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Set Theory Jottings 30. Definability Tools

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Definability Tools

We will need some familiarity with the the “definability powers” of Peano arithmetic. Without giving an exhaustive treatment, here are some of the highlights.

Recursive Tupling Functions

We have a 1–1 correspondence ℕ×ℕ→ℕ. Lots of them! We’ll pick one in a moment; we’ll denote it by

(x,y)↦〈x,y

Here (x,y)∈ℕ×ℕ is an ordered pair, and 〈x,y〉∈ℕ is the number coding it.

We want 〈·,·〉 to be arithmetically definable. The following formula does the trick:

x,y〉= ½(x+y)(x+y+1)+y

It’s easy to see where it comes from. If you list the lattice points in ℕ×ℕ by “cross diagonals” (i.e., (0,0), (1,0), (0,1), (1,1), …), then the predecessors of (x,y) consist of a triangle, plus a “tail” lying along the diagonal. Count them up! You get the above formula. So 〈·,·〉 is not just arithmetic, but recursive.

You can iterate this to get recursive k-tupling correspondences ℕk→ℕ for every k. For example,

x,y,z〉= 〈〈x,y〉, z

The tupling functions allow us to translate formulas like this:

x1x2y1y2

into this:

xy

Using the tupling functions, we can extend the notions of arithmetic and hyperarithmetic to n-ary relations and functions. For relations this is obvious. For a function, we look at its graph: f() is arithmetic (respectively hyperarithmetic) if the relation f()=y is.

Our definition of ℒ2(PA) allowed quantification over set variables. Sometimes there are technical advantages to using function variables instead. These can be “translated away” in a mechanical fashion. Admittedly the details can get a little hairy; for example, try expressing ∀x f(g(x))=g(f(x)) using the relations φf(x,y) ≡ f(x)=y and φg(x,y) ≡ g(x)=y. I will use both freely in ℒ2(PA).

Recursion

Recursion is a basic tool. Here’s the simplest form. Suppose we have a function f:ℕ→ℕ, and let a be any number. Define F by

F(0) = a
F(n+1) = f(F(n))

If f is arithmetic (or hyperarithmetic), does that make F arithmetic (hyperarithmetic)? Here are two ways we can write a formula for F(x)=y, provided we can quantify over arbitrary finite sequences a0,…,ax:

F(x)=y (∃a0,…,ax)[
a0=a
∧ (∀z<x)(az+1=f(az))
y=ax]

and

F(x)=y (∀a0,…,ax)[
a0=a
∧ (∀z<x)(az+1=f(az))
y=ax]

So we have a choice of ∃ or ∀, good news for the hyperarithmetic case. We’ll see soon how to handle arbitrary finite sequences in PA.

More complicated forms of recursion? No problem. For example, say f(x,ȳ,z) is a function of n+2 variables and g(ȳ) of n variables. Define

F(0,ȳ) = g(ȳ)
F(n+1,ȳ) = f(F(n,ȳ),ȳ,n)

So we’re allowing the new value to depend on a bunch of parameters ȳ, on the argument n, and of course on the previous value F(n,ȳ). This scheme is called primitive recursion. It’s handled the same way as the simpler case.

With this in our toolbox, we can define any so-called primitive recursive function. That’s any function you get by starting with a few very basic ones (projection, constant functions, successor) and applying composition and primitive recursion as many times as you like. So-called “course of values” recursions, where the new value depends on all values previously computed, also are available, since we can code the list of previous values using the finite sequence technique (see below). Sets and relations can be coded via functions taking the values 0 and 1; then we can use such relations in boolean conditionals (or more generally “definition by cases”) when defining new functions.

Loosely speaking, primitive recursive functions coincide with the computable functions where you can “clearly see” that the computations always terminate. To get the full panoply of recursive functions, we add the so-called μ-operator. This defines a partial function y, like so:

μy(φ(y,)) = the least y such that φ(y,)
undefined if there is no such y

It’s easy to express this in the language of PA:

μy(φ(y,))=u ≡ φ(u,)∧(∀z<u)¬φ(z,)

Any function defined by applying the μ-operator to a primitive recursive relation is a partial recursive function. If a partial recursive function just happens to be total, it’s a recursive function. But we can’t (computably) tell in general if a partial recursive function is total—that’s the Halting Problem on steroids.

