Melting of Io by Tidal Dissipation

Peale, S. J.; Cassen, P.; Reynolds, R. T.

doi:10.1126/science.203.4383.892

Cited by 558 publications

(327 citation statements)

References 11 publications

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“…Being embedded in the Jovian magnetosphere, they are exposed to the complex flux of low-(plasma) and high-energy electron and ion bombardment (Dalton et al 2010). Io's surface is in fact dominated by sulfur dioxide, which is expelled from the very intense volcanic activity triggered by tidal effects (Peale et al 1979). Although it is thought that Io has lost nearly all of its hydrogen (Zolotov & Fegley 1999), the detection of hydrogen pickup ions by Galileo's plasma analyser (Frank & Paterson 1999) in the space surrounding the satellite raised the question regarding its origin.…”

Section: Solar System Objectsmentioning

confidence: 99%

Thermal and energetic processing of astrophysical ice analogues rich in SO₂

Kaňuchová

Boduch

Domaracka

et al. 2017

A&A

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Context. Sulfur is an abundant element in the cosmos and it is thus an important contributor to astrochemistry in the interstellar medium and in the solar system. Astronomical observations of the gas and of the solid phases in the dense interstellar/circumstellar regions have evidenced that sulfur is underabundant. The hypothesis to explain such a circumstance is that it is incorporated in some species in the solid phase (i.e. as frozen gases and/or refractory solids) and/or in the gas phase, which for different reasons have not been observed so far. Aims. Here we wish to give a contribution to the field by studying the chemistry induced by thermal and energetic processing of frozen mixtures of sulfur dioxide (one of the most abundant sulfur-bearing molecules observed so far) and water. Methods. We present the results of a series of laboratory experiments concerning thermal processing of different H 2 O:SO 2 mixtures and ion bombardment (30 keV He + ) of the same mixtures. We used in situ Fourier transform infrared (FTIR) spectroscopy to investigate the induced effects. Results. The results indicate that ionic species such as HSO − 3 , HSO − 4 , and S 2 O 2− 5 are easily produced. Energetic processing also produces SO 3 polymers and a sulfurous refractory residue. Conclusions. The produced ionic species exhibit spectral features in a region that, in astronomical spectra of dense molecular clouds, is dominated by strong silicate absorption. However, such a dominant feature is associated with some spectral features, some of which have not yet been identified. We suggest adding the sulfur-bearing ionic species to the list of candidates to help explain some of those features. In addition, we suggest that once expelled in the gas phase by sublimation, due to the temperature increase, and/or by non-thermal erosion those species would constitute a class of molecular ions not detected so far. We also suggest that molecular sulfur-bearing ions could be present on the surfaces and/or in the atmospheres of several objects in the solar system, for example icy satellites of the giant planets and comets.

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Section: Solar System Objectsmentioning

confidence: 99%

Thermal and energetic processing of astrophysical ice analogues rich in SO₂

Kaňuchová

Boduch

Domaracka

et al. 2017

A&A

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“…Mayor et al showed that this planet's eccentricity occasionally reaches values of 0.1. Applying common models of tidal heating (e.g., Peale et al 1979;Jackson et al 2008aJackson et al , 2008bBarnes et al 2009), and assuming the planet to be terrestrial-like, GJ 581 e could have 2 orders of magnitude more tidal heating than Jupiter's volcanic satellite Io! Although this planet is not in the IHZ, similar heating rates on planets in the IHZ are unlikely to develop life (Jackson et al 2008a).…”

Section: Introductionmentioning

confidence: 99%

Tidal Limits to Planetary Habitability

Barnes

Jackson

Greenberg

et al. 2009

ApJ

127

110

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The habitable zones (HZs) of main-sequence stars have traditionally been defined as the range of orbits that intercept the appropriate amount of stellar flux to permit surface water on a planet. Terrestrial exoplanets discovered to orbit M stars in these zones, which are close-in due to decreased stellar luminosity, may also undergo significant tidal heating. Tidal heating may span a wide range for terrestrial exoplanets and may significantly affect conditions near the surface. For example, if heating rates on an exoplanet are near or greater than that on Io (where tides drive volcanism that resurfaces the planet at least every 1 Myr) and produce similar surface conditions, then the development of life seems unlikely. On the other hand, if the tidal heating rate is less than the minimum to initiate plate tectonics, then CO 2 may not be recycled through subduction, leading to a runaway greenhouse that sterilizes the planet. These two cases represent potential boundaries to habitability and are presented along with the range of the traditional HZ for main-sequence, low-mass stars. We propose a revised HZ that incorporates both stellar insolation and tidal heating. We apply these criteria to GJ 581 d and find that it is in the traditional HZ, but its tidal heating alone may be insufficient for plate tectonics.

