Geoscience Reference
In-Depth Information
Fig. 3.5.
Spectral solar extraterrestrial flux
F
0
, taking into account the instrumental (K-3)
function (
solid curve
).
Points
show the initial values of
F
0
of the high spectral resolution
from the data according to Makarova et al. (1991)
F
0
have been taken from the topic by Makarova et al. (1991, Fig. 1.3) where the
recent data averaged over several original studies were presented. These values
were recalculated with (1.12) while accounting for the spectral instrumental
function expressed by (3.1) for a correct comparison with the data of the K-3
instrument. Figure 3.5 illustrates obtained curve
F
0
(
λ
). The magnitudes of
δ
correction factor
are presented in the topic by Danishevskiy (1957). The
system of linear equations is finally obtained:
a
1
x
j
+
a
2
y
ij
+
a
3
x
j
+
a
4
y
ij
+
a
5
x
j
y
ij
+
Df
j
−
F
i
=
0,
b
1
x
k
+
b
2
y
ik
+
b
3
x
k
+
b
4
y
ik
+
b
5
x
k
y
ik
+
Df
k
−
F
i
=
0,
(3.7)
a
1
x
j
+
a
2
(−
P
j
)+
a
3
x
j
+
a
4
(−
P
j
)
2
+
a
5
x
j
(−
P
j
)+
Df
j
=
δ
µ
0
.
F
0
System (3.7) consists of (
N
j
+
N
k
)
N
i
+
N
j
equations relative to 11 + 2
N
i
desired
values. Levels
P
i
have been chosen for the equation quantity exceeding the
number of the desired values not less than twice. System (3.7) is solved with
the LST independently for every wavelength, where the inverse squares of the
random standard deviation (Table 3.1) while accounting for the uncertainty
of the deviation from the cosine law are taken as weights. This is to impose
that the additional conditions of the formal mathematical solution do not
contradict physical laws. Here they are: the non-negativity of the radiative flux
Search WWH ::
Custom Search