The “sequence trick” (see below) and the μ-operator together tell us that any partial recursive function is arithmetic. (That is, its graph is an arithmetic relation.) But these techniques go beyond this: if f and g are arithmetic or hyperarithmetic, then so is the F defined by the primitive recursion scheme or the μ-operator, even if f and g are horribly, hideously uncomputable.

Finite Sequences

As we’ve just seen, we need a way to code finite sequences of arbitrary length as single numbers. Gödel gave one technique: code (r1,…,rk) as p1r1···pkrk, where pi is the i-th prime. But this works only once we have a definition of exponentiation, and of the function ipi. Both these yield easily to recursion, but that requires a coding of finite sequences!

Gödel broke the vicious circle with the Chinese remainder theorem. This says that given any sequence of positive integers d1,…,dk, all pairwise coprime, and any sequence r1,…,rk with 0≤ri<di for i=1,…,k, there is an a such that a%di=ri for all i. Here % is the remainder function. We call the di’s divisors and the ri’s remainders.

The Chinese remainder theorem is actually stronger: it says that there is a unique such a satisfying 0≤a<d1···dk. Although we won’t need the stronger version, it falls right out of the easiest proof of the theorem. Let d=d1···dk. Write [d] for the set {0,…,d−1}, likewise for [di]. We have a mapping [d]→[d1]×…×[dk] defined by a↦(a%d1,…,a%dk). The mapping is injective because the di’s are pairwise coprime: if a%di=a′ %di for all i, then di|(aa′) for all i and so d|(aa′). Since the domain and codomain both have d elements, the mapping is surjective. qed.

So if we are given a finite sequence (r1,…,rk), we just have to find divisors di such that they are pairwise coprime and ri<di for all i. The sequence of divisors has to be “orderly”, in the sense that if we had to specify all the di’s individually, we wouldn’t have gained anything. Gödel chose the arithmetic progression di=bi+1, for a suitable b. It turns out that b works if it is a sufficiently large multiple of k!.

How do we use this to handle a quantifier like ∃(r1,…,rk)? Answer: first we define

β(a,b,i) = a%(bi+1)

Formally representing the remainder function is a piece of cake. Then

∃(r1,…,rk)…ri

is equivalent to

ba…β(a,b,i)…

I’ve been a bit sloppy with notation. The ∃ba causes no hiccups. I did not write ∃(r1,…,rk)φ(r1,…,rk). That would suggest a concrete list of k variables. But we want the subscript i in ri to be variable as well. Gödel’s β function makes that possible. We’ll see an example next.

Bitstrings

Forcing in arithmetic uses bitstrings. First, we will regard a subset A⊆ℕ as an infinite bitstring, or equivalently, a function A:ℕ→{0,1}. Second, finite bitstrings will play the role of conditions: if p is a condition (i.e., finite bitstring) and an initial segment of A matches p, then we say A satisfies p. If the condition q extends p (or equals it), we write pq.

Suppose we have a sequence p0p1≤…, defined inductively, starting with an arbitrary condition p0=c. In other words, we have a function f:ℕ×CC, where C is the set of conditions, and for all n∈ℕ, pn+1=f(n,pn). Let A=⋃pn; if the pn’s stop growing at some point (i.e., for some n0, we have pn=pn0 for all nn0), then we make the rest of A all 0’s after that (i.e., nA for all n past the end of pn0). Question: if f is arithmetic, or implicitly defined, or hyperarithmetic, can we say the same for A?

First, how do we code conditions? Using binary notation doesn’t quite do the trick: consider 0001 vs. 01, for example. Pairing a binary number with its length works: 〈k,b〉 where k is the length of the bitstring, and b is the bitstring in binary, padded out with leading 0’s if necessary.

A sketch of the formula ψS that represents xS:

ψS(x)≡ (∃ p0,…,pl)[
p0=c
∧ (∀n<l)[pn+1=f(n,pn)]
xpl]

Let’s look at the individual pieces:

  • (∃ p0,…,pl): we make use of Gödel’s β function. Also, all the pn’s are conditions; we have to make this explicit. I omit details.
  • p0=c: c will be a constant, incorporated into our formula.
  • pn+1=f(n,pn): see below.
  • xpl: i.e., bit x in pl is 1. This translates into a statement about the size of a remainder: b has a 1 in position x iff b=2x+1·q+r with 2xr<2x+1.

