Destination: Earth. Martian Meteorite Delivery

Gladman, Brett

doi:10.1006/icar.1997.5828

Cited by 116 publications

(105 citation statements)

References 47 publications

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“…Ceplecha et al (1998) estimated that 70% of a meteorite is ablated during atmospheric transit. Gladman (1997) suggested that 10 to 20% of the radius of small meteorites is destroyed. In computer calculations, Mileikowsky et al (2000) showed that a rock requires a diameter of more than 0.2 m to avoid being heated to above 100 °C throughout.…”

Section: Survival Of Atmospheric Entrymentioning

confidence: 99%

Planetary targets in the search for extrasolar oxygenic photosynthesis

Cockell

Raven

Kaltenegger

et al. 2009

Plant Ecology & Diversity

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Background:In the coming decades space telescopes will be constructed that will attempt to find the gaseous products of oxygenic photosynthesis, the most promising biosignatures of life, in the atmospheres of temperate Earth-like planets orbiting distant stars. Aims: This paper aims to provide a synthesis of the range of feasible targets -either planets or their satellites -that could harbour photosynthesis. Methods: We calculated photosynthetically active radiation (PAR) fluxes on a diversity of planetary bodies including those receiving direct light from a single star, similarly to the Earth, and investigated the potential of these fluxes to support photosynthesis. Results: All main sequence stars emit radiation that is capable of supporting photosynthesis on Earth-like planets. We discuss tidally-locked M star planets as a special case. Less conventional targets for searches include large moons orbiting gas giant planets, which receive reflected light from their host planets and from the host star, planets in stable orbits in binary star systems, and the search for two planets within the same star system with photosynthetic signatures. Conclusions: A diversity of planetary bodies are targets in the search for extrasolar photosynthesis. The demonstration that many or none of these candidate planetary bodies harbour photosynthesis would be an important conclusion in understanding the evolution and prevalence of photosynthesis.

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Section: Survival Of Atmospheric Entrymentioning

confidence: 99%

Planetary targets in the search for extrasolar oxygenic photosynthesis

Cockell

Raven

Kaltenegger

et al. 2009

Plant Ecology & Diversity

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“…Many studies of cratering dynamics have attempted to describe the dimensions of a crater resulting from an impact capable of ejecting martian materials into an Earth-crossing orbit (Nyquist 1983(Nyquist , 1984Melosh 1985;O'Keefe and Ahrens 1986;Vickery and Melosh 1987;Warren 1994;Gladman 1997;Head 1999;Head and Melosh 2000;Mileikowsky et al 2000;Head et al 2002). Early work indicated that favored candidate craters would be ~100-200 km in diameter and/or that oblique impacts might be required to eject materials from Mars' gravity field, but the most recent estimates have revised the minimum size of circular craters tõ 3 km.…”

Section: Constraints On and Past Searches For Snc Source Regions On Marsmentioning

confidence: 99%

Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars

Hamilton

Christensen

McSween

et al. 2003

Meteorit & Planetary Scien

164

165

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Abstract-The objective of this study was to identify and map possible source regions for all 5 known martian meteorite lithologies (basalt, lherzolite, clinopyroxenite, orthopyroxenite, and dunite) using data from the Mars Global Surveyor Thermal Emission Spectrometer (MGS TES). We deconvolved the TES data set using laboratory spectra of 6 martian meteorites (Los Angeles, Zagami, ALH A77005, Nakhla, ALH 84001, and Chassigny) as end members, along with atmospheric and surface spectra previously derived from TES data. Global maps (16 pixels/degree) of the distribution of each meteorite end member show that meteorite-like compositions are not present at or above TES detectability limits over most of the planet's dust-free regions. However, we have confidently identified local-scale (100s-1000s km 2 ) concentrations of olivine-and orthopyroxene-bearing materials similar to ALH A77005, Chassigny, and ALH 84001 in Nili Fossae, in and near Ganges Chasma, in the Argyre and Hellas basin rims, and in Eos Chasma. Nakhla-like materials are identified near the detection limit throughout the eastern Valles Marineris region and portions of Syrtis Major. Basaltic shergottites were not detected in any spatially coherent areas at the scale of this study. Martian meteorite-like lithologies represent only a minor portion of the dust-free surface and, thus, are not representative of the bulk composition of the ancient crust. Meteorite-like spectral signatures identified above TES detectability limits in more spatially restricted areas (

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“…[ The dynamical studies in this paper describe the ejecta as a spherically symmetric distribution traveling radially away from the planet, similar to the assumption adopted by Gladman 1997. In order to account for a range of velocities, we simulate the particles with velocities, v ∞ , from 0.0 to 3.3 km s −1 , which is related to the launch speed, v l , by…”

Section: A Analytical Treatment Of Direct Transfermentioning

confidence: 99%

“…Thus, subject to the errors of small number statistics, the Venus-Earth transfer efficiency is ∼ 4 × 10 The situation for Mars rocks is more optimistic. Estimates from Gladman 1997 andHalliday et al 1989 indicate that fifteen 100-gram Mars rocks impact the Earth each year.…”

Section: Mass Transfer From Venus and Mars To The Moonmentioning

confidence: 99%