Crystalline water ice on the Kuiper belt object (50000) Quaoar

Nature ◽  
2004 ◽  
Vol 432 (7018) ◽  
pp. 731-733 ◽  
Author(s):  
David C. Jewitt ◽  
Jane Luu
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
Water Ice ◽  
Crystalline Water

scholarly journals Water Ice on the Satellite of Kuiper Belt Object 2003 EL 61

2006 ◽  
Vol 640 (1) ◽  
pp. L87-L89 ◽  
Author(s):  
K. M Barkume ◽  
M. E. Brown ◽  
E. L. Schaller
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
Water Ice

Water Ice on Kuiper Belt Object 1996 TO[TINF]66[/TINF]

1999 ◽  
Vol 519 (1) ◽  
pp. L101-L104 ◽  
Author(s):  
Robert H. Brown ◽  
Dale P. Cruikshank ◽  
Yvonne Pendleton
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
Water Ice

scholarly journals Silicate and ice emission bands in the ISO spectrum of the PAH-emitting carbon-rich planetary nebula CPD-56°8032

1999 ◽  
Vol 191 ◽  
pp. 291-296
Author(s):  
Martin Cohen ◽  
M. J. Barlow ◽  
R. J. Sylvester ◽  
X.-W. Liu ◽  
P. Cox ◽  
...  
Keyword(s):  
Polycyclic Aromatic Hydrocarbons ◽  
Aromatic Hydrocarbons ◽  
Planetary Nebula ◽  
Kuiper Belt ◽  
Simultaneous Presence ◽  
Water Ice ◽  
Polycyclic Aromatic ◽  
Crystalline Water ◽  
History Of ◽  
Bright Emission

Combined ISO SWS and LWS spectroscopy is presented of the late WC-type planetary nebula nucleus CPD-56†8032 and its carbon-rich nebula. The extremely broad coverage (2.4–197 μm) enables us to recognize the clear and simultaneous presence of emission features from both oxygen- and carbon-rich circumstellar materials. Removing a smooth continuum highlights bright emission bands characteristic of polycyclic aromatic hydrocarbons (hereafter PAHs) in the 3–15 μm region, bands from crystalline silicates longwards of 18 μm, and the 43- and 62-μm bands of crystalline water ice. We discuss the probable evolutionary state and history of this unusual object in terms of (a) a recent transition from an O-rich to a C-rich outflow following a helium shell flash; or (b) a carbon-rich nebular outflow encountering an O-rich comet cloud orbiting in a Kuiper-belt-like distribution.

Discovery of the candidate Kuiper belt object 1992 QB1

Nature ◽  
1993 ◽  
Vol 362 (6422) ◽  
pp. 730-732 ◽  
Author(s):  
David Jewitt ◽  
Jane Luu
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object

scholarly journals Photometry of Kuiper belt object (486958) Arrokoth from New Horizons LORRI

Icarus ◽  
2021 ◽  
Vol 356 ◽  
pp. 113723 ◽  
Author(s):  
Jason D. Hofgartner ◽  
Bonnie J. Buratti ◽  
Susan D. Benecchi ◽  
Ross A. Beyer ◽  
Andrew Cheng ◽  
...  
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
New Horizons

scholarly journals Thermal desorption of formamide and methylamine from graphite and amorphous water ice surfaces

2019 ◽  
Vol 15 (S350) ◽  
pp. 370-371
Author(s):  
Henda Chaabouni ◽  
Stephan Diana ◽  
Thanh Nguyen
Keyword(s):  
Energy Distribution ◽  
Thermal Desorption ◽  
Interstellar Dust ◽  
Binding Energies ◽  
Desorption Energy ◽  
Exponential Factor ◽  
Water Ice ◽  
Ice Surface ◽  
Crystalline Water ◽  
Best Fit

AbstractThermal desorption experiments of Formamide (NH2CHO) and methylamine (CH3NH2) were performed in LERMA-Cergy laboratory to determine the values of the desorption energies of formamide and methylamine from analogues of interstellar dust grain surfaces, and to understand their interaction with water ice. We found that more than 95 % of solid NH2CHO diffuses through the np-ASW ice surface towards the graphitic substrate, and is released into the gas phase with a desorption energy distribution Edes = (7460 – 9380) K, measured with the best-fit pre-exponential factor A=1018 s-1. Whereas, the desorption energy distribution of methylamine from the np-ASW ice surface (Edes =3850-8420 K) is measured with the best-fit pre-exponential factor A=1012s-1. A fraction of solid methylamine, of about 0.15 monolayer diffuses through the water ice surface towards the HOPG substrate, and desorbs later, with higher binding energies (5050-8420 K), which exceed that of the crystalline water ice (Edes =4930 K), calculated with the same pre-exponential factor A=1012 s-1.

Reflection Spectrum of the Kuiper Belt Object 1993 SC

1996 ◽  
Vol 111 ◽  
pp. 499 ◽  
Author(s):  
Jane X. Luu ◽  
David C. Jewitt
Keyword(s):  
Reflection Spectrum ◽  
Kuiper Belt ◽  
Kuiper Belt Object

scholarly journals Ceres’ partial differentiation: undifferentiated crust mixing with a water-rich mantle

2020 ◽  
Vol 633 ◽  
pp. A117 ◽  
Author(s):  
Wladimir Neumann ◽  
Ralf Jaumann ◽  
Julie Castillo-Rogez ◽  
Carol A. Raymond ◽  
Christopher T. Russell
Keyword(s):  
Thermal Evolution ◽  
Kuiper Belt ◽  
Radioactive Decay ◽  
Thermal Conditions ◽  
Asteroid Belt ◽  
Final Size ◽  
Water Ice ◽  
Modeled Structure ◽  
Internal States ◽  
And Migration

Aims. We model thermal evolution and water-rock differentiation of small ice-rock objects that accreted at different heliocentric distances, while also considering migration into the asteroid belt for Ceres. We investigate how water-rock separation and various cooling processes influence Ceres’ structure and its thermal conditions at present. We also draw conclusions about the presence of liquids and the possibility of cryovolcanism. Methods. We calculated energy balance in bodies heated by radioactive decay and compaction-driven water-rock separation in a three-component dust-water/ice-empty pores mixture, while also taking into consideration second-order processes, such as accretional heating, hydrothermal circulation, and ocean or ice convection. Calculations were performed for varying accretion duration, final size, surface temperature, and dust/ice ratio to survey the range of possible internal states for precursors of Ceres. Subsequently, the evolution of Ceres was considered in five sets of simulated models, covering different accretion and evolution orbits and dust/ice ratios. Results. We find that Ceres’ precursors in the inner solar system could have been both wet and dry, while in the Kuiper belt, they retain the bulk of their water content. For plausible accretion scenarios, a thick primordial crust may be retained over several Gyr, following a slow differentiation within a few hundreds of Myr, assuming an absence of destabilizing impacts. The resulting thermal conditions at present allow for various salt solutions at depths of ≲10 km. The warmest present subsurface is obtained for an accretion in the Kuiper belt and migration to the present orbit. Conclusions. Our results indicate that Ceres’ material could have been aqueously altered on small precursors. The modeled structure of Ceres suggests that a liquid layer could still be present between the crust and the core, which is consistent with Dawn observations and, thus, suggests accretion in the Kuiper belt. While the crust stability calculations indicate crust retention, the convection analysis and interior evolution imply that the crust could still be evolving.

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