Did your researches with the slot at §14.14 yield the ‘important discovery’ I hinted at. Perhaps you should try again.

Revise as necessary on isovals–a minimum of §§14.1, 14.5 and 14.9. If you didn't ask yourself whether a branch of an isoval could be a world line – representing something moving on the ID universe – consider the question now.

A time-like isoval couldn't be a world line. For its slope is always shallower than 45°, and this would imply a causal influence travelling faster than light, which is impossible (§§10.10–12).

But a branch of a space-like isoval, being always steeper than 45°, could be a world line. Check with the slot that it represents something always moving slower than light. What sort of motion will it represent?

World lines of inertial observers are straight. So this curve must represent the motion of something that is non-inertial. What does ‘noninertial’ mean?

The meaning is in the definition of §5.2–which please reread. The test particle moves away.

But when there is no gravity–as we are assuming (§5.5)–an inertial observer has constant speed relative to any other inertial observer (§5.6). Therefore a non-inertial observer moves with changing speedhe is accelerated in the ordinary sense of the word. So this space-like isoval represents accelerated motion.

Note that acceleration has a quite different status from speed (§§1.1–3, 5.1–2). Speed is purely relative. But everybody can see whether an observer and his test particle stay together or move apart; and so all must agree whether he is accelerated or not.

So far we've not asked questions about what causes things to accelerate. When we do so, we enter the subject of dynamics. Naturally we shall be concerned with relativistic dynamics – the dynamics of things moving at high speed. But curiously enough the main difficulty for most of us will be to get a sound grasp of the fundamentals that belong just as much to Newtonian (slow-speed) dynamics. Making a thorough job of that would fill more pages than you would care to read (or pay for). So I'll make the best compromise I can between full explanation, a bit of fudging and a bit of ‘it can be proved that’. (If you're not interested in the dynamics, you can skip to Chapter 20, provided you can do without the mathematical practice that we'll get on the way.)

We all know that if something is stationary, you need a force to get it moving; and if it's moving, you need a force to stop it. We also know that some things are easier to get moving or to stop than others. A moderate push will get a car going. But try it on a bus! Things vary in the extent to which they resist being speeded up or slewed down. Mass is a quantity that gives a measure to this resistance – though we shall have to work out a more precise statement of this vaguely conceived idea.

(If you have been taught that mass measures the ‘quantity of matter’, please forget it. Also don't confuse mass with weight.

In the region around the Sun there's only one other test to which we can subject our theory–we can ask how well it does in predicting the motion of a planet. Newtonian theory says that the orbit is an ellipse, and observation over the centuries has confirmed that this must be very near the truth. So we shall have to study some properties of ellipses.

If you're already well up in the subject, you may find it good enough to (1) note the definitions of the quantities, as summarised in Figure 31.2; (2) check that (31.7) is an old friend, lightly disguised by writing x/r instead of cos φ (3) check that you know how to derive (31.12) from (31.7), and that you understand its significance; (4) check (as in §31.12 or by geometry) that the extreme values of r are given by (31.17); and (5) make sure you are familiar with (31.22) as a way of putting δ (sin φ) ∼ cos φδφ.

You probably know a practical recipe for drawing an ellipse. The ends of a piece of string are fixed to two pins stuck in a sheet of paper; if a pencil point (always in contact with the paper) is moved so that it keeps the string constantly taut, then it will draw an ellipse. To formalise that a little, we confine ourselves to a plane in which we have chosen two points S and S' (replacing the pins).

Constant gravity exists only as an approximation that does well enough in small regions of space. And on this small scale the only case where Einstein's theory gives a detectably different prediction from Newton's is that of §§23.14–16. For further tests we have to consider vast spaces in which gravity obviously varies from place to place. And to cope with these more complex conditions we shall have to modify two of our most basic assumptions.

Our most fundamental assumption of all–Einstein's Principle of Relativity (§5.11)–involves the explicit condition ‘In the absence of gravity …’. In constant gravity conditions would it still be true that all inertial observers are equivalent?