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“…The value for Mercury is Q Mercury < 190, and for Venus it is Q Venus < 17 (Goldreich and Soter, 1966). Observations of Io imply Q Io < 100 (Peale et al, 1979;Segatz et al, 1988), while the Moon lies at Q Moon = 26.5 -1 (Dickey et al, 1994). These measurements indicate a similar order of magnitude for the tidal dissipation function of all desiccated bodies in the Solar System.…”

Section: E4 Tidal Response In Celestial Bodiesmentioning

confidence: 74%

“…Tidal heating is responsible for the volcanism on Io (Strom et al, 1979;Laver et al, 2007), which was predicted by Peale et al (1979) with the use of tidal theory. Io is a small body orbiting Jupiter with an eccentricity of 0.0041 that is maintained by the gravitational perturbations of its fellow Galilean moons and shows global volcanism that resurfaces the planet on a timescale of 100 to 10 5 years ( Johnson et al, 1979;Blaney et al, 1995;McEwen et al, 2004).…”

Section: Introductionmentioning

confidence: 98%

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

et al. 2013

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Traditionally, stellar radiation has been the only heat source considered capable of determining global climate on long timescales. Here, we show that terrestrial exoplanets orbiting low-mass stars may be tidally heated at highenough levels to induce a runaway greenhouse for a long-enough duration for all the hydrogen to escape. Without hydrogen, the planet no longer has water and cannot support life. We call these planets ''Tidal Venuses'' and the phenomenon a ''tidal greenhouse.'' Tidal effects also circularize the orbit, which decreases tidal heating. Hence, some planets may form with large eccentricity, with its accompanying large tidal heating, and lose their water, but eventually settle into nearly circular orbits (i.e., with negligible tidal heating) in the habitable zone (HZ). However, these planets are not habitable, as past tidal heating desiccated them, and hence should not be ranked highly for detailed follow-up observations aimed at detecting biosignatures. We simulated the evolution of hypothetical planetary systems in a quasi-continuous parameter distribution and found that we could constrain the history of the system by statistical arguments. Planets orbiting stars with masses < 0.3 M Sun may be in danger of desiccation via tidal heating. We have applied these concepts to Gl 667C c, a *4.5 M Earth planet orbiting a 0.3 M Sun star at 0.12 AU. We found that it probably did not lose its water via tidal heating, as orbital stability is unlikely for the high eccentricities required for the tidal greenhouse. As the inner edge of the HZ is defined by the onset of a runaway or moist greenhouse powered by radiation, our results represent a fundamental revision to the HZ for noncircular orbits. In the appendices we review (a) the moist and runaway greenhouses, (b) hydrogen escape, (c) stellar mass-radius and mass-luminosity relations, (d) terrestrial planet mass-radius relations, and (e) linear tidal theories.

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Melting of Io by Tidal Dissipation

Abstract: The dissipation of tidal energy in Jupiter's satellite Io is likely to have melted a major fraction of the mass. Consequences of a largely molten interior may be evident in pictures of Io's surface returned by Voyager I.

Cited by 558 publications

References 11 publications

Thermal and energetic processing of astrophysical ice analogues rich in SO₂

Thermal and energetic processing of astrophysical ice analogues rich in SO₂

Tidal Limits to Planetary Habitability

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

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Melting of Io by Tidal Dissipation

Abstract: The dissipation of tidal energy in Jupiter's satellite Io is likely to have melted a major fraction of the mass. Consequences of a largely molten interior may be evident in pictures of Io's surface returned by Voyager I.

Cited by 558 publications

References 11 publications

Thermal and energetic processing of astrophysical ice analogues rich in SO2

Thermal and energetic processing of astrophysical ice analogues rich in SO2

Tidal Limits to Planetary Habitability

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

Contact Info

Product

Resources

About

Thermal and energetic processing of astrophysical ice analogues rich in SO₂

Thermal and energetic processing of astrophysical ice analogues rich in SO₂