In the last video, we talked about how parallax
is the apparent change in position
of something based on your line of sight.
And if you experience parallax in your everyday life,
if you look outside of the car window while it's moving,
you see that nearby objects seem to be
moving faster than far away objects.
So in the last video, we measured
the apparent displacement of this star at different points
in the year relative to straight up.
But you could also measure it relative to things in the night
sky at that same time of year, that same time of day that
don't appear to be moving.
And they won't appear to be moving because they're
going to be way, way, way farther away than this star
over here.
There might be other galaxies or maybe even other clusters
of galaxies or who knows.
Things that are not changing position.
So that's another option.
And that's another way to make sure
that you're looking at the right part of the universe.
So you could measure it relative to straight up,
if you know based on the time of year and the time of day
that you're looking at the same direction of the universe.
Or you could just find things in the universe that
are way far back that their apparent position isn't
changing.
So just to visualize this again, I'll
visualize it in a slightly different way.
Let's say, this is our-- let's say,
this is a night field of vision.
Let me scroll to the right a little bit.
Let's say, our night field of vision looks like this.
And I'll do it in a dark color because it's at night.
So our night field of vision looks like this.
And let's say, that this right over here is straight up.
This right here is if we're just looking straight
up in the night sky.
And just to make the convention, in the last video,
I changed our orientation a little bit.
But I'll reorient us in a traditional orientation.
So if we make this north, this is south.
This will be west.
And then this will be east.
So when we're looking at the star in the summer,
what will it look like?
Well, first of all, the sun is just to beginning to rise.
So if you could think about it, this north direction--
we're looking at the sun from-- we're looking at the Earth
from above.
So the north will be the top of this sphere over here.
And the south will be the bottom of the sphere, the other side
of this sphere that we're not seeing.
The east will be this side of the sphere
where the sun is just beginning to rise right over there.
So what will be the apparent position of this star?
Well, it's going to be towards the east.
It's going to be towards the direction
that the sun is rising.
So this angle right over here is going to be right over there.
So this will be the angle theta.
So this is in the summer.
And what about the winter?
Well, in the winter in order-- straight up--
in order for straight up to be that same point in time,
or that same direction of the universe I should say,
then, the sun will just to be setting word.
We're rotating around that way.
So we're just going to be capturing the last two
glimpse of sunlight.
So in that situation, the sun is going to be setting.
So this is our winter sun-- so I'll
do a slightly different color-- will be setting on the west.
And now, the apparent direction of that star
is going to be in the direction of the sun again.
But it's going to be shifted away from center.
So it's going to be to the right of center.
Sorry, to the left of center.
So it's going to be right over here.
And it's a little bit unintuitive,
the way I drew it in the last video.
Well, I won't make any judgment on whether the last one is
easier to visualize or this one is.
Over here, I just wanted to make the conventions
so that north is up, south is down.
But I just want to be clear, over here, the sun is-- well,
sun always sets to the west.
So in the winter, the sun will be right over there.
This will be shifted from center in the direction of the sun.
So it'll be at an angle theta just like that in the winter.
Now, that's all review from the last video
I just reoriented how we visualize it.
What I want to do in this video, given that we can measure
theta, how can we figure out how far this star actually is.
So let's just think about it a little bit
before even give you a theta value.
If we know theta, then we know what
this angle is right over here.
Because this is a right angle, we're
going to know this angle right here is 90 minus theta.
We also know the distance from the sun to the Earth.
And let's say, we're just going to approximate here,
it's one astronomical unit.
It changes a little bit over the course of the year.
But the mean distance is one astronomical unit.
So we know that angle.
We know a side adjacent to the angle.
And what we're trying to do is, figure out a side opposite
to the angle-- this distance right
here, the distance from the sun to the star.
And this is, of course, a right triangle.
And you can see it right here.
Here is the hypotenuse.
So now, we just have to break out
some relatively basic trigonometry.
So if we know this angle, what trig ratio deals
with an adjacent side and opposite side?
So let me write down my famous SOHCAHTOA.
I didn't come up with it.
So the famous SOHCAHTOA.
Sine is opposite over hypotenuse.
