TEXT: Foundations
  by Greg Egan
  2:  From Special to General
  Copyright © Greg Egan, 1998.  All rights reserved.
  The first article in this series described some of the ways in which the geometry of 
  spacetime affects travellers moving (relative to their destinations, or each other) at a 
  substantial fraction of the speed of light.  By generalising from the Euclidean metric, 
  which captures such familiar aspects of geometry as Pythagoras's Theorem, to the 
  Minkowskian metric suggested by the fact that the speed of light in a vacuum is the same 
  for everyone, we analysed the “rotated” view of spacetime that two observers in relative 
  motion have with respect to each other, and derived formulas for time dilation, Doppler 
  shift and aberration.
  This article and the next will build the framework needed to provide a similar 
  account of the strange effects that have been predicted to take place in the vicinity of a 
  black hole.  To do this, we need to generalise yet again:  from flat geometry, to curved.
  Gravity as Spacetime Curvature
  The basic premise of general relativity is simple:  the correct way to account for the 
  acceleration of objects due to gravity is to consider spacetime to be curved in the presence 
  of matter and energy.  How does curvature explain acceleration?  If two explorers set off 
  from different points on the Earth's equator, and both head north, their paths will grow 
  steadily closer together, despite the fact that they started out in the same direction.  In 
  spacetime, if two nearby stars start out being motionless with respect to each other, their 
  world lines will draw closer together, despite the fact that those world lines were initially 
  pointing in the same direction.  We could say that the force of gravity is pulling the stars 
  together … but we don't say there's a “force” acting on the explorers, do we?  Of course, 
  the two-dimensional surface of the Earth is a visibly curved object embedded in a larger 
  (and more or less flat) space, but we have no reason to believe that spacetime is 
  embedded in anything larger.  Rather, general relativity assumes that whatever gives rise 
  to spacetime geometry in the first place is tied up with the presence of matter and energy 
  in such a way that the resulting geometry is sometimes curved.
  Manifolds
  Before exploring curved geometry, it will be useful to take a look at a kind of geometry 
  that's neither flat nor curved:  geometry without any metric at all.  Essentially, this is like 
  asking what you can say about lines drawn on a sheet of rubber that remains true 
  
  however much you stretch or squeeze the sheet:  distances and angles lose all meaning, 
  but you can still talk about such things as whether or not two lines intersect.  Why is this 
  relevant to general relativity, which does assign a metric to every part of spacetime?  
  Firstly, everything that's true without reference to a metric can be safely carried over to 
  regions of spacetime where the metric varies from place to place.  Secondly, it reflects the 
  situation you find yourself in when you begin to solve a problem in general relativity:  
  initially, you have no idea what the metric is, since that's the very thing the equations are 
  supposed to tell you.
  Let's start with a familiar situation — two-dimensional space, with flat geometry 
  — and see what concepts can survive the loss of the metric.  Choose a city's central post 
  office as the origin for coordinates, measure distances north and east of it, and ignore the 
  curvature of the Earth.  Every building in the city can be identified by a pair of numbers, 
  (x,y), specifying distances east and north of the post office.  Vectors associated with 
  objects in the city can also be given coordinates in much the same way.  For example, a 
  train's velocity can be assigned two coordinates — call them vx and vy — stating how 
  fast the train is travelling east, and how fast it's travelling north.
  Now, imagine that this city lies, not on solid rock, but on a vast sheet of rubber.  
  The railway track and all the buildings are made of equally flexible material, so the whole 
  city can be stretched and squeezed without anything being disrupted.  What's more,  the 
  imaginary grid lines that initially measured distances north and east of the post office have 
  been painted onto the ground, so they too can flex with it.  Then a giant hand descends 
  from the sky and gives one edge of the city a mighty tug.
  Egan: "Foundations 2"/p.2
  
  Figure 2 shows the result.  But the cosmic intervention doesn't stop here; further 
  stretching and compression is applied, at random, 24 hours a day.  The city dwellers 
  simply have to adapt to the fact that streets no longer meet at the same angle from hour to 
  hour, and buildings are no longer separated by fixed distances.  These concepts are soon 
  discarded as irrelevant.
  The first thing to note is that the idea of assigning coordinates to every point 
  doesn't have to be thrown out.  It no longer makes sense to talk about measuring fixed 
  distances in a fixed direction, but a coordinate grid painted on the ground can do just as 
  good a job at identifying buildings, even if the numbers are now entirely arbitrary.  The 
  library's coordinates remain (3,2), whatever shape the city is in, simply by virtue of the 
  fact that the building lies at the intersection of two lines called “x=3” and “y=2”.
  What's more, if civilisation collapsed, the paint faded, and some later generation 
  decided to construct their own new coordinates without ever having heard of distance, 
  any scheme they adopted would be just as good as the old one, so long as it avoided 
  certain pitfalls.  For example, if two grid lines for different values of the x-coordinate 
  intersected, that would leave the x-coordinate of the point of intersection undefined.  We 
  cope with this happening to longitude at the north and south poles, but even linguistically 
  it's a bit of a nuisance.  Sudden jumps in the value of a coordinate — like the jump from 
  longitude 180° west to 180° east — would also add unwelcome complications.  Of 
  course, in the city these problems are easily avoided, but for the surface of the Earth as a 
  whole (and many other examples) they turn out to be inevitable for any single set of 
  coordinates.  In such cases, the best that can be done is to use as many overlapping sets 
  of local coordinates as necessary to cover the whole surface, each of which, 
  individually, is suitably grid-like.
  Egan: "Foundations 2"/p.3
  
