Jezero crater, with a diameter of 45
km, hosts two inlet channels of deltaic remnants along
with an outlet channel and embraces hydrated minerals
[1-5]. NE Syrtis (located just south of Jezero crater)
has an area of ~ 2500 km2 and a remarkable mineralogical diversity identified from orbital data as described in Salvatore et al. [6] and references therein.
Thermophyscial characteristics are used to quantitatively measure the physical properties of Martian surface [7-11]. These characteristics can be studied
through determining thermal inertia (TI), albedo, and
diurnal temperature changes on the surface [12-13].
On Mars, thermal inertia is an indicator of surface
geological characteristics [14-16]. Surface physical
properties, spatial distribution, and transportation of
fine materials can be understood from the measurement thermal inertia [17-18]. A lower TI represents
unconsolidated loose, fine surface dust, and very few
rocks, a medium/intermediate TI means combination
of cemented surface, sand sized particles, and a fair
number of scattered rocks, whereas a higher TI indicates rocky surface and bedrock outcrops [14-19]. Alternatively, a TI value of 350 Jm-2
K-1
s-1/2 and >1200 Jm-2
K-1
s-1/2 are representative of well-cemented sedimentary rock and
crystalline igneous rocks, respectively [20-21]. The albedo is an important component of the total energy
balance on Mars by controlling the
maximum surface temperature
[13,19]. Typically, dust-mantled terrains show high albedo (>0.26) while
surfaces with larger grains or rocky
materials show relatively low albedo
[15-16,18]. This study aimed at determining thermophysical properties
of Jezero crater and part of its watershed in NW Isidis and NE Syrtis
between ~170
N to 19.50
N and ~760
E
to 78.50
E. The objectives of the study
are: (a) identifying the distribution of
thermal inertia and albedo, and surface geology, and determining the
relationship between (b) thermal inertia and albedo, and (c) elevation
and thermophysical characteristics.