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Section7.3Hyperbolic Geometry with Curvature \(k \lt 0\)

We may do the same gentle scaling of the Poincaré model of hyperbolic geometry as we did in the previous section to the disk model of elliptic geometry. In particular, for each negative number \(k \lt 0\) we construct a model for hyperbolic geometry with curvature \(k\text{.}\)

We define the space \(\mathbb{D}_k\) to be the open disk of radius \(1/\sqrt{|k|}\) centered at the origin in \(\mathbb{C}\text{.}\) That is, \(\mathbb{D}_k\) consists of all \(z\) in \(\mathbb{C}\) such that \(|z| \lt 1/\sqrt{|k|}\text{.}\) In this setting, the circle at infinity is the boundary circle \(|z| = 1/\sqrt{|k|}\text{.}\)

The group \({\cal H}_k\) consists of all Möbius transformations that send \(\mathbb{D}_k\) to itself. The geometry \((\mathbb{D}_k,{\cal H}_k)\) with \(k \lt 0\) is called hyperbolic geometry with curvature \(k\text{.}\) Pushing analogy with the elliptic case, we may define the group of transformations to consist of all Möbius transformations with this property: if \(z\) and \(z^*\) are symmetric with respect to the circle at infinity then \(T(z)\) and \(T(z^*)\) are also symmetric with respect to the circle at infinity. Noting that the point symmetric to \(z\) with respect to this circle is \(\displaystyle z^* = \frac{1}{|k|\overline{z}} = -\frac{1}{k\overline{z}}\text{,}\) we draw the satisfying conclusion that \(T \in {\cal H}_k\) if and only if the following holds: \begin{equation*} \text{if}~z^* = -\frac{1}{k\overline{z}}~~ \text{then}~~ T(z^*) = -\frac{1}{k\overline{T(z)}}. \end{equation*}

Thus, the group \({\cal H}_k\) in the hyperbolic case has been defined precisely as the group \({\cal S}_k\) in the elliptic case. Furthermore, one can show that transformations in \({\cal H}_k\) have the form \begin{equation*} T(z) = e^{i\theta}\frac{z-z_0}{1+k\overline{z_0}z}, \end{equation*} where \(z_0\) is a point in \(\mathbb{D}_k\text{.}\)

Straight lines in this geometry are the clines in \(\mathbb{C}^+\) orthogonal to the circle at infinity. By Theorem 3.2.8, a straight line in \((\mathbb{D}_k,{\cal H}_k)\) is precisely a cline with the property that if it goes through \(z\) then it goes through its symmetric point \(\frac{-1}{k\overline{z}}\text{.}\)

The arc-length and area formulas also get tweaked by the scale factor, and now look identical to the formulas for elliptic geometry with curvature \(k\text{.}\)

The arc-length of a smooth curve \(\vec{r}\) in \(\mathbb{D}_k\) is \begin{equation*} {\cal L}(\vec{r}) = \int_a^b \frac{2|\vec{r}\hskip.04in^\prime(t)|}{1 + k|\vec{r}(t)|^2}~dt. \end{equation*}

The area of a region \(R\) given in polar coordinates is computed by the formula \begin{equation*} A(R) = \iint_R \frac{4r}{(1+kr^2)^2}dr d\theta. \end{equation*}

As in Chapter 5 when \(k\) was fixed at -1, the area formula is a bear to use, and one may convert to an upper half-plane model to determine the area of a \(\frac{2}{3}\)-ideal triangle in \(\mathbb{D}_k\text{.}\) The ambitious reader might follow the methods of Section 5.5 to show that the area of a \(\frac{2}{3}\)-ideal triangle in \((\mathbb{D}_k,{\cal H}_k)\) (\(k \lt 0\)) with interior angle \(\alpha\) is \(-\frac{1}{k}(\pi - \alpha)\text{.}\)

With this formula in hand, we can derive the area of any triangle in \(\mathbb{D}_k\) in terms of its angles, exactly as we did in Chapter 5.

