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--- 183_notes:escape_speed [2015/10/09 20:23] – [Calculating the Escape Speed] caballero
+++ 183_notes:escape_speed [2021/04/01 12:37] (current) – [Calculating the Escape Speed] stumptyl
@@ Line 1: / Line 1: @@
+Section 6.10 in Matter and Interactions (4th edition)
 ===== Escape Speed =====
-Gravitational systems are particularly interesting because there are so many examples of such systems. The formation of our universe from immense galactic structures, to solar systems with planets and moons, and even the orbits of asteroids and comets are all examples of gravitational systems. In these notes, you will read about a particular gravitational phenomenon: how a small object can escape the gravitational bounds of a much more massive object. This object must move with at least the escape speed.
+Gravitational systems are particularly interesting because there are so many examples of such systems. The formation of our universe from immense galactic structures to solar systems with planets and moons, and even the orbits of asteroids and comets are all examples of gravitational systems. **In these notes, you will read about a particular gravitational phenomenon: how a small object can escape the gravitational bounds of a much more massive object. This object must move with at least the escape speed.**
 ==== Conditions on the Speed ====
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   * Final:  $r=\infty$ ;  $v=0$
-The [[183_notes:energy_cons|Energy Principle tells you that the energy of this system is conserved]]. Moreover, you know from the final state where  $r\rightarrow \infty$  and  $v\rightarrow 0$  that both the final potential and final kinetic energies are zero. Hence, the total energy of the system must be zero.
+The [[183_notes:energy_cons|Energy Principle tells you that the energy of this system is conserved]]. __Moreover, you know from the final state where  $r\rightarrow \infty$  and  $v\rightarrow 0$  that both the final potential and final kinetic energies are zero. Hence, the total energy of the system must be zero.__
  $\Delta E_{sys} = W_{surr} = 0 \longrightarrow E_{sys,f} = E_{sys,i}$
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  $v_{esc} = \sqrt{\dfrac{2GM}{R}}$
-This speed defines the minimum speed needed to leave the planet and never return under the gravitational interaction between the object and the planet. Notice that this speed doesn't depend on the mass of the launched object (so long as it is much less than the planet).
+This speed defines the minimum speed needed to leave the planet and never return under the gravitational interaction between the object and the planet. **__Reminder that this speed term utilizes the SI unit of m/s.__**  Notice that this speed doesn't depend on the mass of the launched object (so long as it is much less than the planet).