C. A. O. de l'implantation optimale de programmes de commande

Dumas, Jean-Michel; Prunet, F.

doi:10.1007/bfb0004089

Cited by 5 publications

(10 citation statements)

References 2 publications

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“…Those Eris measurements challenged previous work including our own that had concluded nitrogen was a minority species rather than a majority species (Brown, Trujillo, & Rabinowitz 2005;Dumas et al 2007;Abernathy et al 2009;Merlin et al 2009). That conclusion rested on two observations.…”

Section: Introductionmentioning

confidence: 73%

“…In the lower part of Figure 7, we plot the 1.72 µm methane band in a spectrum of Eris (Dumas et al 2007) (black line) and the best fit Hapke model that includes the two methane phases and an overall bulk abundance of 8% methane and 92% nitrogen (red line).…”

Section: Modelmentioning

confidence: 99%

“…As for Eris, we are limited by the fact we do not know the sub-Earth longitudes corresponding to the optical (Tegler et al 2010) and near-infrared (Dumas et al 2007) spectra. If we assume homogeneity across the surface or a nearly pole-on viewing geometry, then Table 5 suggests Eris too exhibits no evidence of a change in the mixing ratio with depth.…”

Section: Stratigraphymentioning

confidence: 99%

“…Triton bands are narrower and blue shifted compared to the Pluto bands due to most of the methane being in nitrogen-rich crystals, there is no measurable difference between the two Triton band profiles. In the lower part of the plot, we show the 1.72 µm band in Eris' spectrum (Dumas et al 2007). Its minimum is closest to pure methane because it has the largest amount of methane in methane-rich crystals of the three icy dwarf planets.…”

Section: Future Workmentioning

confidence: 99%

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Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

Tegler

Grundy

Olkin

et al. 2012

ApJ

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Received; accepted 1 Visiting Astronomer, MMT Observatory. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution 2 Visiting Astronomer, NASA IRTF -3 - ABSTRACTWe present three near-infrared spectra of Pluto taken with the IRTF and SpeX, an optical spectrum of Triton taken with the MMT and the Red Channel Spectrograph, and previously published spectra of Pluto, Triton, and Eris. We combine these observations with a two-phase Hapke model, and gain insight into the ice mineralogy on Pluto, Triton, and Eris. Specifically, we measure the methane-nitrogen mixing ratio across and into the surfaces of these icy dwarf planets. In addition, we present a laboratory experiment that demonstrates it is essential to model methane bands in spectra of icy dwarf planets with two methane phases − one highly-diluted by nitrogen and the other rich in methane.For Pluto, we find bulk, hemisphere-averaged, methane abundances of 9.1 ± 0.5%, 7.1 ± 0.4%, and 8.2 ± 0.3% for sub-Earth longitudes of 10 • , 125 • , and 257 • . Application of the Wilcoxon rank sum test to our measurements finds these small differences are statistically significant. For Triton, we find bulk, hemisphere-averaged, methane abundances of 5.0 ± 0.1% and 5.3 ± 0.4% for sub-Earth longitudes of 138 • and 314 • . Application of the Wilcoxon rank sum test to our measurements finds the differences are not statistically significant.For Eris, we find a bulk, hemisphere-averaged, methane abundance of 10 ± 2%.Pluto, Triton, and Eris do not exhibit a trend in methane-nitrogen mixing ratio with depth into their surfaces over the few cm range probed by these obser- vations. This result is contrary to the expectation (Grundy & Stansberry 2000)that since visible light penetrates deeper into a nitrogen-rich surface than the depths from which thermal emission emerges, net radiative heating at depth would drive preferential sublimation of nitrogen leading to an increase in the methane abundance with depth.

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Section: Introductionmentioning

confidence: 73%

Section: Modelmentioning

confidence: 99%

Section: Stratigraphymentioning

confidence: 99%

Section: Future Workmentioning

confidence: 99%

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Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

Tegler

Grundy

Olkin

et al. 2012

ApJ

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“…S-type here refers to spectra consistent with the S-complex of taxonomic types rather than the specific S-type. Solars were chosen from 1 Hardorp (1978), 2 Landolt (1992), 3 Colina & Bohlin (1997), and 4 Dumas et al (2007).…”

mentioning

confidence: 99%

AVAST survey 0.4–1.0 μm spectroscopy of igneous asteroids in the inner and middle main belt

Solontoi

Hammergren

Gyuk

et al. 2012

Icarus

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We present the spectra of 60 asteroids, including 47 V-types observed during the first phase of the Adler V-Type Asteroid (AVAST) Survey. SDSS photometry was used to select candidate V-type asteroids for follow up by nature of their very blue i − z color. 47 of the 61 observed candidates were positively classified as V-type asteroids, while an additional six show indications of a 0.9 µm feature consistent with V-type spectra, but not sufficient for formal classification. Four asteroids were found to be S-type, all of which had i − z values very near the adopted AVAST selection criteria of i − z ≤ −0.2, including one candidate observed well outside the cut (at a mean i − z of -0.11). Three A-type asteroids were also identified. Six V-type asteroids were observed beyond the 3:1 mean motion resonance with Jupiter, including the identification of two new V-type asteroids (63085 and 105041) at this distance. Six V-type asteroids were observed with low (< 5 deg) orbital inclination, outside of the normal dynamical range of classic Vestoids, and are suggestive of a non-Vesta origin for at least some of the population.

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THE YOUTHFUL APPEARANCE OF THE 2003 EL₆₁COLLISIONAL FAMILY

Rabinowitz

Schaefer

et al. 2008

The Astronomical Journal

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We present new solar phase curve observations of the 2003 EL 61 collisional family showing that all the members have light-scattering properties similar to the bright icy satellites and dwarf planets. Compared to other Kuiper Belt objects, the five family members we observe (2003 EL 61 , 2002 TX 300 , 2003 OP 32 , 2005 , and 1995 SM 55 ) have conspicuously neutral color (V-I = 0.6-0.8 mag) and flat phase curves at small phase angles (phase coefficients of 0.0 -0.1 mag deg -1 ). Comparing the phase curves we observe for other icy Kuiper Belt objects to the phase curves of icy satellites, we find that the flat phase curves of the 2003 EL 61 family are an indication they have high albedo surfaces coated with fresh ice in the last ~100 Myr. We examine possible resurfacing processes and find none that are plausible. To avoid the influence of cosmic radiation that darkens and reddens most icy surfaces on times scales > ~100 Myr, the family members must be unusually depleted in carbon, or else the collision that created the family occurred so recently that the parent body and fragments have not had time to darken. We also find a rotation period of 4.845 (+/-0.003) h with amplitude 0.26 (+/-0.04) mags for 2003 OP 32 .

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C. A. O. de l'implantation optimale de programmes de commande

Cited by 5 publications

References 2 publications

Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

AVAST survey 0.4–1.0 μm spectroscopy of igneous asteroids in the inner and middle main belt

THE YOUTHFUL APPEARANCE OF THE 2003 EL₆₁COLLISIONAL FAMILY

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C. A. O. de l'implantation optimale de programmes de commande

Cited by 5 publications

References 2 publications

Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

Ice Mineralogy Across and Into the Surfaces of Pluto, Triton, and Eris

AVAST survey 0.4–1.0 μm spectroscopy of igneous asteroids in the inner and middle main belt

THE YOUTHFUL APPEARANCE OF THE 2003 EL61COLLISIONAL FAMILY

Contact Info

Product

Resources

About

THE YOUTHFUL APPEARANCE OF THE 2003 EL₆₁COLLISIONAL FAMILY