Now, how about pn+1=f(n,pn), or in general, w=f(u,v)? If f is an arithmetic function, defined by a formula φ(w,u,v), then we just transcribe φ into our definition ψS(x) for A. So if f is arithmetic, then so is A. (Because of c, we have a definition of A for each initial condition c, with A satisfying c.)

Next, say f is implicitly defined, say by φF; F is a new function symbol added to ℒ(PA). (So φF is a closed formula of ℒ(PA+F).) Transcribing φF into the sketch above gives us a “paired” implicit definition. That is, {(f,A)} is definable by a closed formula in ℒ(PA+F+S), where we’ve added two new symbols. As you can imagine, it’s easy to combine f and A into a single function (or set), but that’s not the same as having an implicit definition for A by itself.

Finally, if f is hyperarithmetic, then so is A. We transcribe the Σ11 or the Π11 formula for f into the sketch, getting a formula ψ(x) in ℒ2(PA). The function (or set) quantifier can be migrated to the front, using basic facts of logic. So we have a Σ11 and a Π11 formula defining A.

Summary: if f is arithmetic, so is A; if f is hyperarithmetic, so is A; but if f is implicitly defined, then the best we can do is a paired implicit definition of A with f.

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Set Theory Jottings 29. Definability

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Three Kinds of Definability

A⊆ℕ is arithmetic if there is a formula φ(x) in ℒ(PA) such that

For all n [nA if and only if ℕ⊧φ(n)]

Tarski’s undefinability theorem says that truth in ℕ is not arithmetic: the set of Gödel numbers of sentences of ℒ(PA) that hold in ℕ is not an arithmetic set. Using the Quine bracket notation where ⌜ψ⌝ is the Gödel number of ψ, we can say: there is no φ(x)∈ℒ(PA) such that for all closed ψ∈ℒ(PA),

ℕ⊧ψ if and only if ℕ⊧φ(⌜ψ⌝)

On the other hand, Tarski gave a recursive definition of satisfaction for first-order logic: if ℒ is a language and M is a structure for ℒ, then M⊧φ∧ψ if and only if M⊧φ and M⊧ψ, etc. We can formalize this for Peano arithmetic by adding a new predicate letter, say T, to ℒ(PA). I’ll write ℒ(PA+T) for this language. We can now express Tarski’s recursive definition this way:

T(⌜ψ⌝) ↔
⌜ψ⌝ = ⌜s=t⌝ ∧ s and t are closed terms with equal values
∨ ⌜ψ⌝ = ⌜¬α⌝ ∧ ¬T(⌜α⌝)
∨ ⌜ψ⌝ = ⌜α∧β⌝ ∧ T(⌜α⌝) ∧ T(⌜β⌝)
∨ ⌜ψ⌝ = ⌜∃x φ(x)⌝ ∧ ∃n T(⌜φ(n)⌝)

This is the outline of a sentence in ℒ(PA+T). With a large but bounded amount of work, it can be translated completely into the formal language. I will only hint at why this is true—a convincing explanation would take many pages. You can find that in many textbooks, and my  Logic Notes also have a bit to say. Anyway: one can show that Peano arithmetic can represent any recursive function. It follows that PA can handle all purely syntactical matters. For example, “n is a Gödel number”; or “n is the Gödel number of a formula of the form α∧β, and k is the Gödel number of α and l is the Gödel number of β’’; or “s is the Gödel number of a closed term whose value is v.”

Say A⊆ℕ. (ℕ,+,·,<,A) (or (ℕ,A) for short) is a structure for ℒ(PA+T), if we interpret T(n) as meaning nA. Then our sentence holds in (ℕ,A) precisely when A is the set of Gödel numbers of true sentences ψ of ℒ(PA).

I generalize. Write ℒ(PA+S) for ℒ(PA) augmented with a new predicate letter S. (ℕ,A) is a structure for ℒ(PA+S), using A to interpret S. Say we have a class 𝒜 of subsets of ℕ, and a closed formula ψS in ℒ(PA+S). Suppose that

For all A⊆ℕ [A∈𝒜 if and only if (ℕ,A)⊧ψS]

Then we say that 𝒜 is an arithmetic class.