  Any mathematical space upon which it's possible to “paint” locally well-behaved 
  coordinates like this is known as a manifold.  An idealised sheet of rubber is a two-
  dimensional manifold.  So is the surface of the Earth; having a metric doesn't disqualify 
  you, it's just not part of the definition.  In general relativity, spacetime is assumed to be a 
  four-dimensional manifold:  at least locally, spacetime can always be given coordinates 
  like those of a four-dimensional grid.
  Returning to the city, one question we still haven't dealt with is the fate of the idea 
  of a “vector”.  Does this make any sense at all, without distances and angles?  
  Surprisingly, it does.  For example, we can still compare one velocity to another, at least 
  at the same point.  A train passing over twenty sleepers per second is, in a very real 
  sense, moving twice as fast as a ghostly second train sharing exactly the same stretch of 
  track but doing just ten sleepers per second; you don't need to worry about distances 
  between the sleepers to know who's being left behind.  And the train is certainly moving 
  in a different direction than a car driving over a level crossing at the same location; the 
  angle between the road and the railway line might be undefined, but no matter how the 
  ground flexes to bring  them together, the two different paths can't be made completely 
  indistinguishable.
  It's easy to assign coordinates, vx and vy, to the train's velocity:  just observe the 
  rate of change of the train's x- and y-coordinates.  This tells you how fast it's passing 
  over the city's coordinate grid lines, rather than how fast it's passing over sleepers along 
  the track.  In Euclidean space, this method agrees exactly with the usual way of splitting 
  up a velocity into components; with the grid in Figure 1 it would yield the expected 
  values in kilometres per hour.  Without a metric, the values are just “coordinate units per 
  hour”.  The particular values of vx and vy depend on the coordinate system being used, 
  but that's equally true with Euclidean coordinates:  if you rotate your axes from north and 
  east to some other orientation, you measure components of the velocity in different 
  directions, so the values are different.
  Still, the motion of the train along the track is something quite independent of any 
  grid painted over the city, and it ought to be possible to characterise it on its own terms.  
  In fact, there's a definition of a vector on a manifold that does this perfectly.  Think of the 
  familiar “number line” of high school mathematics, and imagine drawing part of it on a 
  manifold, so it passes through some point P.  There are lots of different ways you could 
  do this:  crossing into P from different neighbouring points, and crowding or stretching 
  the numbers on the line by various degrees as you approach.  (Even though there's no 
  such thing as distance, once you pick a certain curve through P you can compare two 
  ways of drawing the number line along that curve.)  The combination of the direction in 
  which the line passes through P, and the rate at which the numbers are changing at P, 
  together define a unique tangent vector at P.
  Egan: "Foundations 2"/p.4
  
  Tangent vectors are often drawn as arrows of different lengths, tangent to the 
  curves that define them.  Figure 3 shows several such curves and arrows (successive 
  dots mark successive integer values along the curves).  The lengths of these arrows and 
  the precise angles between them are arbitrary; without a metric, the most you can talk 
  about meaningfully is the ratio of the size of one vector to another that's pointing in the 
  same (or precisely the opposite) direction.
  Velocity vectors are also drawn as arrows in Figures 1 and 2, and though this is a 
  convenient thing to do, it's worth stressing that these arrows aren't “part” of the city, in 
  the way that a road or a railway line is.  Two different diagrams have actually been 
  overlaid here, for convenience:  on top of the drawing of the city is a drawing of the 
  abstract “space” of velocity vectors for the train.  In general, the vectors at each point in a 
  manifold comprise what's known as the tangent space for that point.
  How, exactly, do we make use of our new definition of vectors in terms of 
  numbered curves?  (Or to introduce the correct terminology, parametrised curves, 
  with the numbers along the curve known as its parameter.)  The railway track in Figure 
  2 is just like one of the curves in Figure 3, and the passage of the train along the track 
  assigns a parameter to every point:  t, the time when the train passes.  (Think of a 
  machine strapped to the front of the engine, time-stamping every sleeper.)  And what we 
  can do with such a curve is compute the rate of change of any other quantity that we 
  associate with points in the city, with respect to the parameter t.
  We've already done just that:  in defining the velocity's coordinates, vx and vy, 
  we took the rate of change  (with time) of x and y, two numbers that label every point in 
  the city.  But there's no reason why we have to confine ourselves to coordinates.  To 
  make our city even more fanciful, assume that the ground magically drags the air along 
  Egan: "Foundations 2"/p.5
  
