lecture l04 - astc25 physics of tides tides in the solar system roche limit of tidal disruption
TRANSCRIPT
![Page 1: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/1.jpg)
Lecture L04 - ASTC25
Physics of TidesTides in the solar system
Roche limit of tidal disruption
![Page 2: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/2.jpg)
![Page 3: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/3.jpg)
Damped oscillator as a model equation of tidal wave
braking
Natural frequency of oscillations = sqrt( spring constant)
Deformation (vertical, relative to sphere)
Frequency of forcing = spin frequency = angular speed of planet
forcingFree oscil.
![Page 4: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/4.jpg)
?
![Page 5: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/5.jpg)
![Page 6: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/6.jpg)
Net torque = 0, stable resonance
![Page 7: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/7.jpg)
![Page 8: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/8.jpg)
c
Phobos
Phobos has only ~1 Gyr more to live…
before a crash onto Mars
![Page 9: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/9.jpg)
Io
Europa
Ganimede
Callisto
![Page 10: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/10.jpg)
![Page 11: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/11.jpg)
Tidal flexing and heating of Io causesthe most activevolcanism in theSolar System
![Page 12: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/12.jpg)
Roche limit: tidal forces destroy bodies which come too close to a source of gravitation through differential acceleration
Consider an orbiting mass of fluid held together by gravity. Far from the Roche limit the mass is practically spherical. The body is deformed by tidal forces
Within the Roche limit the mass' own gravity (self-gravity) can no longer withstand the tidal forces, and the body disintegrates.
Particles closer to the primary orbit move more quickly than particles farther away, as represented by the red arrows.
The varying orbital speed of the material eventually causes it to form a ring.
http://www.answers.com/topic/roche-limit#wp-Fluid_satellites
![Page 13: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/13.jpg)
1992
1994
Jupiter disrupted tidally comet Shoemaker-Levy 9 (SL9)
![Page 14: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/14.jpg)
Roche limit:
Fluid limit: tides destroy a body bound byself-gravity withinthat minimumdistance r_R
Solid/rocky limit:the same but with additional binding(electromagnetic) forces of materialstrength
Q: which limit is larger?
First step in the computation is the estimation of the differential torque
Édouard Roche
(1820–1883)
![Page 15: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/15.jpg)
Roche limit
calculation
![Page 16: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/16.jpg)
Comet Shoemaker-Levi SL-9 (1994) disintegrated after approach to Jupiter, and so do the sun-grazing comets.
Roche limit
[pron.: rowsh]
![Page 17: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/17.jpg)
~2.2 R_p
satellites generally outside the rings
Roche limit for fluid satellite (~1849):
Roche limit for rocky satellite: 1.4
![Page 18: Lecture L04 - ASTC25 Physics of Tides Tides in the solar system Roche limit of tidal disruption](https://reader035.vdocument.in/reader035/viewer/2022062518/56649e7f5503460f94b8312f/html5/thumbnails/18.jpg)
Jup
iter
Sat
urn
Ura
nu
s
Nep
tun
e
R_p
2R_p
3R_p
=satellite
rings
0
Roche limit is somewherenear 2 R_p: satellitesdestroyed if closer to their planets.
Ring systems drawn to scale of their planets,
but not to relative scale.