For example, consider the formula

ψS ≡ ∀x (S(x)→S(x·x))

In other words, (ℕ,A)⊧ψS means that A is closed under squaring. The class 𝒜 determined by ψS contains many sets: the set of all squares, the set of all powers of a prime p, the set of numbers whose prime factors all belong to a fixed set of primes, etc.

If {A} is an arithmetic class, then we say that A is implicitly definable by the formula ψS defining its singleton class. So truth in ℕ is implicitly definable.

Observe that any arithmetic set is implicitly definable: just let ψS be ∀x[S(x)↔φ(x)], where φ(x) is the formula in ℒ(PA) defining the arithmetic set.

The class of arithmetic sets enjoys some nice properties: it is closed under intersection, union, and complement. This falls out just from using the logical connectives. The existential quantifier gives us another operation, projection. Let 〈y,z〉 be a recursive pairing function, that is, a recursive bijection from ℕ×ℕ to ℕ. If A is defined by φ(x), then the formula ∃y φ(〈y,z〉) defines the projection of the relation 〈y,z〉∈A onto its second coordinate. (If this relation is a function, then the projection is its range. Likewise, if the relation is a partial function, we can project on the first coordinate to find its domain.)

The class of arithmetic sets is precisely the smallest class of subsets of ℕ closed under intersection, union, complement, projection, and containing the singletons {0} and {1} and the graphs of the addition and multiplication operations. (Take a moment to see why this is true.)

As we will see later, the class of implicitly definable sets is less tidy. For one thing, it’s not closed under intersection.

We recover some of the nice features by passing to a yet more inclusive class, the hyperarithmetic sets. First we expand our language to so-called second-order arithmetic: instead of adding a new predicate letter, we allow variables ranging over subsets of ℕ. Quantification is allowed. I will use capital letters for subsets and lowercase for numbers1. I’ll write S(x) and xS to mean the same thing; you can decide which is vernacular. I’ll write ℒ2(PA) for second-order arithmetic.

Suppose A is implicitly definable via a formula ψS in ℒ(PA+S). Then A is definable in ℒ2(PA) in two ways, existentially:

S SxS)

and universally:

S SxS)

since in both forms, the clause “ψS’’ guarantees that S is the set A. Note that each formula has a sole free number variable, x.

A formula in ℒ2(PA) is called a Σ11 formula if it has an existential set quantifier out in front, no universal set quantifiers, and as many number quantifiers as your heart desires. Likewise, a Π11 has a universal set quantifier out front, no existential set quantifiers, and as many number quantifiers as needed. Thus:

Σ11: S ψ(S,x)
Π11: S ψ(S,x)

where ψ(S,x) can contain number quantifiers in abundance, but no other set quantifiers.

A set is hyperarithmetic or Δ11 if it possesses both a Σ11 and a Π11 definition. (That is, Σ11 and a Π11 formulas with one free number variable, but no other free variables.)

An example: the set of even numbers, arithmetically defined by a formula φ(x)∈ℒ(PA), implicitly defined by a formula Φ(S)∈ℒ(PA+S), and hyperarithmetically defined by formulas α(u)∈Π11 and ε(u)∈Σ11.

Arithmetic definition: φ(x) ≡ ∃y (y+y=x)

Implicit definition: Φ(S) ≡ ∀x (S(x)↔∃y(y+y=x))

Π11 definition: α(u) ≡ ∀S [∀x(S(x)↔∃y(y+y=x))→S(u)]

Σ11 definition: ε(u) ≡ ∃S [∀x(S(x)↔∃y(y+y=x))∧S(u)]

The pattern is clear:

Arithmetic definition: φ(x) ≡ ∃y (y+y=x)

Implicit definition: Φ(S) ≡ ∀x (S(x)↔φ(x))

Π11 definition: α(u) ≡ ∀S [Φ(S)→S(u)]

Σ11 definition: ε(u) ≡ ∃S [Φ(S)∧S(u)]

We see from this that every arithmetic set is implicitly definable, and every implicitly definable set is hyperarithmetic.

The set of Gödel numbers of true sentences in ℒ(PA) provides an example of an implicitly definable set that is not arithmetic, as we’ve just seen. Feferman’s theorem provides an example of a hyperarithmetic set that is not implicitly definable.

