Effects of Shape and Spin on the Tidal Disruption of P/Shoemaker-Levy 9

Details Effects of Shape and Spin on the Tidal Disruption of P/Shoemaker-Levy 9 Effects of Shape and Spin on the Tidal Disruption of P/Shoemaker-Levy 9

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996em%26p...72..113h&link_type=abstract

Earth, Moon and Planets, Volume 72, Issue 1-3, pp. 113-117

Physics

2

Scientific paper

I derive an approximate criterion for the tidal disruption of a “rubble pile” body as it passes close to a planet (or the sun): 2!1!+-% feaafiart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9Lq-Jc9% vqaqpepm0xbba9pwe9Q8fs0-yqaqpepae9pg0FirpepeKkFr0xfr-x% fr-xb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaGaeqyWdi3aaS% baaSqaaiaacogaaeqaaOGaeyisIS7aamWaaeaacaaIYaGaeqyWdihd% caWGWbGccaGGDbWaaeWaaeaadaWcaaqaaiaadkfamiaadchaaOqaai% aadkhaaaaacaGLOaGaayzkaaWaaWbaaSqabeaacaaIZaaaaOGaey4k% aSYaaeWaaeaadaWcaaqaaiabeM8a3bqaaiabeM8a3XGaaGimaaaaaO% GaayjkaiaawMcaamaaCaaaleqabaGaaGOmaaaaaOGaay5waiaaw2fa% amaabmaabaWaaSaaaeaacaWGHbaabaGaamOyaaaaaiaawIcacaGLPa% aacaGGSaaaaa!5229![ρ _c ≈ left[ {2ρ p]left( {{Rp}/r} right)^3 + left( {ω /{ω 0}} right)^2 } right]left( {a/b} right),] where ϱ c is the critical density below which the body will be disrupted, ϱ p is the density of the planet (or sun), R p is the radius of the planet, r is the periapse distance, Ω is the rotation frequency of the body, Ω0 is the surface orbit frequency about a body of unit density, and a/b is the axis ratio of the body, considered as a prolate ellipsoid. For P/Shoemaker Levy 9, in its passage close to Jupiter in 1992, this expression suggests that the critical density is 1.2 for a spherical, non-spinning nucleus, but could be >2.5 for a 2:1 elongate body with a typical rotation period of 10 hours.

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