SubsectionObserving negative curvature

Suppose we are located at a point \(z\) in a hyperbolic universe with curvature \(k\text{.}\) We see in the distance a hyperbolic line \(L\) that seems to extend indefinitely. We might intuitively see the point \(w\) on the line that is closest to us, as suggested in Figure 7.3.2. Now suppose we look down the road a bit to a point \(v\text{.}\) If \(v\) is close to \(w\) the angle \(\angle vzw\) will be close to 0. As \(v\) gets further and further away from \(w\text{,}\) the angle will grow, getting closer and closer to the angle \(\theta = \angle uzw\text{,}\) where \(u\) is an ideal point of the line \(L\text{.}\)

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Figure7.3.2The angle of parallelism \(\theta\) of a point \(z\) to a line \(L\text{.}\)

A curious fact about hyperbolic geometry is that this angle \(\theta\text{,}\) which is called the angle of parallelism of \(\boldsymbol{z}\) to \(\boldsymbol{L}\), is a function of \(z\)'s distance \(d\) to \(L\text{.}\) In Section 5.4 we saw that \(\cosh(d) = 1/\sin(\theta)\) in \((\mathbb{D},{\cal H})\text{.}\) In particular, one may deduce the distance \(d\) to the line \(L\) by computing \(\theta\text{.}\) The formula relating \(\theta\) and \(d\) is called Lobatchevsky's formula. No such analogy exists in Euclidean geometry. In a Euclidean world, if one looks farther and farther down the line \(L\text{,}\) the angle will approach 90\(^\circ\text{,}\) no matter one's distance \(d\) from the line.

Parallax

If a star is relatively close to the Earth, then as the Earth moves in its annual orbit around the Sun, the star will appear to move relative to the backdrop of the more distant stars. In the idealized picture that follows, \(e_1\) and \(e_2\) denote the Earth's position at opposite points of its orbit, and the star \(s\) is orthogonal to the plane of the Earth's orbit. The angle \(p\) is called the parallax, and in a Euclidean universe, \(p\) determines the star's distance from the Sun, \(D\text{,}\) by the equation \(D = d/\tan(p)\text{,}\) where \(d\) is the Earth's distance from the Sun.

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We may determine \(p\) by observation, and \(d\) is the radius of Earth's orbit around the Sun (\(d\) is about 8.3 light-minutes.) In practice, \(p\) is quite small, so a working formula is \(D = \frac{d}{p}\text{.}\) The first accurate measurement of parallax was recorded in 1837 by Friedrich Bessel (1784-1846) . He found the stellar parallax of 0.3 arc seconds (1 arc second = 1/3600\(^\circ\)) for star 61 Cygni, which put the star at about 10.5 light-years away.

If we live in a hyperbolic universe with curvature \(k\text{,}\) a detected parallax puts a bound on how curved the universe can be. Consider Figure 7.3.5. As before, \(e_1\) and \(e_2\) represent the position of the Earth at opposite points of its orbit, so that the distance between them is \(2d\text{,}\) or about 16.6 light-minutes. Assume star \(s\) is on the positive real axis and we have detected a parallax \(p\text{,}\) so that angle \(\angle e_1se_2 = 2p\text{.}\)

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Figure7.3.5A detected parallax in a hyperbolic universe puts a bound on its curvature

The angle \(\alpha = \angle e_1e_2s\) in Figure 7.3.5 is less than the angle of parallelism \(\theta = \angle e_1e_2u\text{.}\) Noting that \(\tan(x)\) is an increasing function and applying Theorem 7.3.3 it follows that \begin{equation*} \tan(\alpha/2) \lt \tan(\theta/2) = e^{-\sqrt{|k|}2d}. \end{equation*}

We may solve this inequality for \(|k|\text{:}\) \begin{align*} \tan(\alpha/2) \amp \lt e^{-\sqrt{|k|}2d} \amp \\ \ln(\tan(\alpha/2)) \amp \lt -\sqrt{|k|}2d \amp \ln(x) ~\text{is increasing}\\ \bigg[ \frac{\ln(\tan(\alpha/2))}{2d}\bigg]^2 \amp > |k|\amp x^2.~ \text{is decreasing for}~x\lt 0 \end{align*}

To get a bound for \(|k|\) in terms of \(p\text{,}\) note that \(\alpha \approx \pi/2 - 2p\) (the triangles used in stellar parallax have no detectable angular deviation from 180\(^\circ\)), so \begin{equation*} |k| \lt \bigg[ \frac{\ln(\tan(\pi/4-p))}{2d}\bigg]^2. \end{equation*}

