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The apparent position of an object in the sky may be
changed by several different physical effects. The speed of light changes as it passes through a
medium such as air. The speed of light in air depends on its temperature
and its pressure, Make a simple model of the atmosphere as n
layers of uniform air above a flat Earth, At
the first boundary, sin(i1) / sin(r1) = v0
/ v1 . But, by simple geometry, r1 = i2,
r2 = i3 and so on.
So we have In other words, the refractive indices of the
intervening layers all cancel out. Now rn is the apparent zenith
distance of the star, z', Refraction has no effect if a star is at the zenith
(z=0). Define the angle of refraction R by R = z -
z'. We assume R will be small, so, approximately, Thus, approximately, Here v0 is c, the velocity of light in a
vacuum, which is constant. A star is at Right Ascension 5h
0m and declination +26°20'.
How much will the stars
image be shifted by atmospheric refraction, What will be the stars
Right Ascension and declination, Click here
for the answer. At large zenith
distances, this model is inadequate. Previous section:
The Moon
One of these is
refraction.
We define the refractive index of any
transparent medium as 1/v,
where v is the speed of light in that
medium.
so the refractive index of the air varies in
different parts of the atmosphere.
with a different
velocity of light vi for
each layer (i from 1 to n).
Apply Snell's Law of
Refraction at each boundary.
At the next boundary, sin(i2)
/ sin(r2) = v1 / v2 , and so on.
sin(i1) = (v0 /
v1) sin(r1)
=
(v0 / v1) sin(i2)
=
(v0 / v1) (v1 / v2)
sin(r2)
=
(v0 / v2) sin(r2)
=
..........
=
(v0 / vn) sin(rn)
The only thing that matters is
the ratio between v0
(which
is c, the speed of light in vacuum)
and vn (the
speed in the air at ground level).
and i1 is its true zenith
distance, z.
So sin(z) = (v0 / vn)
sin(z').
But at any other position, the star is apparently raised;
the effect is greatest at the horizon.
Rearrange this as z = R + z'.
Then sin(z) = sin(R)
cos(z') + cos(R) sin(z').
sin(R)
= R (in radians), and cos(R) = 0.
sin(z)
= sin(z') + R cos(z').
Divide throughout by sin(z') to get
sin(z)/sin(z') = 1 + R/tan(z')
which is to say,
v0/vn
= 1 + R/tan(z').
So we can write
R
= (v0/vn - 1) tan(z')
We write this
as
R = k tan(z')
where
k = (v0/vn - 1)
But vn depends on
the temperature and pressure of the air at ground level.
At
"standard" temperature (0°C = 273K) and pressure (1000
millibars),
k = 59.6 arc-seconds.
The formula in the Astronomical Almanac is
k
= 16.27" P/(273+T)
where P is in millibars, and T is in °C.
Exercise:
The latitude φ
is +56°20'.
Local Sidereal Time is 5h 0m.
Atmospheric
pressure is 1050 millibars,
and the temperature is +5°C.
What is the stars true altitude?
and in which
direction?
corrected for refraction?
The amount of refraction
near the horizon is actually determined observationally.
At
standard temperature and pressure,
refraction at the horizon
(horizontal refraction) is found to be 34 arc-minutes.
Next section:
Sunrise,
sunset and twilight
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