCS) during the MESSENGER orbital
phase modified from the file PIA14866 (link to the web page of this
image is provided in the references). C Craters used for SFD
analysis in Figure4 and geo-chronological characterization of each
crater. Colors show diameter classes from 40 to 120 km [crater data
from FASSETT et al. (2011)]. Background image resolution used
during mapping: 0.7 km/pixel. Equidistant cylindrical projection
used on images and sinusoidal equal-area projection for area
calculations. GIS software: QuantumGIS 1.7.1
b
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Stratigraphic data is more complex to gather from
reflectance or spectral observations. Data produced
by instruments on board the Mariner10 and MES-
SENGER missions did not allow for the easy building
of a constrained model of the material in the imme-
diate subsurface, also due to uncertainties over thelocal-scale mineralogical characterisation of out-
cropping terrains still needing to be clarified. This
lack of stratigraphic constraints also has effects on
formulating a definition of correct ages for outcrop-
ping material. However, the morphological features
observed during GIS mapping, constrained by the
degree of cratering of each deposit, do allow defini-
tion of a depositional order in time.
The above considerations allow us to assign the
following relative ages, from the oldest to the youn-
gest formations: Age IV for the IT, Age III for LRM
and LRM_C, Age II for HRP, IP and LVD, and Age I
for LBP deposits (Fig.1). These ages are purely
indicative of the depositional steps during which themapped units were deposited from the older IT to the
younger LBP. This order is established on the basis of
morphological features and cratering. It is impossible
to univocally define the absolute timing of the
appearance of these units. However, it is clear that,
from the beginning of the deposition of the IT unit to
the end of the deposition of the LBP unit, a remark-
able phase of the geological resurfacing of Mercury is
Figure 3SFD analyses for crater classes defined with geo-chronological constraints (see text for details). Plot is built considering cumulative number
(N) of craters with diameterDClarger or equal than comparative diameter dCfor each class, normalized by area covered by geological unit on
the whole planet (A). T1, T2, T3, T4 classes defined in text and in Fig. 2. Table:n/Aratio between number of craters per crater class (n) and
A(units in 10E6 km2
).S: exponent of the cumulative SFD for each crater class (i.e., fractal dimension of each class). Classes encompass all
observed craters with diameters between 40 and 412 km. Errors reported for the calculation ofSare cumulative of errors resulting from linear
fit and from data points
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shown (i.e., a time interval). Another limitation
coming from the lack of constrained stratigraphic
information is that we cannot locate or estimate units
overlaps, either in global or in local-scale analysis.
Analysis of SFD was carried out starting from
the recently published crater catalogue (FASSETT
et al. 2011). From this catalogue, our analyses do
not consider craters with diameter (DC) smaller
than 40 km, or the nine larger basins (i.e., craters
with diameter larger than 412 km). The lower
bound allows us to exclude the effects of secondary
cratering that may produce uncertainties in the
results; the upper bound is introduced to reduce
redundancy of the major craters on the cumulative
plot.
The geo-chronological data derived from the
basemap is therefore combined with the position of
the centre of each crater. This process organises the
entire crater catalogue in four classes using the geo-
chronological attributes of the basemap (i.e., out-
cropping geology and relative ages). The GIS
software automatically carries out this classification,
but it is followed by a careful evaluation of each
crater, to best characterise its relative age by con-
sidering its morphological features, the outcropping
unit at its centre, and the morphological relations
between this deposit and the surroundings. Based on
these criteria, we identify four geo-chronological
classes of craters, from the youngest to the oldest: T1,
T2, T3 and T4 (Fig. 2).
Figure 4SFD analyses for crater classes defined with geo-chronological constraints and diameters between 40 and 120 km (see text for details). Plot is
built considering cumulative number (N) of craters with diameter DClarger or equal than comparative diameter dCfor each class, normalized
by area covered by geological unit on the whole planet (A). T1, T2, T3, T4 classes defined in text and in Figure 2. Table:n/Aratio between
number of craters per crater class (n) and A (units in 10E6 km2). S: exponent of the cumulative SFD for each crater class (i.e., fractal
dimension of each class). Errors reported for the calculation ofSare cumulative of errors resulting from linear fit and from data points
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Some assumptions were made in this process of
crater classification: (1) if a crater is surrounded by a
unit that is younger than the unit outcropping at its
centre, the impact occurred prior to the deposition of
the surrounding unit, which never filled the basin
produced by the impact; (2) if a crater is filled by a
unit younger than the surrounding unit, the impact is
deemed to have occurred just before filling, and thus
infill material deposition is coeval with the impact;
(3) if an impact occurred in a region extensively
covered by a single unit, the impact is deemed to
have occurred soon after unit deposition and thus is
coeval with the target unit.
From this classification, we obtain the number
(n) of craters for each class, and by the re-projection
of the map in Fig. 1A to sinusoidal equal area pro-
jection, we obtain the area covered by each unit (A).The ratio betweenn and A represents crater density of
craters with diameters between 40 and 412 km. We
found a relatively constant number of craters per
10E6 km2 from T1 to T4; in particular, 3438 for
classes T4T2 and 23 for T1.
