Tides on Earth, in the Solar System and Beyond..
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1 483rd WE-Heraeus Seminar Extrasolar Planets: Towards Comparative Planetology beyond the Solar System Tides on Earth, Rosetta_CD\PR\what_is_RS.ppt, :36AM, 1 in the Solar System and Beyond.. Martin Pätzold Rheinisches Institut für Umweltforschung an der Universität zu Köln Abteilung Planetenforschung Köln
2 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 2
3 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 3
4 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 4
5 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 5
6 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 6
7 tide levels for Hamburg, Sankt Pauli: Tuesday, 7th June 2011 (CEST) Rosetta_CD\PR\what_is_RS.ppt, :36AM, 7 Low tide 04: m High tide 09: m Low tide 16: m High tide 21: m Bundesamt für Seeschifffahrt und Hydrographie
8 Mont St. Michel, Bretagne Rosetta_CD\PR\what_is_RS.ppt, :36AM, 8
9 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 9
10 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 10
11 The tidal force is a differenced force! Rosetta_CD\PR\what_is_RS.ppt, :36AM, 11
12 The formation of the tidal bulge is usually known as the (high) tide Rosetta_CD\PR\what_is_RS.ppt, :36AM, 12
13 Revolution without rotation Rosetta_CD\PR\what_is_RS.ppt, :36AM, 13
14 Revolution without rotation But the Earth rotates! Rosetta_CD\PR\what_is_RS.ppt, :36AM, 14
15 The Earth rotates faster than the Moon revolves Rosetta_CD\PR\what_is_RS.ppt, :36AM, 15
16 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Rosetta_CD\PR\what_is_RS.ppt, :36AM, 16
17 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 17 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Torques try to pull the tidal bulge back into LOS
18 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 18 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Torques try to pull the tidal bulge back into LOS Consequence is a slow down of Earth rotation (tidal friction)
19 average change in LOD due to lunar tides: 2.3 ms/cy Rosetta_CD\PR\what_is_RS.ppt, :36AM, 19 change in LOD relative to s
20 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 20 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Torques try to pull the tidal bulge back into LOS Consequence is a slow down of Earth rotation (tidal friction) another consequence from conservation of angular momentum: the Moon recedes from the Earth
21 The first extraterrestrial applied space geophysicist seismometer Lunar Laser Ranging Reflector Rosetta_CD\PR\what_is_RS.ppt, :36AM, 21 Buzz Aldrin, Apollo 11, 1969
22 Apollo 15 reflector Lunar Laser Ranging Wettzell Lunar Laser Station Rosetta_CD\PR\what_is_RS.ppt, :36AM, 22
23 Lunar Laser Ranging The Moon recedes from Earth by 4m/cy Wettzell Lunar Laser Station Apollo 15 reflector Rosetta_CD\PR\what_is_RS.ppt, :36AM, 23
24 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 24 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS by 3 Earth rotates below the tidal bulge A location on the surface experiences periodically high and low tides
25 Ocean tides are the directly visible manifestation of tidal forces Rosetta_CD\PR\what_is_RS.ppt, :36AM, 25
26 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 26 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Torques try to pull the tidal bulge back into LOS Consequence is a slow down of Earth rotation (tidal friction) another consequence from conservation of angular momentum: the Moon recedes from the Earth Is there a case in the solar system where a moon revolves faster than the planet rotates?
27 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 27 The Earth rotates faster than the Moon revolves The tidal bulge is advancing the direct LOS Torques try to pull the tidal bulge back into LOS Consequence is a slow down of Earth rotation (tidal friction) another consequence from conservation of angular momentum: the Moon recedes from the Earth Is there a case in the solar system where a moon revolves faster than the planet rotates? YES, there is!
