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Normal and Geodesic Curvatures, As Well As Some Material About the Second Fundamental Form and the Christoffel Symbols

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Normal and Geodesic Curvatures, As Well As Some Material About the Second Fundamental Form and the Christoffel Symbols Math 120A Discussion Session Week 6 Notes February 14, 2019 This week we'll repeat some of what you heard in lecture about normal and geodesic curvatures, as well as some material about the second fundamental form and the Christoffel symbols. Normal and geodesic curvatures 3 Earlier in the quarter we spent some time defining the curvature κ of a curve in R and then the 2 planar curvature k of a curve in R . The planar curvature allowed us to extract a little more information than the original curvature. For instance, by integrating the planar curvature over a 2 closed curve in R we were able to obtain a topological invariant, the rotation index. The reason we were able to make sense of planar curvature is that in two dimensions we can choose a preferred normal vector for our curves. Specifically, if t(s) was the unit tangent vector to α at α(s) then the unit normal vector was obtained by rotating t(s) 90◦ counterclockwise. 3 Now suppose x: U! R parametrizes a patch on a surface S. So x produces coordinates on S, allowing us to (locally) treat S as the two-dimensional object that it is. In particular, we can use x to choose a preferred normal vector for curves in S. The parametrization x gives us a unit normal vector n(u; v) to our surface S. Let α(s) be a unit-speed curve in S, and let fT; N; Bg be its Frenet-Serret frame. Now consider the vector S(s) := n(α(s)) × T(s): This vector is perpendicular to n | thus tangent to S | and perpendicular to T. So S(s) is a 2 normal vector to α as it would be seen by an inhabitant of S. Just as in the case of R , we have a preferred normal vector for our curves. In order to define curvature as it would be experienced by an inhabitant of our surface we should recall the definition of planar curvature. Planar curvature measures the extent to which our unit tangent vector is turning towards our unit normal vector, and does so in a signed way. Concretely, 2 if α(s) is a unit-speed curve in R we define k(s) := hα00(s); n(s)i; where n(s) is1 the preferred normal vector along α. We play a similar game on the surface S. The geodesic curvature should tell us how much α0 is turning towards S, which is the preferred normal vector along α from the point of view of S. So we define the geodesic curvature by 00 κg(s) := hα (s); S(s)i: For emphasis we'll repeat: the geodesic curvature represents the planar curvature, as it would be measured by an inhabitant of the surface. 1This should be the only time in these notes that we use n for a normal to a curve. Otherwise we're using n to denote a unit normal to S. 1 Figure 1: A constant-height curve in a sphere. The red vectors represent S the preferred normal to α in S. The green vectors are α00. Notice that these are not perpendicular to S, so the geodesic curvature will be nonzero. One example of geodesic curvature that might come to mind is that of a great circle in a sphere. Consider, for instance, Earth's equator. Because our planet is round2 we know that the equator curves, but this is about as straight as we can hope for a curve on Earth to be. We'll soon see that the geodesic curvature of the equator is indeed 0, meaning that it's a straight line from our point of view | that is, as seen by Earthlings. Before we compute any geodesic curvatures it's worth noting that S is a member of an obvious orthonormal basis at α(s), given by (n; T; S). From its definition we see that the geodesic curvature is the S-component of α00(s), so we wonder about the other components. Because α is unit speed we know that α00 is perpendicular to T = α0, so the T-component is zero. We can then define the normal curvature of α to be 00 κn(s) := hα (s); n(s)i; so that 00 α (s) = κn(s)n(s) + κg(s)S(s): The normal curvature can be used to tell us about the extent to which the surface itself is curving, and later in the quarter we'll use it for this purpose. 