  with it when it's deformed, so that at any given moment, every point in the city will have 
  a certain temperature, a certain air pressure, a certain carbon monoxide level.  The train's 
  velocity then offers a way of computing a rate of change of any one of these, as it 
  ploughs across thermal (or pressure, or pollution) gradients.
  A quantity with a value at every point in a manifold is called a scalar field.  We 
  write the rate of change of a scalar field, f, along a curve with parameter t, as ∂tf.  Don't 
  be put off by the symbol; this is just shorthand for:  “Look at two points on the curve, 
  with t values t1 and t2, and f values f1 and f2.  Then ∂tf is the value that the ratio 
  (f2–f1)/(t2–t1) approaches as the points get closer together”.
  Using this terminology, we can write:
  vx
  =
  ∂tx
  (1a)
  vy
  =
  ∂ty
  (1b)
  for the coordinates of any vector, v:  these are the rates of change of the ordinary 
  manifold coordinates as we move along the curve that defines the vector.  In cases other 
  than velocity the curve parameter need not have anything to do with time, so in general 
  the most that can be said about vector coordinates is that they're measured in “coordinate 
  units per parameter unit”.
  In effect, the vector v is the operation described by the symbol ∂t, since that 
  captures everything about the train's motion (or whatever) at the point in question.  If a 
  vector v is defined by a curve with parameter t, we'll use v and ∂t interchangeably, and 
  write v(f) for the rate of change, ∂tf, of a particular scalar field.
  We can add and subtract vectors, or multiply a vector by a numeric factor, to yield 
  a new vector.  The simplest way to do this is to declare that the rate of change of any 
  scalar field is linear in terms of the vector:
  (av + bw)(f)
  =
  av(f) + bw(f)
  (2)
  for any numbers a and b, and any vectors v and w.  We can then write any vector v as a 
  linear expression in terms of coordinate vectors:
  v
  =
  vx∂x + vy∂y
  (3a)
  and the rate of change for a particular scalar field, f, as:
  v(f)
  =
  vx∂xf + vy∂yf
  (3b)
  What does this mean?  The two coordinate vectors, ∂x and ∂y, are defined by grid lines, 
  Egan: "Foundations 2"/p.6
  
  rather than the time-stamped railway track; the symbols ∂x and ∂y just mean “take the rate 
  of change of anything, with respect to x (along a curve of constant y), or with respect to 
  y (along a curve of constant x)”.  Equation (3a) then tells us that a certain linear 
  combination of those two rates of change will give the rate of change for the train as it 
  moves along the railway line.  To make this concrete, let's take the rate of change of air 
  pressure, and rewrite Equation (3b) in English:
  (The rate of change of air pressure with time, for the moving train) equals 
  (the rate of change of x with time, for the train) times (the rate of change 
  of air pressure with x), plus (the rate of change of y with time, for the 
  train) times (the rate of change of air pressure with y).
  The advantage of describing v with Equation (3a), rather than just stating its coordinates 
  (vx,vy), is that it's an expression for the vector itself, true regardless of the coordinate 
  system.  Sure, v is described in terms of particular coordinate vectors, but if we want to 
  change coordinates, and if we know how to describe ∂x and ∂y in terms of the new 
  coordinate vectors, we can just substitute those descriptions into Equation (3a).
  There's one more geometrical object on manifolds that we need to talk about, which 
  arises directly out of the idea of scalar fields.  Figure 4 shows a series of contour lines for 
  air pressure over the city:  lines along which the pressure is constant, or “isobars”.  The 
  arrows crossing the isobars show the direction in which the pressure difference is driving 
  the air (ignoring all real meteorological complications like the Coriolis force).
  The arrows in Figure 4 are drawn perpendicular to the contour lines, so for a 
  Egan: "Foundations 2"/p.7
  
  moment let's stick to Euclidean space, where “perpendicular” actually means something.  
  There are plenty of other examples where this idea is useful.  Which way will a boulder 
  roll at a certain point on a complicated hilly terrain?  Draw contour lines for altitude, then 
  draw an arrow perpendicular to the contour line passing through the boulder.  There are 
  two possible arrows you could draw; pick the one in the direction of decreasing altitude, 
  and that's the way the boulder will fall.  You can even give the arrow a length 
  proportional to the steepness of the ground; that is, the rate of change of altitude with 
  distance.  Rate of change?  That sounds like a vector!  It is; it's called the gradient 
  vector for the scalar field of altitude.  Actually, the gradient vector is defined as the 
  direction in which the scalar field increases — it's uphill, not downhill — so the motion 
  of the boulder is in the opposite direction to the gradient vector.  Similarly, the motion of 
  air in Figure 4 is in the opposite direction to the gradient vector for the air pressure.
  In a manifold without a metric, there's no way of classifying two directions as 
  being “perpendicular”, so you can't construct gradient vectors from a scalar field.  
  However, you can still ask how rapidly the contour lines are crossed when you're 
  moving with a certain velocity.  This is really the same thing as asking for the rate of 
  change of the scalar field; you just have to take account of the interval between the 
  contour lines and the direction in which you're crossing them.
  For example, the train in Figure 4 is crossing the isobars in the direction of 
  decreasing pressure, so if p is the pressure, ∂tp will be negative, and equal to –0.5 times 
  the number of isobars the train is crossing per second (since the isobars are drawn at 
  intervals of 0.5 kiloPascals).  If the train was moving in the opposite direction, ∂tp would 
  be positive, and if the track was at a tangent to the contour lines, ∂tp would be zero.  But 
  you can't single out any one direction in which ∂tp is greatest, because you can make ∂tp 
  as large as you like just by travelling faster.  In Euclidean space, you can pick the 
  direction which, for a given speed, yields a faster rate of change of air pressure than any 
  other direction.  Without a metric, though, “a given speed” means nothing.
  The geometrical object the contour lines themselves represent is known as a 1-
  form.  (There's a reason for this:  the process we used to get contour lines from a scalar 
  field can be generalised to make structures called 2-forms, 3-forms, and so on.)  The 
  1-form generated from the scalar field f is called df, or “the differential of f”.
  What can we do with a 1-form?  As we've seen, we can combine it with a vector 
  at any point to get a number.  This number is known as the inner product of the 1-form 
  and the vector.  The inner product is written by enclosing the 1-form and the vector in 
  angle brackets, e.g.:
  <df,v>
  =
  v(f)
  (4)
  Equation (4) is just convenient shorthand for the things we've been discussing.  The 1-
  Egan: "Foundations 2"/p.8
  