28 The Mars/Phobos case Rosetta_CD\PR\what_is_RS.ppt, :36AM, 28
29 The Mars/Phobos case Phobos size : 26 x 22 x 18 km period : 7 h 39 m distance : 9,378 km Mars radius period : 3,990 km : 24 h 37 m Rosetta_CD\PR\what_is_RS.ppt, :36AM, 29 Deimos size : 15 x 12 x 10 km period : 30 h 17 m distance : 23,459 km
30 The Mars/Phobos case Phobos size : 26 x 22 x 18 km period : 7 h 39 m distance : 9,378 km Mars radius period : 3,990 km : 24 h 37 m Rosetta_CD\PR\what_is_RS.ppt, :36AM, 30 Deimos size : 15 x 12 x 10 km period : 30 h 17 m distance : 23,459 km synchronous orbit: planetary rotation = moon revolution Mars 24 h 37 m 21,000 km distance Phobos: inside Deimos: outside
31 The Mars/Phobos case Rosetta_CD\PR\what_is_RS.ppt, :36AM, 31
32 The Mars/Phobos case Rosetta_CD\PR\what_is_RS.ppt, :36AM, 32
33 The Mars/Phobos case The orbit of Phobos decays until the Roche limit is reached. 1/ 3 1/ 3 P MP ar crs crp S M S Rosetta_CD\PR\what_is_RS.ppt, :36AM, 33
34 The Mars/Phobos case The orbit of Phobos decays until the Roche limit is reached. Roche limit: 1/ 3 1/ 3 P MP ar crs crp S M S Rosetta_CD\PR\what_is_RS.ppt, :36AM, 34 Proportionality factor c depends on the nature of the secondary: fluid c = 2.44 => a R = 10,500 km solid c = 1.26 => a R = 5,500 km rubble pile c = 1.54 => a R = 6,700 km
35 The Mars/Phobos case The orbit of Phobos decays until the Roche limit is reached. Roche limit: 1/ 3 1/ 3 P MP ar crs crp S M S Rosetta_CD\PR\what_is_RS.ppt, :36AM, 35 Proportionality factor c depends on the nature of the secondary: fluid c = 2.44 => a R = 10,500 km solid c = 1.26 => a R = 5,500 km rubble pile c = 1.54 => a R = 6,700 km Phobos is highly porous => rubble pile (Andert et al., 2010)
36 When will Phobos reach the Roche limit? Roche a 13/2 a 13/2 R k M 2, Mars Ph R 5 GM Q M Mars Mars Mars Mars Rosetta_CD\PR\what_is_RS.ppt, :36AM, 36
37 When will Phobos reach the Roche limit? Roche a 13/2 a 13/2 R k M 2, Mars Ph R 5 GM Q M Mars Mars Mars Mars Rosetta_CD\PR\what_is_RS.ppt, :36AM, 37
38 When will Phobos reach the Roche limit? Roche a 13/2 a 13/2 R k M 2, Mars Ph R 5 GM Q M Mars Mars Mars Mars Rosetta_CD\PR\what_is_RS.ppt, :36AM, 38
39 Other tidal phenomena in the solar system Rosetta_CD\PR\what_is_RS.ppt, :36AM, 39 forcing Mercury in a 3/2 resonance forcing all moons in the solar system into synchronous rotation deforming the Jupiter moon Io periodically => tidal heating => volcanic activity and the non-plus-ultra:
40 Other tidal phenomena in the solar system Rosetta_CD\PR\what_is_RS.ppt, :36AM, 40 forcing Mercury in a 3/2 resonance forcing all moons in the solar system into synchronous rotation deforming the Jupiter moon Io periodically => tidal heating => volcanic activity and the non-plus-ultra: synchronizing the Pluto system
41 Tides in extrasolar systems Rosetta_CD\PR\what_is_RS.ppt, :36AM, 41 studying tides in extrasolar planetary systems requires the knowledge of mass and size of the planet and the star feasible with transiting planets combined with radial velocity observations and spectroscopy orbital decay => survivability stellar spin-up spin-orbit coupling => synchronization of rotation and revolution circularization => e -> 0
42 The tidal potential or the Doodson constant two tidal potentials: a)the primary acting on the secondary b) The secondary acting on the primary Rosetta_CD\PR\what_is_RS.ppt, :36AM, 42 D ps GM a 3 p R 2 s D sp GM a s 3 R 2 p
43 The tidal potential or the Doodson constant two tidal potentials: a) The primary acting on the secondary b) The secondary acting on the primary Rosetta_CD\PR\what_is_RS.ppt, :36AM, 43 D ps GM a 3 p R 2 s Earth/Moon system: Earth on Moon Moon on Earth D ps = 20.9 m 2 /s 2 D sp = 3.5 m 2 /s 2 D sp GM a s 3 R 2 p Sun on Earth D sp = 1.6 m 2 /s 2
44 When will the planet reach the stellar Roche limit? Rosetta_CD\PR\what_is_RS.ppt, :36AM, 44 Roche a 13 / 2 a 13 / 2 R k M 2, star P R 5 GM Q M star star star star
45 When will the planet reach the stellar Roche limit? Rosetta_CD\PR\what_is_RS.ppt, :36AM, 45 Roche a 13 / 2 a 13 / 2 R k M 2, star P R 5 GM Q M star star star star stellar property factor
46 When will the planet reach the stellar Roche limit? Rosetta_CD\PR\what_is_RS.ppt, :36AM, 46 Roche a 13 / 2 a 13 / 2 R k M 2, star P R 5 GM Q M star star star star
47 Rosetta_CD\PR\what_is_RS.ppt, :36AM, 47 tidal forces affect the evolution of extrasolar planetary systems if a < 0.1 AU if M p is large may force orbits towards e -> 0 may lead to the loss of companions may force massive companions into doublesynchronous rotation but the companion is not safe. may spin-up stellar rotation (look for old fast rotating stars)
48 book your next boat tour when the tide is in! Rosetta_CD\PR\what_is_RS.ppt, :36AM, 48
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