This preview has intentionally blurred sections. Sign up to view the full version.
View Full Document
Unformatted text preview: Ge/Ay133 – Problem Set #2 Due October 13 th , 2011 1 Angular Momenta (a) Verify eq. (1.1) (page 3) in Armitage, and use it to estimate the total angular momentum of the spinning sun, and how much angular momentum the sun would have if it were spinning on the verge of breakup (i.e. the outer layers are essentially in orbit). Treat the sun as a uniform sphere. (b) Verify that the total angular momentum in the planets dwarfs that of the sun (also page 3 of Armitage) by summing the orbital angular momenta of all of the planets (ignore spins; they’re insignificant). The data needed for parts (a) and (b) may be found in Table 1.1 and pages 2,3 of Armitage. (c) Calculate the angular momentum of a spherical uniformlyrotating gas cloud that has a density of 100 hydrogen molecules per cm 3 , a radius of 10 parsecs (1 parsec is 3 × 10 16 m) and a rotation period of 100 million years (same formula as for the Sun). (d) What do you make of any of this (i.e. can we use any of this information to help us understand the process of planet formation and what do you think it tells us)? Note that many of the problems in this class will have a similar “what do you make of any of this” type question. The reason is that the calculations above are designed to make you think about the bigger picture of what is happening. So here is where youabove are designed to make you think about the bigger picture of what is happening....
View
Full Document
 Fall '10
 list
 Solar System, surface density, MMSN, mass surface density

Click to edit the document details