  form df means “the contour lines of f”, and <df,v> means “the rate at which someone 
  travelling with velocity v crosses the contour lines of f, times the interval at which those 
  contours are drawn … times minus one if they're being crossed in descending order”.  
  On the right hand side, v(f) is “the rate of change of f for someone travelling with 
  velocity v.”
  While keeping the picture of contour lines in mind, we can also give a slightly 
  more mathematical definition of a 1-form:  it's anything that we can combine with a 
  vector to yield a number at any point in the manifold, such that the number we get is 
  linear with respect to the vector.  In other words, doubling the vector doubles the result, 
  and a vector that's the sum of two others gives the sum of the individual results.  Since 
  the rate of change that a vector gives from a scalar field is linear in terms of the vector — 
  see Equation (2) — the inner product defined by Equation (4) will also be linear:
  <df,av + bw>
  =
  (av + bw)(f)
   
   
  =
  av(f) + bw(f)
   
   
  =
  a<df,v> + b<df,w>
  (5)
  There's no reason why you can't have a 1-form — call it m — that satisfies these 
  equations in place of df, but doesn't happen to be the differential of any scalar field.  We 
  could draw a stack of lines at any point that yielded the right inner product for m, but 
  they wouldn't intermesh from point-to-point like the true contour lines in Figure 4.  In 
  this case, it makes more sense to think of the lines being drawn in the tangent space for 
  each point, since they don't really belong in the manifold.  The inner product then counts 
  how many lines of the 1-form a given vector pierces, from base to tip (with the usual 
  corrections for interval and direction).
  Just as we can add and subtract vectors, and multiply them by numeric factors, 
  we can do the same with 1-forms, by declaring that the inner product will be linear, not 
  just in the vector, but in the 1-form as well:
  <am + bn,v>
  =
  a<m,v> + b<n,v>
  (6)
  And just as we can give a vector v coordinates vx and vy, we can give a 1-form m 
  coordinates mx and my.  (Note that vector coordinates are written with superscripts, and 
  1-form coordinates are written with subscripts.)  These are defined by:
  mx
  =
  <m,∂x>
  (7a)
  my
  =
  <m,∂y>
  (7b)
  which, for the special case of m = df, become:
  Egan: "Foundations 2"/p.9
  
  (df)x
  =
  ∂xf
  (7c)
  (df)y
  =
  ∂yf
  (7d)
  Here, the units for the 1-form's coordinates are “scalar field units per coordinate unit” 
  (e.g. kiloPascals per coordinate unit).  In general, when m is not a differential, all we can 
  say is that mx and my are in “1-form units per coordinate unit”.
  We can write the 1-form itself in terms of two coordinate 1-forms:
  m
  =
  mxdx + mydy
  (8)
  where dx and dy are just the differentials of the manifold coordinates x and y, which are 
  two perfectly good scalar fields after all.  Note that:
  <dx,∂x>
  =
  1
  (9a)
  <dx,∂y>
  =
  0
  (9b)
  <dy,∂x>
  =
  0
  (9c)
  <dy,∂y>
  =
  1
  (9d)
  which in turn lets us write:
  <m,v>
  =
  <mxdx + mydy, vx∂x + vy∂y>
   
   
  =
  mxvx  + myvy
  (10)
  If you multiply the units involved, the manifold's coordinate units cancel out, 
  yielding “1-form units per parameter unit”.  Unlike the individual coordinates vx, vy, mx 
  and my, this number is completely independent of the coordinate system.  Why?  Because 
  it's almost just counting the number of intersections of one line with some other lines — 
  and you can't get much more objective than that.  The only proviso is that the 1-form and 
  the vector's curve parameter do involve a particular choice of units; for example, in the 
  case of our train crossing the air pressure contours, the inner product <dp,v> would be 
  in kiloPascals per second.
  Curved Geometry
  Now that we have a set of geometrical objects at our disposal that can function 
  independently of any coordinate system — let alone any metric — the idea of doing 
  geometry with a variable, curved metric becomes much less daunting.  When Einstein 
  was developing general relativity he postulated that the laws of physics should be 
  Egan: "Foundations 2"/p.10
  
