Tidal Forces. Effects of Tidal Forces. The Roche Distance: Tidal Breakup
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1 Reading:, Chap. 4, Sect. 4.6 (Tides); Chap. 12 (all) Homework #8: On website, due in recitation on Friday/Monday, Oct. 27/30 Exam 2 - Two weeks from Today (November 6) Last time: The Gas and Ice Giant Planets Astro 120 Fall 2018: Lecture 18 page 1 Jupiter (and Saturn) Today: Tides and Rings Tidal forces as differential gravitational force (stretch) deformation, spin synchronization, orbital changes the Roche Distance: tidal breakup Planetary Rings: flatness, structure, and resonances Ring Systems ways of seeing rings: reflection, transmission, occultation Saturn vs. Uranus, Jupiter, Neptune Atmosphere Composition (H, He) and cloud coloration Zones, Bands and circulation patterns Interior Differences between Jupiter and Saturn Uranus and Neptune Tidal Forces Astro 120 Fall 2018: Lecture 18 page 2 Tidal force = differential gravitational force (stretch) Gravity Stretching force Increases with decreasing distance Increases with increasing size Effects of Tidal Forces Deforms objects (Stretch+ squeeze) tidal bulge solid body tides (rock/ice) ocean tides Spin synchronization: grav. pull on planet/moon bulge slows rotation eventually, moon rotates once per orbit: 1:1 resonance Earth rotation slowed by Moon day gets longer (0.015 second/millennium) Orbital changes Moon pulled along by planet bulge orbit spirals outwards month gets longer (0.14 seconds/mill.) Synchronous rotation: rotation period = orbital period Astro 120 Fall 2018: Lecture 18 page 3 The Roche Distance: Tidal Breakup Astro 120 Fall 2018: Lecture 18 page 4 Satellites are held together by self-gravity Tidal force tries to stretch the satellite (F ~ 1/d 3 ) tide How close before F > self-gravity? tide Minimum Distance: The Roche Distance D = Roche distance = 2.5 x R R planet If a satellite strays to within D R it may be torn apart by tidal forces planet moon distance Jupiter Amalthea 2.5 R ju Mars Phobos 2.8 R ma Saturn Mimas 3.1 R sat Uranus Miranda 5.1 R ur Earth Moon 60 R earth
2 Planetary Rings Astro 120 Fall 2018: Lecture 18 page 5 Astro 120 Fall 2018: Lecture 18 page 6 always found inside the Roche limit not solid extremely thin gappy broad and bright (Saturn) narrow and dark (Jupiter, Uranus, Neptune) origins? Astro 120 Fall 2018: Lecture 18 page 7 The rings are very thin! (Cassini image, August 2015) Astro 120 Fall 2018: Lecture 18 page 8 Rings, edge on Saturn in background Shadow of rings on Saturn cloudtops
3 Astro 120 Fall 2018: Lecture 18 page The rings are very thin! (Cassini image, August 2015) What are they? Why so flat? 9 Astro 120 Fall 2018: Lecture 18 page 10 Solid sheets? Liquid? What? extremely thin translucent - stars shine through rotation speed changes with distance from planet Rings made of billions of particles (dust boulder size) Dimensions (Saturn s Rings) 300,000 km across Why so flat? less than 0.15 km (150m) thick material concentrates in equator more collisions when passing up or down vertical extent continually reduced Structure within the rings Astro 120 Fall 2018: Lecture 18 page 11 Large Gaps i.e. Cassini Division gap between A and B rings (not empty, but lower density of particles) Multiple rings broad rings composed of many(!) narrow rings Resonances orbital period of a ring region can be an integer fraction of a nearby moon s orbital period ring particle repeatedly tugged by moon resonance clears gap at specific place in ring example: Cassini Divison = 2:1 resonance with Mimas Astro 120 Fall 2018: Lecture 18 page 12
4 Astro 120 Fall 2018: Lecture 18 page 13 Astro 120 Fall 2018: Lecture 18 page 14 shepherding moon(lets) embedded in rings keep rings in line Atlas Daphnis Pan Complex ring structure slowly becoming understood Astro 120 Fall 2018: Lecture 18 page Cassini Ring Plane Crossing 15 Astro 120 Fall 2018: Lecture 18 page 16 Cassini Ring Plane Crossing
5 Astro 120 Fall 2018: Lecture 18 page 17 Astro 120 Fall 2018: Lecture 18 page 18 Cassini Ring Plane Crossing 3 ways to detect rings: Astro 120 Fall 2018: Lecture 18 page 19 Astro 120 Fall 2018: Lecture 18 page 20 Saturn ring occultation reflection transmission large and/or reflective particles (ice, rock) small particles (dust) scatters light forward (like fog) Amount of light blocked occultation high particle density blocks starlight
6 Ring Systems Astro 120 Fall 2018: Lecture 18 page 21 Astro 120 Fall 2018: Lecture 18 page 22 Saturn broad, reflective rings: water-ice particles size from dust to boulders gaps contain much smaller particles Uranus narrow, dark rings discovered by occultation in 1977 particles of carbon residue from methane ice? sharp ring edges caused by shepherding satellites Uranus Rings (transmission) Voyager 2 Uranus Rings (reflection) Jupiter Neptune Astro 120 Fall 2018: Lecture 18 page 23 dark, narrow ring discovered by Voyager in 1979 bright when viewed by transmission dark, very tenuous rings seen by Voyager in 1989 bright when viewed by transmission Astro 120 Fall 2018: Lecture 18 page 24 Saturn Jupiter Uranus Neptune
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