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So we've got a theory of space and time Einstein's theory of general relativity and the idea here is that matter controls the metric which tells you how far apart any two little elements close together in space actually are and the metric might not be the normal one the Pythagoras won but can actually be curved you're all the strange and this causes things to move in funny sorts of ways what's the lot to do with cosmology well I think we're pretty lucky because you know there's almost an infinite number of ways one could twist and turn space, but the universe conveniently appears to be pretty much the same everywhere that is that every part of the universe seems like every other part of the universe and there is no preferred direction and that turns out to give us a lot of leverage on what the metric can or cannot be and this is something that Alexander Friedmann went through and figured out but let's first think about how things work in spherical coordinates which is not something people normally work in okay, so we've talked about the metric before telling you if you've got two objects with the position x camp;z then how far apart they are we've also talked about cylindrical polar coordinates which is where you measure how far out something is around and height, but there's a third sort of coordinate, so it turns out the third sort of coordinates is the ones we actually need to understand the real metric of our own universe and these are called spherical polar coordinates they're also the coordinates used to measure positions on the sky let's do my central declination and it on earth left you NAAFA to tour it spherical polar coordinates so what we've got is we measure angle down from some pole there just Site you measure distance out, and we measure angle around the equator which is Phi in this case, and so I think it's pretty obvious if we want to go from distance, so DS remember it's just how far you're going to travel between point a and point B and our point A's are going to have coordinates R theta and Phi and if we want to just move out in radius by a little of our well that directly translates to s yep, so you're moving our yes is going to be Dr yes since that's easy now if you're going to change an angle down from the pole this would be a bit like latitude on the earth or declination in the sky then if you move a given angle that your distance corresponding to that it's going to be bigger the further out you are if you're very close am I moving small angle doesn't go very far was if I move up a very long lever arm the end moves much further and this is just the small angle approximation we've talked about many times in these courses so far just that the distance is just R times the change in angle theta yep so your s about that you move is that radius times the angle and radians and since we are definitely in the small angle approximation D theta, so it's as small as you can get it should all work yeah then we get to the slightly more...
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