mark kennedy said:
Could you elabortate a little because stellar trignometry does not relate very well to radiometric dating.
Why certainly! See, first we establish that the speed of light in a vaccuum is constant. We know this for quite a while, and while I'm sure you'd love and stay and chat about it, you can go
here or here to
read more about it.
Then there is trigonomity. This is just plain mathemathics. Sounds incredibly complicated and new-age, but infact it isn't. This is a very old technique, which has been used in astronomy for the first time by Friedrich Bessel in 1838 (while measurring 61 Cygni), but on a non-stellar basis this technique is used for other methods for a much longer time.
[history]Aristarchus was born in 310 BC, and allthough very little of Aristarchus' mathematical and astronomical calculations and work has survived the age of time, there are still some very remarkable observations known today that this person has made. Most of the things we know about this man, ironically enough comes from people who didn't share his views of the Universe.
He's considered to be the first person to propose that the Earth orbits around the Sun, an idea not found very likely by the people who studied Artisoteles's work, which later became the base of Roman/Greek science.
Aristarchus proposed that the Earth orbited the sun in a circle, and rotated on its own axis giving rise to both the daily and yearly motions of the night sky. Science as a study of the Universe was in its infancy, and the notion of disproving or supporting a hypothesis using experimentation and observations was simply not done. This was a belief, but with good reasons:
His hypothesis that the Earth orbited the Sun explained the observed nightly and yearly motions of the stars, but it has a catch. If the Earth orbits the sun, the positions of the stars should appear to shift. If you go out tonight and carefully note the position of a star and go back in six months and repeat the observations, the star will have shifted slightly. This is a geometric shift because the Earth has moved from one side of the Sun to the other.
Realizing that there should be a parallax between the stars, mathematical people began to search for one, but with the tools of that time, they rejected Aristarchus's model because they couldn't find it. So even though the rivals of Aristarchus were motivated to reject the idea of the Earth orbiting the Sun for non-scientific reasons, they actually had scientifically justified reasons for rejecting it. [/history]
You can test parallax for yourself though. For instance let's say you have a nearby object in front of you, then you cover one eye with your hand. If you were to move your hand to cover your other eye instead, you'd find out that the nearby object acts as if it jumps horizontially.
The famous astronomer Halley was one of the first the propose that the paralax between Venus, Earth and the Sun
(in famous venus-transists) can be used to detirmine the scale/distance of the solar system.
We can define the parallax as the apparent change in the position of an object due to a change in the location of the observer. What you need in order to measure the parallax is the observation of a distant object from two vantage points, the distance between the two vantage points, and a measurement of an angle.
Consider this simple measurement. Stretch your right arm and close the left eye. With your right eye open, position your thumb in the line of sight of a distant object. Keeping the arm in the same outstretched position, open the left eye and close the right one. You'll see that, with respect to the outstretched arm, the position of the far waway object has shifted. By measuring the angle by which it has shifted, one can get a measurement of the distance. The further apart are the observation points, the better.
In astronomy, parallax measurements take advantage of the fact that, as the Earth orbits around the Sun, relatively near-by stars appear to move with respect to the fixed, very distant stars. I'
ve made this handy dandy graph, that should explain it better then I can do. I've made one minor error: the parallax angle is only half of what 's pictured (that's the /2 part).
To measure the parallax of objects which are very far away from us, we have to use the largest baseline possible. The largest possible baseline is Earth's orbit, and if we'd wait for 6 months we'd be at the other side of the spectrum. Using the Earth's orbit, we make one measurement of the position of a star at two times half a year apart, for example on March 31st and on September 31. you can use any date though.
Parallax measurements depends on how accurately you can measure small angles. The farther a star is, the smaller the parallax angle. If a star is farther than 50
parsecs it will not appear to move with respect to the fixed background stars we use in the measurement.
Let's get a calculating, and let's get started. The distance between our earth and our sun is called one astronimcal Unit (AU) (this is the baseline thing we talked about (shortend to B)). The d stands for the distance (in parsecs).
2þ (in arc seconds) = 2 B / d.
As a reminder: for measurements from the Earth, B = 1 AU. let's take an example, we know that a star is 2 parsecs away, so what's it's arc then?
þ = 1 / 2 = 0.5 arc-seconds
But now we want to know what the distance is. Let's take our nearest star as an example: Proxima Centauri. With help of Nasa (allthough I'm sure you can measure it yourself), we know that the þ is 0,76 arcsec.
d = B / þ.
So if þ=0.76 arc-seconds, B=1 AU, then d=1.3 parsecs. You can convert this then to 4.3 light-years, since 1 parsec = 3.26 light-years. Or you could use
this.
Wikipedia has written a nice piece on it if you want to learn more.
This method only works with stars that are relativly close to Earth.
There are 50 other ways ( like Spectroscopic Parallax, Trig. Parallax, Expansion Parallax, Statistical Parallax, Secular Parallax, Trig exp. Parallax, "Moving cluster method", LED, Spectroscopic Visual Binaries Brightest Cluster Galaxies calb, Faber-Jackson Relation, Type Ia Supernovae effect and many others) to get to know the distance between stars, galaxies, and other stellar objects. Do you understood what I said or do you want to rebute it?