Those aren't the two we care about.
Cosine is adjacent over hypotenuse.
We don't know what the hypotenuses is.
And we don't care about it just yet.
But a tangent is the opposite over the adjacent.
So if we take the tangent of the angle.
If we take the tangent of 90 minus theta,
this is going to be equal to the distance to the star.
This distance right over here.
The distance to the star, or the distance from the sun
to the star.
We can later figure out the distance from the Earth
to the star.
It's not going to be too different
because the star is so far away.
But the distance from the sun to the star
divided by the adjacent side, divided
by one astronomical unit.
I'm assuming everything is in astronomical units.
So you can multiply both sides by one.
And you'll get the distance in astronomical units.
The distance is equal to the tangent of 90 minus theta.
Not too bad.
So let's actually figure out what a distance would
be based on some actual measurements.
Let's say, you were to measure some star.
Measure this apparent-- this change in angle right here.
Let's say, you've got the total change in angle
right over here from six months apart, the biggest spread.
And you're making sure you're looking
at a point in the universe relative to straight up.
You can do it other ways.
But this is really just simplifies our visualization
and simplifies our math.
And you get it to be 1.5374 arc seconds.
And I want to be very clear.
This is a very, very, very, very, very, small angle.
Just to visualize it or another way
to think about it is, one point, there
are 60 arc seconds per arc minute.
And there are 60 arc minutes per degree.
Or another way to think about is a degree is like an arc hour.
So if you want to convert this to degrees,
you have 1.5374 arc seconds times
one degree is equal to 3,600 arc seconds.
The dimensions cancel out.
And you get this as being equal to-- get the calculator out.
This is being equal to 1.5374 divided by 3,600.
So it's 4.206.
I'll round because we only want five significant digits.
This is of infinite precision right here
because that's an absolute quantity.
It's a definition.
So let me write this down.
So this is going to be 4.2706 times 10 to the negative 4
degrees.
Could write it just like that.
Now, let me be clear.
This is the total angle.
This angle that we care about is going to be half of this.
So we could divide this by 2.
So let me just do our significant digits 4.2706
divided by 2, or I could even say times 10
to the negative 4-- divided by 2 is
going to be 2.1353 times 10 to the negative 4.
So that's this angle right over here.
This angle, or the shift from center we could visualize it,
is going to be 2.1353 times 10 to the negative 4.
So now that we know that, we already
figured out how to figure out the distance.
We can just apply this right over here.
So let's just take the tangent-- make
sure your calculator is in degree mode.
I made sure of that before I started this video.
--of 90 minus this angle right here.
So instead of retyping it, I'll just write the last answer.
So 90 minus this angle.
And we get this large number-- 268,326.
Now remember, what were our units?
This distance right here is 268,326.
I should just round because I only
have five significant digits here.
300 and-- although with trig numbered, with the trig,
when you're using, involving trigonometry,
the significant digits get a little bit shadier.
But I'll just write the whole number
here 268,326 astronomic units.
So it's this many distances between the sun and the Earth.
Now, if we wanted to calculate that into light years,
we just have to know-- and you could
calculate this multiple ways.
You could just figure out how far
an AU is versus a light year.
So this is AUs.
One light year is equivalent to 63,115 astronomical units,
give or take a little bit.
So this is going to be equal to-- the AUs
cancel out-- this quantity divided
by that quantity in light years.
So let's do that.
So let's take this number the we just got divided by 63,115.
And we have in light years.
And so it's about 4.25 light years.
I'm messing with the significant digits
here but just roundabout answer, 4.25 light years.
Now remember, that's about how far
the closest star to the Earth is.
And so the closest star of the Earth
has this very, very, very apparent,
a very small change in angle.
You could imagine as you go to further and further stars
from this, that angle, this angle right
here is going to get even smaller and smaller
and smaller.
And all the way until you get really far stars.
And it would be, even with our best instruments,
you won't be able to measure that angle.
Anyway, hopefully, you found that cool because you just
figured out a way to use trigonometry
in a really good way to measure angles in the night sky
to actually figure out how far we are from the nearest stars.
I think that's pretty neat.