[1] So this is a two-sorted first-order language. Alternately, add predicates set and number, and treat ∃X… as vernacular for ∃x(set(x) ∧ …), etc.

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From Kepler to Ptolemy 26

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The Vicarious Hypothesis

Part II of the Astronomia nova bears the title “Imitation of the Ancients”. Kepler obtains a model for Mars with an eccentric circle and an equant. But the eccentricity is not bisected. Instead, the center is closer to the equant than to the sun. See the figure below. (Notation: S=Sun, C=Center, E=Equant, r=radius, eS=SC/r, and eE=EC/r.)

The Vicarious Model

As this post is a bit long, let me highlight the main points.

  • The general model has parameters eS and eE. We always have eS+eE=2e, where e is the eccentricity.
  • We get the best fit for heliocentric longitudes using the ratio eS:eE=5:3. This is quite close to Kepler’s vicarious hypothesis.
  • We get the best fit for latitudes and “off to the side” observations with eS=eE, the famous “bisection of eccentricity”. It’s longitudes or latitudes, you can’t have both! At least with a circular orbit.
  • Kepler determined the parameters for his vicarious hypothesis by an intricate double iteration, using four acronychal observations.
  • The whirlpool force hypothesis requires bisection of eccentricity.
  • Although Kepler ultimately rejected the vicarious hypothesis as the correct model, he continued to use it to compute heliocentric longitudes. This is an implicit appeal to his “zeroth law”.

A Modern Perspective

I will refer to the scheme of the figure above as the vicarious model; Kepler used this term for a particular choice of parameters. By the “elliptical model”, I mean the usual elliptical orbit with the planet obeying the area speed law. I assume throughout that the period is the same for both models.

Before considering what Kepler wrote and did, we’ll examine the two models with modern techniques.

Suppose all we care about are heliocentric longitudes. We want to choose the parameters in the vicarious model to match these as accurately as possible. We don’t care about latitudes or distances. Observationally, this means we look only at acronychal measurements of the geocentric longitude. For as noted in post 24, when the planet is in opposition, the heliocentric and geocentric longitudes are equal.

What parameters will make the vicarious model best approximate the elliptical model for heliocentric longitudes? Evans and Linton (p.179) derive the answer: eS+eE=2e where e is the eccentricity of the ellipse, and eS:eE=5:3.

Evans obtains this result several ways. He imposes three conditions on the motion. Let P be perihelion, and Q quadrature (i.e., the point such that PSQ is a right angle). First condition: the time from perihelion P to Q must be the same for both models. To an excellent approximation when e is small, this implies that eS+eE=2e.

Second condition: the angular speed at aphelion must be the same for both models. This gives the equation

\frac{1-e_E}{1+e_S}=\frac{\sqrt{1-e^2}}{(1+e^2)^2};

retaining only terms up to order e2, this becomes

eS+eE = 2e+2eeS5/2e2

Third condition: the angular speed at perihelion must be the same for both models. By similar reasoning, we have

\frac{1+e_E}{1-e_S}=\frac{\sqrt{1-e^2}}{(1-e^2)^2};

approximated to

eS+eE = 2e−2eeS+5/2e2

So we have three equations: eS+eE=2e, and the aphelion and perihelion angular speed results. Any two of these equations yields eS:eE=5:3.

Evens gives another derivation, using an expression for the heliocentric longitude measured from perihelion as a function of time. (Linton gives essentially the same derivation, but using aphelion instead of perihelion.) Let this be θ, and let ω be the average angular speed, i.e., 2π/T. Up to second order in e, the expression is

θ(t) = ωt+2e sin ωt+5/4e2 sin 2ωt

for the elliptical model, and

θ(t) = ωt+(eS+eE) sin ωteS(eS+eE) sin 2ωt

for the vicarious model. So first: when eS+eE=2e, the expressions agree to first order in e. Second: when also eS:eE=5:3, we have eS=5/4e, and so they agree to second order.

In short, the vicarious model gives very good heliocentric longitudes when eS:eE=5:3. To quote Evans: “In fact, with the precision achievable with naked-eye observations even in Kepler’s day, there is no perceptible error in the angular position anywhere around the orbit—as Kepler himself verified.”