  generally covariant, which means it should be possible to formulate those laws in a 
  way that works equally well for any choice of coordinates.  This is not to claim that there 
  is no objective difference between, say, the way we normally measure coordinates 
  around us in nearly flat spacetime (x, y, and z measured at right angles to each other, t 
  measured in the direction of our world lines), and some arbitrary set of wiggly lines, 
  resembling Figure 2.  We can tell the difference very easily!  But you can state the laws 
  of physics, and solve the appropriate equations, without knowing in advance how to 
  construct a coordinate grid with lines as straight as possible, meeting at right angles.  The 
  metric that defines these things is very real, but unless you have firsthand experience of 
  the region of space in question, it's something you don't know until you've calculated it.
  To study curvature, though, we're initially going to use examples where we don't 
  have to solve equations in general relativity to find the metric.  Rather, we'll look at 
  curved surfaces in flat space, where the metric is “inherited” from the three-dimensional 
  space in which the surface is embedded.  Spacetime curvature doesn't arise like that — 
  the metric is not inherited from some larger, flat “hyperspace” — but we can still define 
  measures of curvature that are equally applicable in both cases.
  Figure 5 shows the surface of the Earth, covered with a  familiar coordinate grid:  
  x and y are just longitude and latitude.  As mentioned earlier, there are problems with this 
  grid at the poles and the 180° meridian, but we'll stick to a region that avoids those 
  mathematical trouble spots.  We will make one slight change from the standard way of 
  measuring latitude and longitude:  we'll measure these angles in radians, rather than 
  degrees.  If you haven't come across this before, it's an extremely simple idea; 360° is 
  equal to 2π radians — the circumference of a circle with a radius of one — and any 
  smaller angle's equivalent in radians is just equal to the length of a proportionately 
  smaller arc.
  Egan: "Foundations 2"/p.11
  
  As before, imagine a train in motion across this surface.  But now that the notion 
  of “distance” is allowed, we can ask:  what's the relationship between the train's speed, 
  in kilometres per hour, and vx and vy, the rate at which its x- and y-coordinates are 
  changing?  If the train was heading purely in the y-direction, due north along a meridian, 
  its speed would be equal to Evy, where E is the radius of the Earth.  Why?  Because vy is 
  just ∂ty, the rate of change of the train's angle from the equator.  Multiplying by the 
  radius of the meridian the train is travelling on — which is just the radius of the Earth — 
  converts an angle (measured in radians) into an arc length; equally, it converts a rate of 
  change with time of that angle into the rate of change of the arc length.
  If the train was heading purely in the x-direction, along a line of latitude, almost 
  the same argument would apply.  However, the radius of each circle of latitude obviously 
  depends on the latitude, and it's not hard to see that the value is E cos y.  So the train's 
  speed would be (E cos y) vx.
  Given that the train is actually heading partly in each of these two directions, we 
  can use Pythagoras's Theorem to find its speed.  This is where we make use of the plain 
  old Euclidean metric of flat, three-dimensional space.  The two directions, ∂x and ∂y, are 
  at right angles to each other, and from a satellite's point of view they can be treated like 
  vectors in a Euclidean plane.  The speed of the train is:
  |v|
  =
  √[(E cos y)2 (vx)2 + E2 (vy)2]
  (11)
  What metric for the curved surface of the Earth will agree with this result?  A metric 
  applied to the same vector twice is supposed to yield the square of the length of that 
  vector, |v|2=g(v,v), so:
  Egan: "Foundations 2"/p.12
  
  g(v,w)
  =
  (E cos y)2 vxwx + E2 vywy
  (12)
  is clearly compatible with Equation (11), since this gives:
  g(v,v)
  =
  (E cos y)2 (vx)2 + E2 (vy)2
   
  We can use Equation (12) to find the train's speed from the rates at which its 
  longitude and latitude are changing, anywhere on the surface of the Earth (except for the 
  poles and the 180° meridian).  However, we can't substitute, say, the x- and y-
  coordinates of the point P in Figure 5 in place of vx and vy, and expect Equation (12) to 
  give us the distance from O to P.  Why not?  Because the metric's relationship to the 
  coordinates changes as you change latitude; that “cos y” in the formula means you can't 
  just add up the length of all the steps you took as you walked from O to P, and expect 
  them all to bear an identical relationship to the amounts by which they increased your 
  latitude and longitude.  In Euclidean space, if you head off along a straight line, equal 
  strides always involve the same increments in your x- and y-coordinates.  In general, this 
  isn't true.  What you can always do is use calculus to add up the distance along any path, 
  taking account of the varying relationship of distance to the coordinates.  That's not 
  difficult, but we won't go into the details here.
  Equation (12) can be rewritten in a way that makes it clear that the metric is a 
  geometrical object, independent of the coordinate system.  Equations (3a) and (9) allow 
  us to rewrite the coordinates of the vectors in terms of inner products with the coordinate 
  1-forms:  vx=<dx,v>, vy=<dy,v>, and similarly for the coordinates of w.
  g(v,w)
  =
  (E cos y)2 <dx,v><dx,w> + E2 <dy,v><dy,w>
   
  This in turn can be expressed with a more compact notation:
  g
  =
  (E cos y)2 dx⊗dx + E2 dy⊗dy
  (13)
  The symbol ⊗ is called the tensor product.  Just as dx and dy can be combined with a 
  single vector to yield a number, dx⊗dx and dy⊗dy can be combined with pairs of 
  vectors to yield numbers.  You can multiply as many 1-forms as you like in this fashion, 
  and they need not be the coordinate 1-forms.  For example, if m, n and p are 1-forms 
  and u, v and w are vectors:
  m⊗n⊗p(u,v,w)
  =
  <m,u><n,v><p,w>
   