The SFD analysis was performed for each geo-
chronological class. The size-frequency plot N(DCC
dC)/Avs. dCin Fig.3shows that crater classes T1T4
have a fractal behaviour, with the number of craters
inversely proportional to their diameter, and defines
different linear trends following scale-invariant dis-
tributions, S being the exponent of the cumulative
crater SFD (i.e., the fractal dimension of each crater
class). The cumulative number of craters (N) is nor-
malised to the area covered by each geological unit to
which each crater class refers (A). It is interesting
to note that the value of Sdecreases across classes
from T4 (3.38 0.08) to T3 (3.16 0.09), T2
(2.81 0.1) and T1 (2.68 0.11), indicating a
change in the fractal behaviour of the population. This
change is likely driven by a variation of one or more ofthe properties affecting the impact (Eq. 1) and involves
all the craters of the same class.
To further constrain our analysis and to avoid
statistical redundancy of larger craters (in particular
for classes T3 and T1), we removed craters with
diameters larger than 120 km (Fig.4). Reducing the
upper limit allow us to analyse craters formed by the
flux of asteroids of diameter (DA) within the range
from 13 to 310 km (i.e., 12 B DC/DA B 40;
MELOSH, 1989; OKEEFE and AHRENS 1993), and
allows us to focus on asteroids considered to have a
constant flux toward the terrestrial planet region over
the last 3.5 Ga (BOTTKE et al. 2002; MINTON and
MALHOTRA2010). This further constraint permits us to
highlight the effects of other parameters, which affect
craterization aside from the variation of the flux of
impactors (e.g. the variation of rheological properties
of target material). Also, in this case, we found a
relatively constant number of craters per 10E6 km2
from T4 to T1; in particular, 3234 for classes T4T2
and 20 for T1. SFD still follows different linear trends
with S, which is constant for classes T4 and T3
(3.49 0.1) and decreases from classes T2
(2.56 0.05) to T1 (2.09 0.04) (Fig.4).
3. Discussion
The results of the SFD analysis presented in
Fig.4 can be explained by one or more of the fol-
lowing hypotheses: (1) a change in the flux (number
and/or size) of impactors through the Hermean sur-
face, (2) the variable angle of incidence of impactors,
(3) varying impact velocities, (4) a different rheo-
logical response of the planetary crust to impactors.
These results can also represent effects of the overlap
of the mapped units. The main limitations pertaining
to this global scale approach came from the lack of
chronological and stratigraphic constraints on unit
deposition. These limitations are more evident and
efficient in a global-scale approach than in a local
scale approach, because of the wider distribution of
deposits and the higher complexity of the geological
scenario. Resurfacing events (producing unit over-
laps), if present, are certainly a limitation to crater
statistics (MICHAEL and NEUKUM2010): increasing the
area of interest for the analysis will increase theprobability of including regions where units overlap.
This, in turn, means that statistics of the underlying
unit will be incomplete if calculated after the depo-
sition of the mantling unit. This problem is certainly
significant, and is directly related to the uncertainties
concerning the sub-surface geometries and distribu-
tion of mapped units. The currently available data do
not allow the exclusion of one or more of the
hypotheses presented above, but the intent of this
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paper is to contribute to the debate with an approach
to global scale analysis by providing relevant issues
for discussion.
The first hypothesis cannot be excluded by the
available data regarding the uncertainty of the
definition of the age of deposition and the temporal
relationships between one unit and the other.
However, this analysis shows that the density of
cratering [i.e., the ratio between the total number of
craters (n) per each geological unit and the relative
area coverage (A)] is more or less constant (Figs. 3,
4). In the absence of absolute age data about the
deposition of the mapped units, and considering
that all units have likely been deposited in a rela-
tively brief time interval (MARCHI et al. 2013), the
above observation suggests that during the observed
time span or, at least, after the units were depos-ited, the flux of asteroids across Mercurys surface
has undergone negligible variation.
Regarding the second and third hypotheses, the
normal velocity component of an impact, depending on
both velocity and angle of impact, is likely to directly
affect the formation of craters (MELOSH,1989; MARCHI
et al. 2005; HOLSAPPLE and HOUSEN 2007; MASSIRONI
et al.2009: XIAOet al.2014) in relation to the location
of the impact at different latitudes and longitudes.
However, the geological units to which classes T1T4
refer are distributed across the whole planet (Fig. 1A).
We believe that this outcome does not allow for the
possibility that normal velocity variation could play a
key role in generating the observed systematic varia-
tion of S from T4 to T1 crater populations, but
currently, its effects cannot be precisely quantified.
The diameter of the crater can also be affected by
varying only the angle of impact; however, this
would not significantly affect the statistics of the
whole population, because non-circular craters are
only produced for very low impact angles(i.e.,\10) (MELOSH, 1989).
The fourth hypothesis defines the variation in
crater size as a function of the properties of the tar-
geted geological unit (MASSIRONI et al. 2009; XIAO
et al.2014). The variation in Smay, according to this
hypothesis, reflect a change in the rheology of Mer-
curys upper crust (MARCHI et al. 2012).
