Near IR spectra and real and imaginary indicies of refraction of ices of relevance to KBOs

Details Near IR spectra and real and imaginary indicies of refraction of ices of relevance to KBOs Near IR spectra and real and imaginary indicies of refraction of ices of relevance to KBOs

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p13c0185b&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P13C-0185

Physics

Geophysics

5205 Formation Of Stars And Planets, 5422 Ices, 6020 Ices, 6210 Comets (6023), 6224 Kuiper Belt Objects

Scientific paper

Fitting spectra of outer Solar System bodies requires lab spectra of real mixtures at appropriate temperatures because the mathematical addition of spectra of pure materials is not equivalent to those of actual mixtures, and spectra are often temperature dependant. IR spectra of outer Solar System objects are primarily in the near-IR (i.e., below 3 microns) where reflected sunlight is greatest, but there has been a dearth of near IR spectra of ice mixtures relevant to Solar System environments, and almost no indices of refraction at all. We shall present new near IR spectra and real and imaginary indicies of amorphous and crystalline H2O at various temperatures and also H2O ice mixtures. Methane (CH4) is of interest because it is present on a number of outer Solar System objects, including Triton and Pluto, KBOs Quaoar, 90377 Sedna, 2003 UB313, and FY9 and CH4 is known to be present in a number of comets. Carbon dioxide (CO2) has been observed in many comets, the Uranian satellite Ariel, Jupiter's satellites Europa, Ganymede and Callisto, Saturn's satellites Phoebe and Iapetus etc. Since H2O is nearly ubiquitous in the outer Solar System, CH4 and CO2 on icy planetesimals is likely to come into contact with H2O, potentially changing its spectral properties. So, we shall present near IR spectra of H2O-CH4 and H2O-CO2 ice mixtures at various concentrations and temperatures. For H2O-CH4 see http://www.astrochem.org/H2OCH4.html and Bernstein, Cruikshank, and Sandford, 2006 Icarus, 181, 302-308 for more information. For H2O-CO2 mixtures, see http://www.astrochem.org/CO2H2O.html and Bernstein, Cruikshank, and Sandford 2005 Icarus, 179, 527-534. This work was supported by NASA's Planetary Geology and Geophysics program (NRA-02-OSS-01-PGG).

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