  Egan: "Foundations 2"/p.13
  
  You can also combine vectors in the same fashion, or even a mixture of vectors and 1-
  forms:
  u⊗v(m,n)
  =
  <m,u><n,v>
   
  m⊗n⊗w(u,v,p)
  =
  <m,u><n,v><p,w>
   
  The tensor product of r vectors and s 1-forms is called a tensor of rank (r,s).  
  Since each vector can create a number if combined with a 1-form, and each 1-form can 
  create a number if combined with a vector, you can “feed” r 1-forms and s vectors to 
  such a tensor, and it will give you a number.  Because this number is produced by 
  multiplying a string of inner products together, and each inner product is linear in both 
  the 1-form and the vector, tensors are completely linear:  feed them anything twice as big, 
  and the number they produce from it will be doubled.
  Equation (13) shows that the metric for the surface of a sphere is a tensor of rank 
  (0,2):  it can be fed two vectors, and from them it produces a number.  In the previous 
  article, we showed that both the Euclidean and Minkowskian metrics are linear, so this 
  aspect should come as no surprise.  We also showed that those metrics were symmetric, 
  i.e. g(v,w)=g(w,v), which is also clearly true of Equation (13), since it's the sum of 
  two tensors which combine identical 1-forms with the first and second vectors fed to 
  them.  The most general form a two-dimensional metric can take is:
  g
  =
  gxxdx⊗dx + gxydx⊗dy + gyxdy⊗dx + gyydy⊗dy
  (14)
  where each of the numbers gxx, gxy, gyx, gyy can vary from point to point in the 
  manifold, but gxy must equal gyx everywhere, to ensure that the metric is symmetric.  
  These numbers are called the coordinates of the metric, and like those of vectors and 1-
  forms they depend on the particular coordinate system being used.  But Equation (14) as 
  a whole is independent of the coordinate system.  To take a simple example, if we 
  switched from x and y to new coordinates u and v, where u=x/2 and v=y/2, we'd make 
  the substitutions du=dx/2, dv=dy/2 (i.e. dx=2du, dy=2dv):
  g
  =
  4gxxdu⊗du + 4gxydu⊗dv + 4gyxdv⊗du + 4gyydv⊗dv  
   
  =
  guudu⊗du + guvdu⊗dv + gvudv⊗du + gvvdv⊗dv
   
  So the metric's new coordinate  guu is equal to 4gxx, but that's balanced by the 
  fact that du⊗du yields numbers one-quarter the size of those dx⊗dx yields from the same 
  vectors.  The same thing holds for guv, gvu, and gvv.  The metric's coordinates have 
  changed, but the thing itself is unaltered, just as a train travelling down a railway track is 
  unaltered by the coordinates used to measure its velocity.
  Egan: "Foundations 2"/p.14
  
  Parallel Transport
  It's common knowledge that the “straightest possible” line — the technical name for this 
  is a geodesic — between two points on the surface of a sphere is an arc of a great circle, 
  a circle whose radius is equal to the radius of the sphere.  If you travel along a great 
  circle, there's a sense in which your velocity vector is always pointing in “the same” 
  direction, as opposed to swerving from side to side.  But what exactly does this mean?  
  It's easy to say when two vectors at different points are parallel in Euclidean space — in a 
  rectangular coordinate system the two vectors will have identical coordinates — but in 
  curved space, the issue is a great deal more subtle.
  Figure 6 shows the velocity vector ∂t at two different points for a ship travelling 
  at a constant speed along a great circle.  From a satellite's view, the velocity is clearly 
  different from P to Q, but both vectors lie in the same plane:  the plane of the great circle.  
  As the ship moves around the Earth, it can't head off along a truly straight line; that 
  would take it up into space!  Instead, its velocity vector has to rotate downwards, in order 
  to stay horizontal as the Earth curves away.  This rotation is entirely perpendicular to the 
  surface of the Earth; if it was partly sideways, the ship would swerve off course.
  That's simple enough, but how can we characterise this from the ship's point of 
  view?  The coordinates of its velocity clearly don't stay constant:  at P the ship is heading 
  north-east, and at Q it's heading south-east.  In general, vx and vy are going to change in 
  a complicated manner, even as the ship maintains a constant speed along a geodesic.
  The idea that we can take a vector at P and move it along some path to Q — 
  Egan: "Foundations 2"/p.15
  
  without “really” changing it, even though its coordinates might change — is known as 
  parallel transport.  It's this idea that defines a geodesic:  parallel transport tells you 
  how to carry a kind of “reference copy” of your initial velocity with you as you go.  If 
  your actual velocity agrees with the reference copy all the way, you're moving along a 
  geodesic; if it doesn't, you're not.
  Physically, you could do this by setting a gyroscope spinning with its axis in the 
  direction of your initial velocity (and subtracting out the gradual tilt of the axis towards 
  the vertical, as the local definition of “horizontal” changed), but what we need is a 
  mathematical recipe to predict the difference between the gyroscope's direction and a 
  fixed compass bearing.  We'll assume that parallel transport is a linear process for the 
  vectors being “transported”:  adding two vectors or multiplying a vector by some number 
  at the starting point, and then transporting the result, ends up giving you the same final 
  vector as doing the transporting first and the adding or multiplying later.  We'll also 
  assume that over very short distances the difference between gyroscope and compass 
  bearing is linear for the vector describing your motion; this is really just saying that the 
  recipe for parallel transport, though it will vary from point to point (like the metric), 
  doesn't undergo any wild jumps that would stop you from treating it as fixed over a small 
  enough region.  Then if we know what happens to ∂x when we move a short distance ε 
  in the x-direction, what happens to it if we move in the y-direction, and what happens to 
  ∂y after the same two moves, all these assumptions of linearity let us work out what 
  happens to any vector, moved (a short distance) in any direction.
  It's standard notation to write the effects of these four possible moves as:
  ∇x∂x
  =
  Γxxx ∂x + Γyxx ∂y
  (15a)
  ∇y∂x
  =
  Γxxy ∂x + Γyxy ∂y
  (15b)
  ∇x∂y
  =
  Γxyx ∂x + Γyyx ∂y
  (15c)
  ∇y∂y
  =
  Γxyy ∂x + Γyyy ∂y
  (15d)
  Don't be put off by the unfamiliar symbols; as ever, this is just shorthand for 
  things we've just discussed.  After increasing our x-coordinate by a small amount ε, “the 
  difference between the ∂x the coordinate grid gives us and the parallel-transported 
  reference copy of the ∂x we started off with, divided by ε” is what we'll call ∇x∂x, with 
  the subscript x in ∇x indicating the direction of the move.  We divide out the particular 
  change in x, ε, because the effect is linear, and what we really care about is the rate per 
  coordinate unit.  This is a vector, with coordinates Γxxx and Γyxx.  Once you include the 
  two coordinate vectors and the two directions you can consider moving in, there are eight 
  of these numbers at every point, and together they characterise a particular way of doing 
  parallel transport.  They're known as the connection coefficients for the geometry, 
  or sometimes the Christoffel symbols.
  Egan: "Foundations 2"/p.16
  