The dependence of crater size on the rheology of
the target material is given by:
R f g; qA; qT; m; a; U; Yf g 1
in which R is the craters final radius, g the gravita-
tional acceleration, qAand qTthe densities of asteroid
and target, m the impactors mass, a the impactors
radius, U the normal velocity component, and Y the
strength of target material (HOLSAPPLE and HOUSEN2007).
From the power-law relationship defining size-
frequency distributions (Figs. 3and 4), we obtain the
result:
N DC dC =A CdSC 2
in which dC= 2R. Thus, the variations ofScould be
representative of variations in the rheological
parameters (i.e., strength and density) of the materials
involved in the impact, possibly indicating the pre-
sence of a secondary crust and/or a compositional
variation in the population of the LHB projectiles
(MARCHIet al.2012; BROZ et al.2013). However, we
have not found any evidence to support an interpre-
tation of the observed change in S as caused by a
cometary origin of part of the LHB impactor popu-
lation, and this is in agreement with the work of
MARCHI et al. (2012).
Considering the results of the SFD for craters with
diameters between 40 and 120 km (Fig.4), if we
assume that the SFD of asteroids with diameterbetween 3 and 10 km during the observed time
interval related to the mapped geological units was
constant (BOTTKE et al. 2002; MARCHI et al. 2009;
MINTON and MALHOTRA 2010), and normal velocity
component of the impacts to do not affect signifi-
cantly the crater populations, the stratified crust
model could be supported by some observations:
1. LRM and IT units (i.e., crater classes T3 and T4,
respectively) were mapped as very similar depos-
its (DENEVI et al. 2009), the only difference lyingin their colour properties. The slopes of their SFD
are equal for craters with 40 B DCB 120 (Table
in Fig.4), suggesting (in a rheology-driven sce-
nario) that the response to the impact was similar
for both geological units, and therefore that the
rheological properties of the units are similar. This
observation is not supported when the upper limit
in crater diameter is removed, i.e., considering
craters with 40B DCB 412 (Fig.3), because
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Schanges from T4 to T3. However, in this case,
Sis certainly affected by the lack of craters larger
than 250 km found in T3, and more generally, by
the wider population of impactors.
2. The large number of volcanic plains, covering
wide regions of the planets surface (MALIN,1976;
STROM, 1977; SPUDIS and GUEST, 1988; DENEVI
et al. 2009; HEAD et al. 2011; STOCKSTILL-CAHILL
et al. 2012; Denevi et al. 2013), suggests that
resurfacing involved planet-scale areas, and this
observation is in agreement with recent works
(MARCHIet al. 2013).
In this interpretation, the natural conclusion is that
Mercurys surface is younger than 3.5 Ga, and therefore
postdates the LHB. This observation contrasts with pre-
vious works [e.g., models proposing a differentiation in
the origin and evolution of Mercurys impactor popula-
tions, in comparison with data from the Moon and Mars
(STROM etal. 2005; STROM etal. 2008; STROM etal. 2011)].
The contrast might be resolved by considering the oldest
unit IT (i.e., crater class T4) to be the target unit on which
LHB acted. If this is so, LHB produced a greater number
of impacts, and therefore an higher surface alteration
within IT deposits, where volcanic activity was more
intense (IVANOVet al.2002; HEADet al.2011), contrib-
uting to the deposition of the succeeding younger units in
a relatively brief phase after LHB. These units, fillingbasins previously created by LHB impacts, concealed
large numbers of craters and IT deposits, leading to the
present state in which, for population T4, the observed
crater density is clear-cut. In this way, crater class T4 and
therefore IT deposits become the key to definitive proof
of the global-scale effects of LHB emplacement on
Mercurys surface and crustal evolution (MARCHI et al.
2009). However, improvements in the development of
the global geological map (with particular regard to older
terrains) and of evolutionary models of resurfacing his-
tory will certainly contribute to refinement of our model.
4. Conclusions
We conclude that SFD analysis for geologically
constrained global-scale crater classes, if properly
constrained, will allow one to use crater statistics
not only for in situ investigation (referring to a
limited area and to a relative/absolute dating of
deposits in this area), but also for wider applica-
tions. In fact, given the global coverage, these
applications can help us to constrain asteroid flux
models and global resurfacing models, and improve
characterization of target and impactor properties
(geological and rheological). New data from
MESSENGER and the upcoming BepiColombo
mission will help us to more precisely define the
geological properties and the chronology of target
materials formation, while high-resolution images
will improve the quality of the crater catalogue for
low-resolution imaged areas.
Acknowledgments
We would like to dedicate this work to the memory of
Angioletta Coradini, who played a leading role in
many international scientific projects and was among
the founders of space science in Italy. We all miss her
enthusiasm and her contributions to planetary sci-
ences. The authors also thank Caleb I. Fassett for
making the crater catalogue available and for con-
structive comments on a preliminary version of this
paper. We want to thank the two anonymous
reviewers for their constructive and insightful com-
ments, which improved the quality of the manuscript.
This work was funded by the ASI-INAF BepiCo-
lombo agreement number I/022/10/0.
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