3 Example 1. Let S be the sphere of radius R > 0 in R centered at the origin. We have a familiar parametrization of this surface given by x(u; v) = (R sin v cos u; R sin v sin u; R cos v): Now suppose α is cut out of S by a plane of the form z = c, as seen in Figure1. Along α the quantity R cos v is constant, and thus v is constant. Let θ0 be this constant value. We'll further 2I hope I've not offended anyone. 2 assume that −R < c < R, so that 0 < θ0 < π. Then we can produce a unit-speed parametrization of α as s s s α(s) = x ; θ0 = R sin θ0 cos ;R sin θ0 sin ;R cos θ0 : R sin θ0 R sin θ0 R sin θ0 Notice that s s α0(s) = − sin ; cos ; 0 R sin θ0 R sin θ0 and −1 s s α00(s) = cos ; sin ; 0 ; R sin θ0 R sin θ0 R sin θ0 so α(s) is indeed unit-speed. Now to compute the normal and geodesic curvatures of α we'll need to get our hands on S = n × T. We already have T(s) = α0(s), and because we're on a sphere centered at the origin we have 1 s s n(s) = α(s) = sin θ0 cos ; sin θ0 sin ; cos θ0 : R R sin θ0 R sin θ0 Then i j k s s sin θ0 cos sin θ0 sin cos θ0 S = n × T = R sin θ0 R sin θ0 − sin s cos s 0 R sin θ0 R sin θ0 s s = − cos θ0 cos ; − cos θ0 sin ; sin θ0 : R sin θ0 R sin θ0 Finally we can compute the geodesic curvature: 00 κg(s) = hα (s); S(s)i −1 2 s 2 s = − cos θ0 cos − cos θ0 sin R sin θ0 R sin θ0 R sin θ0 1 = cot θ : R 0 We can bring this computation back to reality. If α parametrizes the equator of S then θ0 = π=2, in which case the geodesic curvature is indeed zero. So the equator is seen as a straight line in S. On the other hand, if 0 < θ0 < π=2 then the geodesic curvature is positive, and α is turning towards S. In the southern hemisphere we have π=2 < θ0 < π, so the geodesic curvature is negative. In this region α is turning away from S, so this make sense. At last we'll compute the normal curvature of α. We have 00 κn(s) = hα (s); n(s)i −1 2 s 2 s = sin θ0 cos + sin θ0 sin R sin θ0 R sin θ0 R sin θ0 −1 = : R 3 Notice that this value doesn't depend on θ0 at all. Indeed, we can check that every curve on the sphere of radius R has geodesic curvature ±1=R. Indeed, let γ be a unit-speed curve on this sphere, and continue letting n be the outward-pointing normal. Then n = x=R, so we have 1 κ = hγ00; ni = γ00; γ : n R Now because γ takes its values on the sphere we know that hγ; γi = R2 for all values of s. Differ- entiating this tells us that hγ0; γi = 0 for all values of s. Differentiating again yields hγ00; γi + hγ0; γ0i = 0: But we've assumed that γ is unit-speed, so we see that hγ00; γi = −1, and thus 1 −1 κ = hγ00; γi = : n R R Later in the quarter we'll use this computation to describe the curvature of the sphere. It's worth pointing out that if we didn't care about signs, then we could have saved ourselves 2 2 2 some trouble by first computing κ and κn. Then we could have used the equation κ = κn + κg to solve for the geodesic curvature, up to sign. The second fundamental form and the Christoffel symbols We can think of the geodesic and normal curvatures as the tangential and normal components of the curvature, respectively. Indeed, you'll show in homework that 2 2 2 κ = κg + κn; 3 where κ is the usual curvature of a curve in R . Both of these curvatures are computed using the second derivative of our curve, so a natural next step is to wonder whether we can compute these more generally. That is, if we have a surface patch x: U!S, can we compute the tangential and normal components of xij, for each 1 ≤ i; j ≤ 2? First, let's write xij = c1x1 + c2x2 + c3n; (1) 3 where ck : U! R is some function , for k = 1; 2; 3. How do we determine the components c1; c2; c3? The normal component c3 is easy enough. We simply notice that hxij; ni = c3; since n is perpendicular to both x1 and x2, and n has unit length. We thus define Lij := hxij; ni; and we call the quantities Lij the coefficients of the second fundamental form.
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