Chapter 12: Problem 81
State the definition of a vector-valued function in the plane and in space.
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Chapter 12: Problem 81
State the definition of a vector-valued function in the plane and in space.
These are the key concepts you need to understand to accurately answer the question.
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Centripetal Force An object of mass \(m\) moves at a constant speed \(v\) in a circular path of radius \(r .\) The force required to produce the centripetal component of acceleration is called the centripetal force and is given by \(F=m v^{2} / r .\) Newton's Law of Universal Gravitation is given by \(F=G M m / d^{2}\), where \(d\) is the distance between the centers of the two bodies of masses \(M\) and \(m\), and \(G\) is a gravitational constant. Use this law to show that the speed required for circular motion is \(v=\sqrt{G M / r}\)
Find the vectors \(T\) and \(N\), and the unit binormal vector \(\mathbf{B}=\mathbf{T} \times \mathbf{N}\), for the vector-valued function \(\mathbf{r}(t)\) at the given value of \(t\). $$ \mathbf{r}(t)=t \mathbf{i}+t^{2} \mathbf{j}+\frac{t^{3}}{3} \mathbf{k} $$ $$ t_{0}=1 $$
You are asked to verify Kepler's Laws of Planetary Motion. For these exercises, assume that each planet moves in an orbit given by the vector- valued function \(\mathbf{r}\). Let \(\boldsymbol{r}=\|\mathbf{r}\|\), let \(\boldsymbol{G}\) represent the universal gravitational constant, let \(M\) represent the mass of the sun, and let \(m\) represent the mass of the planet. Prove that \(\mathbf{r} \cdot \mathbf{r}^{\prime}=r \frac{d r}{d t}\)
Find the curvature \(K\) of the curve. \(\mathbf{r}(t)=4 \cos 2 \pi t \mathbf{i}+4 \sin 2 \pi t \mathbf{j}\)
Find all \(a\) and \(b\) such that the two curves given by \(y_{1}=a x(b-x) \quad\) and \(\quad y_{2}=\frac{x}{x+2}\) intersect at only one point and have a common tangent line and equal curvature at that point. Sketch a graph for each set of values of \(a\) and \(b\).
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