  This gives us the language in which to talk about parallel transport, but we still 
  don't know what recipe to use in any given case — what the values of the connection 
  coefficients are, in terms of the metric.  It turns out that there are two equivalent ways to 
  pin this down.  You can assume either that:  (1) parallel transport must yield geodesics 
  that give the shortest possible distance between nearby points (or in spacetime, the 
  longest distance), or (2) parallel transport of vectors changes neither their length nor the 
  angle between them, and what's more ∇y∂x=∇x∂y:  the x coordinate vector changes 
  when you move in the y-direction in exactly the same way as the y coordinate vector 
  changes when you move in the x-direction.
  It's beyond the scope of this article to prove that these requirements are identical, 
  but it's worth knowing both.  Condition (1) is very simple to talk about, and makes great 
  intuitive sense.  In Euclidean space, straight lines are the shortest paths between points, 
  so it's only reasonable that the “straightest” path between points in curved space should 
  be the shortest.  In Minkowskian spacetime, straight lines are the longest paths, so the 
  same should apply to geodesics in curved spacetime.  In fact, the fundamental reason for 
  all of this lies in quantum mechanics, but that's a topic for a later article.  Condition (2) is 
  a little more complicated, but the first part sounds pretty reasonable:  if the reference copy 
  of our ship's velocity changed length as we moved, what sort of standard would it be?  
  And if we carried a reference copy of “starboard” (to the right) that didn't continue to lie 
  at 90° to the reference copy of our velocity, we wouldn't know which to steer by, since 
  the two would contradict each other.
  It's possible to use Condition (2) to write a completely general formula for the 
  connection coefficients in terms of the metric, but we'll just state the results for the 
  surface of a sphere:
  ∇x∂x
  =
  (sin y cos y) ∂y
  (16a)
  ∇y∂x
  =
  (–tan y) ∂x
  (16b)
  ∇x∂y
  =
  (–tan y) ∂x
  (16c)
  ∇y∂y
  =
  0
  (16d)
  Equation (16a) says that ∂x (east) tilts in the y-direction (north) when you travel in the x-
  direction (east), to an extent that's zero either on the equator or on the poles (since either 
  sin y or cos y is zero in those cases), and negative in the southern hemisphere.  To see 
  this, find the point on Figure 6 where the great circle is tangent to a circle of latitude, just 
  west of point Q.  The two curves are initially parallel, but then the circle of latitude — the 
  definition of “east” — veers north relative to the great circle.  Equation (16b) says that ∂x 
  decreases in the x-direction (i.e. shrinks) as you travel in the y-direction:  as you travel 
  north, a velocity measured in degrees or radians per hour east comes to mean less and 
  less in terms of kilometres per hour, as the circles of latitude shrink.  Equation (16c) says 
  Egan: "Foundations 2"/p.17
  
  that as you watch ∂y while moving in the x-direction (i.e. keep an eye on what happens to 
  “north”, relative to your gyroscope, as you travel east), it tilts in the negative x-direction 
  (west) by an amount that's greater at greater latitudes (tan y starts off equal to zero at 
  y=0, and grows with latitude).  That makes sense:  the north pole lies precisely on your 
  left when you start out east, but if you travelled along a great circle like the one in Figure 
  6, it would swing to the rear of you, which is west, as you turned to the south.
  The Curvature Tensor
  What happens when you parallel-transport a vector around a closed loop?  Figure 7 
  shows this happening on the surface of the Earth:  a vector v is transported along each of 
  the three sides of a triangle PQR built from geodesic arcs.  The angle between the vector 
  and each geodesic it moves along remains unchanged, and to make the example even 
  simpler, v is chosen initially to be a tangent vector to one side of the triangle, PQ, at P.  
  After being transported from P to Q this is still true — the angle between the vector and 
  the curve remains zero.  Transport from Q to R is almost as easy:  the vector just ends up 
  making the same angle with QR at R and at Q … and then the same can be said about its 
  angle with RP at R and at P.
  At the end of the process, back at P, v no longer points in the same direction.  
  This couldn't happen in Euclidean space, where the vector would remain parallel to its 
  initial position throughout.  In curved space, though, there is no absolute criterion for 
  saying one vector is parallel to another vector at another point.  All you can do is 
  transport a copy of the first vector over to the second one, by a particular route, and see 
  if they agree — and whether they do or don't will generally depend on the path you take.
  Egan: "Foundations 2"/p.18
  