We remark that for values of \(p\) near 0, the expression \(\ln(\tan(\pi/4-p))\) has linear approximation equal to \(-2p\text{,}\) so a working bound for \(k\text{,}\) which appeared in Schwarzschild's 1900 paper [27], is \(|k| \lt (p/d)^2\text{.}\)

SubsectionExercises

1

Prove that for \(k \lt 0\text{,}\) any transformation in \({\cal H}_k\) has the form \begin{equation*} T(z) = e^{i\theta}\frac{z-z_0}{1+k\overline{z_0}z}, \end{equation*} where \(\theta\) is any real number and \(z_0\) is a point in \(\mathbb{D}_k\text{.}\) Hint: Follow the derivation of the transformations in \({\cal H}\) found in Chapter 5.

2

Assume \(k \lt 0\) and let \(s = 1/\sqrt{|k|}\text{.}\) Derive the following measurement formulas in \((\mathbb{D}_k,{\cal H}_k)\text{.}\)

a. The length of a line segment from \(0\) to \(x\text{,}\) where \(0 \lt x \lt s\) is \begin{equation*} d_{k}(0,x) = s\ln\bigg(\frac{s+x}{s-x}\bigg). \end{equation*} Hint: Evaluate the integral by partial fractions.

b. The circumference of the circle centered at the origin with hyperbolic radius \(r\) is \(c=2\pi s\sinh(r/s).\)

c. The area of the circle centered at the origin with hyperbolic radius \(r\) is \(A = 4\pi s^2 \sinh^2(\frac{r}{2s})\text{.}\)

3

Let's investigate the idea that the hyperbolic formulas in Exercise 7.3.2 for distance, circumference, and area approach Euclidean formulas when \(k \to 0^-\text{.}\)

a. Show that the hyperbolic distance \(d_{k}(0,x)\) from 0 to \(x\text{,}\) where \(0 \lt x \lt s,\) approaches \(2x\) as \(k \to 0^-\text{.}\)

b. Show that the hyperbolic circumference of a circle with hyperbolic radius \(r\) approaches \(2\pi r\) as \(k \to 0^-\text{.}\)

c. Show that the hyperbolic area of this circle approaches \(\pi r^2\) as \(k \to 0^-\text{.}\)

4

Triangle trigonometry in \((\mathbb{D}_k,{\cal H}_k)\text{.}\)

Suppose we have a triangle in \((\mathbb{D}_k,{\cal H}_k)\) with side lengths \(a,b,c\) and angles \(\alpha, \beta,\) and \(\gamma\) as pictured in Figure 5.4.12.

a. Prove the hyperbolic law of cosines in \((\mathbb{D}_k,{\cal H}_k)\text{:}\) \begin{equation*} \cosh(\sqrt{|k|}c)=\cosh(\sqrt{|k|}a)\cosh(\sqrt{|k|}b)-\sinh(\sqrt{|k|}a)\sinh(\sqrt{|k|}b)\cos(\gamma). \end{equation*} b. Prove the hyperbolic law of sines in \((\mathbb{D}_k,{\cal H}_k)\text{:}\) \begin{equation*} \frac{\sinh(\sqrt{|k|}a)}{\sin(\alpha)}=\frac{\sinh(\sqrt{|k|}b)}{\sin(\beta)}=\frac{\sinh(\sqrt{|k|}c)}{\sin(\gamma)}. \end{equation*}

5

As \(k \lt 0\) approaches 0, the the formulas of hyperbolic geoemtry \((\mathbb{D}_k,{\cal H}_k)\) approach those of Euclidean geometry. What happens to Lobatchevsky's formula as \(k\) approaches 0? What must be the angle of parallelism \(\theta\) in the limiting case? Is this value of \(\theta\) independent of \(d\text{?}\)

6

Bessel determined a parallax of \(p = .3\) arcseconds for the star 61 Cygni. Convert this angle to radians and use it to estimate a bound for the curvature constant \(k\) if the universe is hyperbolic. The units for this bound should be light years\(^{-2}\) (convert the units for the Earth-Sun distance to light-years).

7

The smallest detectable parallax is determined by the resolving power of our best telescopes. Search the web to find the smallest detected parallax to date, and use it to estimate a bound on \(k\) if the universe is hyperbolic.