Near-Infrared Spectrophotometry of Phobos and Deimos

Rivkin, A. S.

doi:10.1006/icar.2001.6767

Cited by 84 publications

(78 citation statements)

References 41 publications

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“…At longer NIR wavelengths, Rivkin et al (2000) found close agreement between >2-µm ISM spectra of Phobos and independent telescopic measurements. Erard and Calvin (1997) compared ISM data at >2.2µm with spatially overlapping Mariner IRS spectra and found close agreement at 2.2-2.6 µm.…”

Section: Radiometric Calibrationsupporting

confidence: 72%

“…ISM measurements of the martian moon Phobos were therefore used to provide continuity in radiometric calibration from the shorter wavelengths out to 3.16 µm. Phobos is well-suited for this purpose because it exhibits no evidence of absorptions in this wavelength range (Bell et al 1989, Rivkin et al 2000. For calibration purposes, the spectrum of Phobos at these wavelengths was assumed to be featureless with the low slope typical of anhydrous chondrites (Erard et al 1994).…”

Section: Radiometric Calibrationmentioning

confidence: 99%

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Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Murchie

Kirkland

Erard

et al. 2000

Icarus

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Section: Radiometric Calibrationsupporting

confidence: 72%

Section: Radiometric Calibrationmentioning

confidence: 99%

Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Murchie

Kirkland

Erard

et al. 2000

Icarus

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“…It is worth noting that while all of Deimos' surface and most of Phobos' surface had these absorptions, the areas of Phobos associated with Stickney and its ejecta have a more shallow spectral slope than the rest of Phobos and lack these absorptions, and are apparently anhydrous. Previous Earth-and space-based observations of Phobos and Deimos did not find convincing evidence for hydrated minerals (Murchie and Erard, 1996;Rivkin et al, 2002a;Gendrin et al, 2005. ) The Trojan asteroids, irregular satellites of the giant planets, and perhaps even Phobos and Deimos are thought to derive from the transneptunian object (TNO) population in Nice Model interpretations.…”

Section: Vilas Et Almentioning

confidence: 90%

Astronomical Observations of Volatiles on Asteroids

Rivkin¹,

Campins²,

Emery³

et al. 2015

Asteroids IV

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We have long known that water and hydroxyl are important components in meteorites and asteroids. However, in the time since the publication of Asteroids III, evolution of astronomical instrumentation, laboratory capabilities, and theoretical models have led to great advances in our understanding of H 2 O/OH on small bodies, and spacecraft observations of the Moon and Vesta have important implications for our interpretations of the asteroidal population. We begin this chapter with the importance of water/OH in asteroids, after which we will discuss their spectral features throughout the visible and near-infrared. We continue with an overview of the findings in meteorites and asteroids, closing with a discussion of future opportunities, the results from which we can anticipate finding in Asteroids V. Because this topic is of broad importance to asteroids, we also point to relevant in-depth discussions elsewhere in this volume.1 Water ice sublimation and processes that create, incorporate, or deliver volatiles to the asteroid belt Accretion/Solar system formation 1.1The concept of the "snow line" (also known as "water-frost line") is often used in discussing the water inventory of small bodies in our solar system. The snow line is the heliocentric distance at which water ice is stable enough to be accreted into planetesimals. The placement of the snow line has varied in different models. A location just inside Jupiter helps explain the greater mass of the giant planets as they accrete a larger fraction of the mass in the solar nebula. Although the location of the snow line before and during planet formation is uncertain, some studies show it may have fallen within the asteroid belt (Lunine, 2006). The location of the snow line in our solar system coinciding with the asteroid belt is consistent with observations of disks around other stars (e.g., Su et al., 2013), where planetesimal rings tend to coincide with the snow line around those stars. However, it seems the relatively simple concept of a static snow line requires revisions in light of new results on several fronts. For instance, the snow line likely moved with time as the Sun's luminosity changed early in solar system history (e.g., Martin and Livio, 2012). Even though there is no agreement on the details of planetesimal formation and growth, some models favor the growth of ~100 km-scale planetesimals directly from cm-scale pieces Cuzzi et al., 2010; for a dissenting view see Weidenschilling, 2011). Hence, the timing of those assemblies as conditions change could have a strong influence on the amount of radioactive elements present in a planetesimal's interior and on its rock-to-ice ratio, further complicating the concept of a snow line. Recent observations also point to a more complex picture. For example, the concept of an asteroid-comet continuum, where there is no clear boundary between primitive asteroids and cometary nuclei (e.g., Gounelle, 2011) is gaining support and is consistent with the intermittent cometary behavior of some main belt and near-E...

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“…In terms of reflectance spectrometry of their surfaces, Phobos exhibits two distinct spectral units, a 'redder' unit and a 'bluer' unit, the latter associated with the walls and ejecta of Stickney. T-type asteroids and highly space-weathered mafic mineral assemblages are the closest spectral matches to parts of the surface (Murchie and Erard, 1996;Rivkin et al, 2002). Deimos resembles a D-type asteroid.…”

Section: Scientific Backgroundmentioning

confidence: 86%

“…In addition there have been many Earth-based telescopic observations (e.g. Rivkin et al, 2002) including HST/WFPC2 (Cantor et al, 1999;Showalter et al, 2006) and radar (Ostro et al, 1989;Busch et al, 2007). …”

Section: Scientific Backgroundmentioning

confidence: 99%

Mars Phobos and Deimos Survey (M-PADS) – A martian Moons orbiter and Phobos lander

Ball

Price

Walker

et al. 2009

Advances in Space Research

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We describe a Mars 'Micro Mission' for detailed study of the martian satellites Phobos and Deimos. The mission involves two ~330 kg spacecraft equipped with solar electric propulsion to reach Mars orbit. The two spacecraft are stacked for launch: an orbiter for remote investigation of the moons and in situ studies of their environment in Mars orbit, and another carrying a lander for in situ measurements on the surface of Phobos (or alternatively Deimos). Phobos and Deimos remain only partially studied, and Deimos less well than Phobos. Mars has almost always been the primary mission objective, while the more dedicated Phobos project (1988-89) failed to realise its full potential. Many questions remain concerning the moons' origins, evolution, physical nature and composition. Current missions, such as Mars Express, are extending our knowledge of Phobos in some areas but largely neglect Deimos. The objectives of M-PADS focus on: origins and evolution, interactions with Mars, volatiles and interiors, surface features, and differences. The consequent measurement requirements imply both landed and remote sensing payloads. M-PADS is expected to accommodate a 60 kg orbital payload and a 16 kg lander payload. M-PADS resulted from a BNSC-funded study carried out in 2003 to define candidate Mars Micro Mission concepts for ESA's Aurora programme.

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Near-Infrared Spectrophotometry of Phobos and Deimos

Cited by 84 publications

References 41 publications

Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Astronomical Observations of Volatiles on Asteroids

Mars Phobos and Deimos Survey (M-PADS) – A martian Moons orbiter and Phobos lander

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