  The failure of the vector to return to its initial direction can be linked to a well-
  known property of triangles in curved space:  the failure of their angles to add up to 180°.  
  The angle the vector v makes with successive sides of the triangle jumps at each vertex, 
  by 180° minus the angle at the vertex; in total, this means it ends up rotated by 540° minus 
  the sum of the angles.  If that sum was 180°, the net rotation would be 360° and the 
  transported vector would match the original.  On a sphere, the angles of a triangle always 
  add up to something more than 180°, so the transported vector in Figure 7 is rotated by 
  less than 360° and fails to line up with the original.
  It's clear that this discrepancy, δv, between the original vector and the transported 
  version must shrink as the triangle (or any other loop) gets smaller, because on a small 
  enough region of the Earth's surface the geometry is indistinguishable from Euclidean 
  geometry.  However, we can still ask exactly how rapidly δv shrinks, and it turns out 
  that for small enough loops it's proportional to the area of the loop, and unaffected by its 
  shape.  So we can create a kind of standardised small loop, a square which consists of 
  travelling ε units in the x-direction,  ε units in the y-direction, –ε units in the x-direction, 
  and –ε units in the y-direction, where ε is a small number whose precise value doesn't 
  matter.  All that's needed to compute the discrepancy in any vector transported around 
  this loop are the connection coefficients, and the rates at which they're changing in the x- 
  and y-directions.
  The result for the surface of a sphere turns out to be quite simple:
  δv
  =
  ε2 (–vy ∂x + vx (cos y)2 ∂y)
  (17)
  Note that this is perpendicular to the original vector:
  Egan: "Foundations 2"/p.19
  
  g(v,δv)
  =
  ε2 ( (E cos y)2 vx(–vy) + E2 vyvx (cos y)2)
   
   
  =
  0
   
  and its size relative to the original vector is:
  |δv|
  =
  ε2 √[(E cos y)2 (–vy)2 + E2 (cos y)4 (vx)2]
   
  |v|
  =
  √[(E cos y)2 (vx)2 + E2 (vy)2]
   
  |δv| / |v|
  =
  ε2 cos y
   
  which is proportional to the area of the loop, once you take into account the fact that ε 
  units of longitude comprise a shorter distance at higher latitudes, by a factor of cos y.  
  For a given loop, δv is perpendicular to v and proportional to it in length, so this 
  confirms that the parallel-transported version of v has simply been rotated (if δv wasn't 
  perpendicular, that would imply some expansion or contraction as well).
  Equation (17) can be rewritten as:
  R
  =
  ∂x⊗dy – (cos y)2 ∂y⊗dx
  (18a)
  δv
  =
  –ε2 R(v)
  (18b)
  where R is a tensor of rank (1,1).  From our earlier description of tensors, a tensor of 
  rank (1,1) would be fed a 1-form and a vector, to produce a number.  But you can also 
  leave the vector part “unfed” — combined with nothing — and use the tensor to produce 
  one vector from another.  In other words, Equations (18a) and (18b) are the same as 
  Equation (17) because (∂x⊗dy)(v)=vy∂x and (∂y⊗dx)(v)=vx∂y, with the 1-forms dy and 
  dx combining with the vector v, and the vectors ∂x and ∂y left untouched as vectors.
  The tensor R is almost the Riemann curvature tensor — a famous 
  geometrical object containing all the information about the curvature of a given space or 
  spacetime.  There's one slight omission, though; we haven't considered the fact that in 
  general, you need to specify what plane the loop lies in.  There's only one possibility in 
  two dimensions, but in three or four you have to specify a choice.  The full Riemann 
  tensor takes this into account:  as well as feeding it the original vector v, you have to feed 
  it two other vectors, say w and z, which together single out the plane of the loop.  
  What's more, you can move the factor of ε into those vectors, so they specify the size of 
  the loop as well.
  We can modify Equations (18a) and (18b) to work like this:
  R
  =
  (∂x⊗dy – (cos y)2 ∂y⊗dx) ⊗ (dx⊗dy–dy⊗dx)
  (19a)
  δv
  =
  –R(v, ε ∂x, ε ∂y)
  (19b)
  Egan: "Foundations 2"/p.20
  
  Here, the (dx⊗dy–dy⊗dx) part of R simply converts the last two vectors fed to R into 
  the number ε2.  But it would cope just as well with whatever vectors you fed it; for 
  example, if you reversed the roles of  ∂x and ∂y and traversed the standard loop in the 
  opposite direction, it would give –ε2 instead.
  In the next article, we'll see how the curvature of spacetime can be linked to the 
  distribution of matter and energy, through Einstein's equation — and then we'll look at 
  one solution of that equation in detail:  a black hole.
  Egan: "Foundations 2"/p.21
  
SOURCE: textdata/thevault/Vault2.0.-.Fiction-and-audiobooks/Books/E/Egan, Greg/Foundations/Egan, Greg - Foundations 2 - From Special To General.pdf