The most basic and intuitive method for
measuring a star's distance employs elementary trigonometry. It is called the "*parallax
method*" because it uses the phenomenon of
"parallax". One can get a simple idea of this by holding an index
finger at arm's length- then looking at it with only
the right eye open, then only the left. What you'll see as you do
this alternatively is the visible shift
of your index finger against the given background. Say from one part of your book
shelf to another. (A very tiny shift.)

The angle that is subtended between the different background points, with respect to your nose ("vertex" of the resulting triangle), say, is the "parallax angle". The diagram below shows how it is measured:

Here,
the points E1 and E2 represent Earth at two opposite points of its orbit around
the Sun. The star indicated is the one for which the distance(d) is sought.
Using photographs of the star taken at the points E1 and E2, we can measure
what is called the angle of parallax p. The solution for the distance can be
obtained from:

d = r/ tan(p)

that is, equal to the radius (R) of the Earth's orbit, e.g 1 A.U. or
astronomical unit = 93 million miles = 1.5 x 10^{11} meters) divided by the tangent of the angle p. (which will be a very small angle). The tangent is a function which denotes a
ratio of lengths for a right triangle. In this case, the tangent of the angle p
is defined:

tan(p) = opposite/ adjacent = R/d

i.e., the side opposite the angle (R),
divided by the side (d = distance to star) adjacent to the angle (d). Using algebra, one
then makes d the subject, which means solving for it.

It can be shown, from the above, that
for angle p = 1" (one second of arc, or 1/3600 of a degree! ) the distance
to the star is always 1 pc (parsec). Bear
in mind 60' = 1 deg and 60" = 1' or 1 minute of arc) the resulting d =
206, 265 A.U. or astronomical units (206, 265 x 1.5 x 10^{11} m).

The
exact term logically chosen for this particular distance is the parallax-second
or *parsec* and doing
the math (tedious, but possible) shows the distance turns out to be:

1 parsec = 3. 26 light years.

Now, given this relationship , it
follows that any proportionate decrease in the angle p allows one to work out
the resulting distance! Thus, if p = 0.5" then d = 2 parsecs or 6.52 Ly,
if p = 0.25" then d = 4 parsecs or about 13 Ly and so on. Thus it was
found that even the nearest stars were light years distant - using the simplest
conceptual method available. The first successful parallax measurements - so
far as we know - took place around 1838, when Friedrich Bessel (Germany), and
Friedrich Struve (Russia) detected the parallaxes of the stars 61 Cygni, Alpha
Centauri and Vega, respectively.

Another application of basic trigonometry in involves obtaining the relative distance to an inferior or superior planet in relation to the Earth. As we've seen before, it's easy to apply Kepler's 3rd law to obtain the basic dimensions of an orbit, namely the semi-major axis of the orbit - or the mean distance from the Sun. But things become somewhat more difficult when we seek to find the distance say, of the Earth to the planet, or the planet at a specific time - say before it commences retrograde motion.

So we consider two cases in the diagram below:

__Case (A) Inferior planet__

*perpendicular*to the planet's heliocentric radius vector, pV. Then by a careful measurement of the angle SEp, say over a series of nights around maximum elongation, one can obtain a value for the angle of maximum elongation. At such time the angle SEp is right-angled hence:

Sp/ SE = sin(SEp)

The quantity Sp/SE is the distance of the planet from the Sun in terms of Earth units or AU, (i. e. astronomical units). Let Sp = R and SE = a(E) the semi-major axis for Earth's orbit, then:

*Example*:

__Case (B) Superior Planet__

Here, we let the planet p be in opposition at some given time with the Earth and Sun (e.g. showing the alignment S-E-p in diagram (B). As we know, with opposition, the elongation is a straight angle or 180 degrees. Then after t days have elapsed the Earth's radius vector SE has moved ahead of the planet’s as shown in comparing SE1 to Sp1. As can be seen, this reduces the angle of elongation from 180 degrees at opposition to angle SE1p1. This is then measured.

Now, over t days, the angle ESp will have increased from 0 (at opposition) to a value Θ given by:

Θ = [n – n

_{p}] t

where n, n

_{p}are the mean daily motions of the Earth and the planet, respectively. Using relations for the periods seen in the previous chapter, we may write:

Θ = 360 (1/P - 1/P') t

where P and P' are the

**(See my post of Jan. 11th) for the Earth and the planet, respectively. Then it follows:**

*sidereal periods*So, since t and S are both known, Θ can be obtained - that is, angle E1Sp1 is calculated. Hence, angle E1p1S can be found from:

angle E1p1S = 180 - angle SE1p1 - angle E1Sp1

sin(p1E1S)/ Sp1 = sin(E1p1S)/SE1

or:

Sp1/ SE1 = sin(p1E1S)/ sin(E1p1S)

again, giving the distance from the Sun in terms of Earth's distance unit.

__Problems: __

1) Estimate the distance of Venus from the Sun at its most recent maximum
elongation, if the angle of max. elongation was 46 degrees.

2) A recent observation of Mars 36.5 days after opposition showed an angle of
elongation = 136 degrees. Find the distance of Mars from the Earth if Mars'
orbital period = 687 days.

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