Okay, what if we do care about distances and latitudes? Geocentric latitudes provide a means to determine distances. I’ll explain this in more detail below, but intuitively: the closer you are to Mars, the bigger the latitude looks. An optical effect, just like approaching a vertical pole and seeing it look taller. Viewing Mars out of opposition, “from the side”, furnishes another way to check actual distances.

Perihelion and aphelion are minimal and maximal Sun-Mars distances, so a vicarious model that tries to do a good job with distances will share the apsidal line with the elliptical model. That means they will also have the same center and same r, where r is the vicarious radius and the elliptical semi-major axis. In the elliptical model, the Sun-Mars distance at aphelion is r+e and at perihelion is re. In the vicarious model, these distances are respectively r+eS and reS. Conclusion: the vicarious model gives the correct Sun-Mars distance at aphelion and/or perihelion only when eS=e. In other words, the eccentricity must be bisected.

The upshot: using the scheme of the above figure, you are faced with Scylla and Charybdis. You can have an excellent model for finding heliocentric longitudes at any time, all around the orbit. Just choose eS:eE=5:3. Or you can have a model for distances that is accurate at aphelion and perihelion. Choose eS=eE=e. You can’t have both.

One more observation: if we do bisect the eccentricity, then the two expressions for θ(t) will first disagree at order e2. That is, in the term with the factor sin 2ωt. The maximum (absolute) value occurs when 2ωt=±π/2. Since 2ω=4π/T, that means at tT/8. For small eccentricity, this is close to the octants.

What Kepler Did

After some preliminaries, Kepler gets down to business in Chapter 16 of the Astronomia nova. It takes four parameters to specify a vicarious model: the two eccentricities eS and eE, the direction of aphelion, and a time when the planet is at aphelion (known as the epoch). Kepler used four acronychal observations to derive the parameters.

Determining the Vicarious Parameters

The left of the figure above is Kepler’s diagram; the right side removes some clutter. A is the sun, B is the center of the orbit, and C is equant. D, E, F, and G are the four acronychal observations. They give us heliocentric longitudes: the directions of the lines AD, AE, AF, and AG. The directions from the equant (CD, CE, CF, and CG) are called mean longitudes. Since we know the times of the observations, we would know the mean longitudes if we knew the epoch and the direction of aphelion. That’s because the planet moves uniformly when viewed from the equant, and we know the period. Referring to the right side of the figure, you can see that we’d have two angles of the triangle AGC; of course, this also holds for the other three triangles. Temporarily chose the distance unit so that AC has length 1. Then we can solve all these triangles and find the positions D, E, F, and G.

Kepler imposed two constraints. First, the four acronychals must lie on a circle. This is easily checked, since a quadrilateral is cyclic if and only if opposite angles add to 180°. Also, the center B of the circle must lie on the line segment AC. If these are met, then we can determine both the radius and the center of the circle. That gives us the two parameters of the vicarious model, AB/r=eS and CB/r=eE.

Unfortunately, there is no direct way to find the epoch and direction of aphelion from the acronychals. Kepler proceeded iteratively. Starting with an estimate for these two quantities, he computed the positions DEFG. If these failed the circle requirement, he adjusted the direction of aphelion. “Repeat until done”, i.e., until DEFG lie on a circle. Gingerich (Ch.22) calls this the “inner iteration”. Then Kepler checked that B lay on the line segment from A to C. If not, he adjusted the epoch. This is the “outer iteration”, since the aphelion direction must now be recomputed. Eventually the process converged on values with both requirements satisfied. Kepler’s final result: eS:eE=18564:11332≈4.91:3.

Gingerich (Ch.22) and Voelkel (pp.106–107,111,114–121) present the whole messy story, based on Kepler’s copious manuscripts. In contrast to the account in the Astronomia nova, Kepler began in 1600 by tackling the earth’s orbit (i.e., revising Tycho’s solar theory). In the same year he made his first assault on the orbit of Mars. The two investigations continued in a tangled fashion, with interruptions, until sometime in 1602.

Downfall: Down but not Out

In Chapter 18, Kepler proclaims victory:

You see then, O studious reader, that the hypothesis found by the method developed above, is able in its calculations to account, in turn, for the four observations upon which it was founded, but also to comprehend all the other observations within two minutes…

And Chapter 19 begins:

Who would have thought it possible? This hypothesis so closely in agreement with the acronychal observations, is nonetheless false…

Chapters 19 and 20 then show, “with great thoroughness and almost masochistic delight” (Koestler (p.322)) that the vicarious hypothesis disagrees with geocentric latitudes and observations out of opposition.

