Secondary and sesquinary craters on Europa

Zahnle, Kevin; Alvarellos, J. L.; Dobrovolskis, Anthony R.; Hamill, Patrick

doi:10.1016/j.icarus.2007.10.024

Cited by 72 publications

(46 citation statements)

References 24 publications

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“…This combination of liquid water and an available energy source is among the known requirements for life, and has led to much speculation as to the potential habitability of this vast ocean. Significantly, Europa's surface is relatively young (between 60 and 100 Ma; Zahnle et al 2008) and exhibits an intricate overlay of cracks and ridges. This suggests that liquid from the ocean beneath is at times expressed on the surface.…”

Section: Introductionmentioning

confidence: 99%

Chemistry of Frozen Sodium–magnesium–sulfate–chloride Brines: Implications for Surface Expression of Europa’s Ocean Composition

Hodyss

Choukroun

et al. 2016

ApJL

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The composition of Europa's subsurface ocean is a critical determinant of its habitability. However, our current understanding of the ocean composition is limited to its expression on the surface. This work investigates experimentally the composition of mixed sodium-magnesium-sulfate-chloride solutions when frozen to 100 K, simulating conditions that likely occur as ocean fluids are emplaced onto Europa's surface. Micro-Raman spectroscopy is used to characterize phase composition of the frozen brines at 100 K.

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Section: Introductionmentioning

confidence: 99%

Chemistry of Frozen Sodium–magnesium–sulfate–chloride Brines: Implications for Surface Expression of Europa’s Ocean Composition

Hodyss

Choukroun

et al. 2016

ApJL

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“…Moons of Jupiter (Zahnle et al 2008) andSaturn (Alvarrelos et al 2005;Bierhaus et al 2012) and Mars (Ramsey and Head 2013).…”

Section: Studied Locationsmentioning

confidence: 99%

Sinuous Rille

Komatsu¹,

Hargitai²

2015

Encyclopedia of Planetary Landforms

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“…184 100. † Antapex initial conditions generated assuming the spallation model (Melosh 1989) as modified by Zahnle et al (2008). Table 5 likewise lists the fates of ejecta launched from the six cardinal points on the surface of Telesto.…”

Section: Ejecta From Coorbitals Produced By Centaur Impactsmentioning

confidence: 99%

“…Fates of "realistic" (that is, resulting from cometary impact) ejecta from Telesto after 100,000 years; see Table 4 for explanation. (Melosh 1989) as modified by Zahnle et al (2008).…”

Section: Ejecta From Coorbitals Produced By Centaur Impactsmentioning

confidence: 99%

Exchange of ejecta between Telesto and Calypso: Tadpoles, horseshoes, and passing orbits

Dobrovolskis

Alvarellos²,

Zahnle

et al. 2010

Icarus

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We have numerically integrated the orbits of ejecta from Telesto and Calypso, the two small Trojan companions of Saturn's major satellite Tethys. Ejecta were launched with speeds comparable to or exceeding their parent's escape velocity, consistent with impacts into regolith surfaces. We find that the fates of ejecta fall into several distinct categories, depending on both the speed and direction of launch.The slowest ejecta follow sub-orbital trajectories and re-impact their source moon in less than one day. Slightly faster debris barely escape their parent's Hill sphere and are confined to tadpole orbits, librating about Tethys' triangular Lagrange points L 4 (leading, near Telesto) or L 5 (trailing, near Calypso) with nearly the same orbital semi-major axis as Tethys, Telesto, and Calypso. These ejecta too eventually re-impact their source moon, but with a median lifetime of a few dozen years. Those which re-impact within the first ten years or so have lifetimes near integer multiples of 348.6 days (half the tadpole period).Still faster debris with azimuthal velocity components ∼ > 10 m/s enter horseshoe orbits which enclose both L 4 and L 5 as well as L 3 , but which avoid Tethys and its Hill sphere. These ejecta impact either Telesto or Calypso at comparable rates, with median lifetimes of several thousand years. However, they cannot reach Tethys itself; only the fastest ejecta, with azimuthal velocites ∼ > 40 m/s, achieve "passing orbits" which are able to encounter Tethys. Tethys accretes most of these ejecta within several years, but some 1% of them are scattered either inward to hit Enceladus or outward to strike Dione, over timescales on the order of a few hundred years.

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Secondary and sesquinary craters on Europa

Cited by 72 publications

References 24 publications

Chemistry of Frozen Sodium–magnesium–sulfate–chloride Brines: Implications for Surface Expression of Europa’s Ocean Composition

Chemistry of Frozen Sodium–magnesium–sulfate–chloride Brines: Implications for Surface Expression of Europa’s Ocean Composition

Sinuous Rille

Exchange of ejecta between Telesto and Calypso: Tadpoles, horseshoes, and passing orbits

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