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change qualitatively in a broad range of ionospheric and magnetospheric pa-
rameters at the transition from
I
=
π/
2 to arbitrary magnetic inclinations. In
order to clarify the validity of that statement, we rewrite (7.99) and (7.100),
introducing parameter
X
K
:
Y
2
∆
A
|
X
K
=
X
−
.
(7.107)
sin
I
|
Then
∆
=
∆
A
∆
SK
,
where
∆
SK
=
ζ
4
κ
s
k
0
−
ζ
3
−
X
K
.
Equation (7.99) for the reflection coecients matrix can be then easily
written as
⎛
⎝
⎞
⎠
κ
S
∆
A
k
0
Y
κ
S
k
0
sign
I
2
∆
A
∆
SK
R
=
1
+
Y
√
ε
m
sin
I
.
(7.108)
∆
S
√
ε
m
−
A little later we shall show that, except of some exotic and practically
uninteresting cases, dependency of
∆
A
on the wa
ven
umber
k
is insignificant
and can be replaced with
∆
(0)
A
+
√
ε
m
)
,
and
X
K
,
in turn, with
=
−
(
X/
|
sin
I
|
Y
2
/
(
X
+
√
ε
m
|
X
(0)
K
) . Equation (7.108) for matrix
R
shows
the results of calculating for
R
with a vertical
B
0
to be transferred to an
arbitrary inclination of
B
0
. It is necessary that we only replace
Y
by
Y/
sin
I
and
X
by
X
K
.
Likewise, matrix
T
=
X
−
sin
I
|
with account being taken of inclination
I
becomes
⎛
⎞
Y
(
m
)
Y
(
m
)
∆
A
g
g
ζ
3
−
−
Y
sign
I
⎝
⎠
2
∆
A
∆
SK
ζ
3
T
=
.
(7.109)
Y
(
e
)
∆
S
Y
(
e
)
g
ζ
2
g
ζ
2
Y
sign
I
−
|
sin
I
|
The Role of the Ground Conductivity
We obtain approximate expressions for transformation matrices for the hori-
zontal wavenumbers
k
0
√
ε
a
k
(7.110)
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