# Talk:Asteroids in fiction

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## Update flag

I'm removing this, because I have no idea what it is doing in this article (it seems particularly inappropriate to an article about works of fiction). RandomCritic 16:47, 19 October 2006 (UTC)

## Merger

As far as I can tell, "merger" will essentially take the form of deleting the entire section from the Asteroid article; there's nothing there that isn't already here. Which does not, of course, mean that it's a bad idea. RandomCritic 19:47, 14 April 2007 (UTC)

## Gundam Entry

Sorry for not noticing the paragraph down there before adding stuff. The problem here is, Juno(renamed Luna II in the series) is a real asteroid, while the others have no real world reference. Would it be better to have it seperated from the virtual ones and listed under Juno, or would it be better to tag everything down in the virtual section? Seems like the virtual section is a bit to long for now(most information could be found on the page I linked to on Luna II anyway), we can trim it down and just mention the names and location instead of having the lengthy plot here. MythSearchertalk 07:20, 18 April 2007 (UTC)

Perhaps a Gundam Wing reference can be added under Mineral Extraction. There were various asteroids designated MO#. With MO III being destroyed in Endless Waltz; It was a mobile suit factory/base. — Preceding unsigned comment added by 142.167.230.161 (talk) 19:04, 1 June 2012 (UTC)

## Can anyone hunt this one down?

I remember an old Outer Limits-like episode (B&W, ca. 1960s or early 1970s) taking place on an asteroid, where the plot is about the search for a fossil (Archaeopteryx-like) that an astronaut had glimpsed. He fails to find it (his air running out, or some such) by a hair's breadth (it was litterally behind the last rock he turned back at). Ring any bells? Urhixidur (talk) 05:23, 9 December 2007 (UTC)

## Earth-to-rubble energy computation

A simple estimation, assuming uniform density, goes as follows. The energy required to pull the Earth apart is equivalent to that released during its formation (one process being just the time-reverse of the other). Midway through the process, we have a central sphere of radius r, density ρ, upon which accretes a shell of thickness dr (same density). The energy involved is just the gravitational potential energy, GMm/r. The central mass M is (4/3)πr³ρ, the shell mass m is 4πr²drρ. Thus the total energy is:

$\int\limits_{0}^{R}\frac{G M m}{r} = \int\limits_{0}^{R}\frac{G (4\pi r^3 \rho) (4\pi r^2 \rho dr)}{3r} = \frac{16\pi^2G \rho^2}{3}\int\limits_{0}^{R}r^4 dr = \frac{16\pi^2G \rho^2}{15}R^5$

Plugging in the numbers for G (6.67242×10−11 m³/kg s²), R (6.371×106 m), and ρ (5.515×103 kg/m³) we get 2.24×1032 J. Dividing by the Sun's luminosity of 3.85×1026 W yields 5.83×105 s = 6.75 d. The equation can be rewritten as 3GM²/5R, if you wish to apply it to other bodies such as Venus, Mars, Jupiter, etc. Urhixidur (talk) 19:12, 25 November 2008 (UTC)