Geocentric Latitude

We’ve already seen all the ingredients. First, latitudes. Consider the Sun-Earth-Mars triangle (see figure above). At opposition this lies in a plane perpendicular to the earth’s orbit (the ecliptic). The inclination of Mars’s orbital plane is the angle Earth-Sun-Mars. The geocentric latitude is the supplement of the angle Sun-Earth-Mars. If you know the Earth-Sun distance, then you can solve the triangle and get the Sun-Mars distance.

Kepler does this in Chapter 19, and concludes that the Martian eccentricity is between 0.08000 and 0.09943; his vicarious hypothesis sets it at 0.11332. He also notes that “combined eccentricity” (i.e., from the sun to the equant) is about 0.18564; half that is 0.9282, or just about the mean between 0.08000 and 0.09943.

Chapter 20 looks at some longitudes when Mars at perihelion and aphelion, but Earth is “off to the side”—that is, away from opposition. Again the results refute the vicarious model, and fit a bisected eccentricity rather well.

Puzzling. Kepler anticipates the resolution: “the orbit of the star is not a perfect circle, but an oval…”

Although the vicarious hypothesis failed, it still provides Martian longitudes to an accuracy of 2′. Kepler uses it for this purpose in subsequent chapters. In other words, Kepler assumes that if the earth were in opposition, instead of off to the side, then the vicarious longitudes would be correct.

Note the implicit appeal to the zeroth law: No special treatment for the earth. The solar longitude of Mars can’t depend on Earth’s position. Okay, but why prefer the acronychal (opposition) data to the off-to-the-side data?

Answer: the longitudes in question are the Sun-Mars directions. An acronychal observation directly measures this, since the Earth-Mars and Sun-Mars directions are identical. This doesn’t hold for an off-to-the-side measurement. So we should trust the acronychal values, and the vicarious hypothesis gives those values with good accuracy around the whole of Mars’s orbit.

Feetnote

(1) The Mars model by Longomontanus, mentioned in post 24, used a Copernican epicyclet instead an equant (see post 20). But we can convert it into a nearly equivalent equant model; Evans shows how to translate the parameters. Under this transformation, the Longomontanus model had eS:eE=5:3.

(2) Kepler complains in Chapter 16:

If this wearisome method has filled you with loathing, it should more properly fill you with compassion for me, as I have gone through it at least seventy times at the expense of a great deal of time, and you will cease to wonder that the fifth year has now gone by since I took up Mars, although the year 1603 was nearly all given over to optical investigations.

Gingerich (Ch.21) wondered why it took Kepler 70 iterations. He programmed it, and it took the computer only 9 trials! He guessed initially (and wrongly) that “Kepler was horribly plagued by numerical errors”. But when he gained access to Kepler’s manuscripts (Ch.22), he found two causes: bad data, and Kepler’s treatment of redundant observations. Gingerich writes:

Thus we see that in the vicarious orbit solution Kepler worked always with the same four oppositions, but the results were repeatedly tested against additional oppositions. In the course of five years’ work, the reduction of the basic data was continually improved. His 70 iterations were spent (probably) in five separate solutions differing only in the values chosen for the initial times and angles.

Gingerich also notes a fine point I glossed over in my account:

Tycho Brahe had no operational way of knowing precisely when Mars was at opposition. Tycho’s raw observations only approximated the opposition places, and Kepler was obliged to correct and interpolate them to obtain the acronychal positions he required.

(3) The whirlpool force explanation for the equant requires bisecting the eccentricity (see post 4 and post 20). So in considering the vicarious model at all, Kepler tempered his commitment to this hypothesis.

Voelkel (pp.107–111) found confirmation in a document Kepler wrote around 1602. We’ve noted how the inverse distance speed law works tolerably well within an orbit, but fails when comparing different orbits (see post 20). In the document, Kepler notices his earlier errors in this matter.Voelkel suggests that this realization freed Kepler to study other divisions of eccentricity. It must have come as a relief when the latitude and off-side computations indicated that eccentricity should be bisected.

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