Yes–since the inertial observers in this case are exactly like those of the no-gravity case, but observed by an accelerated observer (§§23.6, 23.12).

If, on the other hand, gravity varies from place to place, then this Principle is no longer true. For simplicity imagine that the Earth is the only massive body in the Universe. Then (ii) and (iv) of §23.5 are inertial observers, one at the Earth's surface, the other very very far away in space. Our demonstration (§23.6) that these have identical experiences only worked because we confined our observers to small rooms. If we let them watch things moving inertially a few thousand miles away, will their experiences be the same?

No. As (ii) sees it, such things will have accelerations of different sizes in different directions (depending on position relative to the Earth's centre). But (iv) will detect no deviation from motion in a straight line at constant speed.

It's time to attempt some sort of summing up. We've left the Special Theory so far behind that I'm not going to return to it now. Anyhow, since it's so generally acknowledged as a well-established theory that lies at the roots of so much of today's scientific thought, what is there to discuss? The General Theory is a more interesting topic–still subject to active controversy.

Let's begin with a limitation. It never lived up to its title, with the suggestion of a great all-round generalisation of the Special Theory. It turns out, as I said in the Introduction, to be only a theory of gravitation, and as such we must judge it. So let's start by comparing Einstein's theory of gravitation with Newton's at a philosophical level. You'll know by this time where my preference lies.

Please reread §§26.46–7. There we have one reason for preferring Einstein's outlook: at the most basic level it involves one assumption fewer than Newton's. And so (although technically more complicated) it is simpler in principle. And most of us would agree (though it's hard to say precisely why) that simple explanations are philosophically preferable to complicated ones.

We can't, of course, blame Newton for being more complicated–the Einstein approach was inconceivable in his time. But we can note what caused him to be so. And that is simply that his theory begins by saying, in essence, ‘If there were no gravity’, things would behave in such and such a way. That's unsatisfactory, because you can never find true no-gravity conditions in which to test its truth.

Another book on Relativity for the layman! Why? What's different about it?

There have been many books on Einstein's theory, written by authors who are highly expert in this field and who have gone to an immense amount of trouble to explain it with great logical clarity, yet in simple terms that should be comprehensible to any reasonably intelligent person even if he has had no scientific education. And still these books have left most of their readers bewildered. Why? After discussions with dozens of students I think I can answer that question. The difficulties that really trouble the layman are not those which you would logically expect. The Relativity expert, no matter how diligent and sympathetic, is unlikely to discover these difficulties, even more unlikely to know how to cope with them.

I am definitely not one of these Relativity experts. What I know of the subject has been learnt laboriously from their works. But I think I can claim to be an expert in something different–in the art of teaching science to the non-scientist. That has been my job since 1950.

I introduced Relativity amongst my courses in 1958. And since then I have been teaching it to carpenters and clerks, housewives, miners and insurance agents–to all sorts of people who have no special qualifications for learning the subject (and others like teachers and professional engineers who have limited qualifications). At first I taught it badly. But the customs of the Adult Education world enabled me to learn by my mistakes.

Suppose that W–the observer of the previous chapter moving with constant acceleration – watches any inertial observers that may be around. How will their motion appear to him?

Think, for example, about several cars moving at various steady speeds along a straight road, and about what their motion would look like when observed from another car that has constant acceleration. I think you'll conclude that the distance between W and any inertial observer E is changing in a constantly accelerated manner, and that therefore

(A possible worry: maybe it won't work out quite like that–because E and W don't agree about times and distances. Actually if you do the calculations, based on our Chapter 22 near-equations, you discover that the statement is only strictly true if E is near to W and moving slowly relatively to him–both conditions to be interpreted in an asaccurately-as-we-wish sense. But that's good enough for us, since we'll only want to use this proposition in nearby, slow-speed conditions.)

Maybe you protested that W knows (by the particle test) that he is accelerated, and so he can't regard himself as stationary. But do you know of any circumstances in which an observer's test particle runs away and yet he insists that he's at rest?

Your test particle accelerates rapidly away from you (cf. §5.4). Yet you have no difficulty in thinking of yourself as stationary.