A Tentative Identification of HCN Ice on Triton

Details A Tentative Identification of HCN Ice on Triton A Tentative Identification of HCN Ice on Triton

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...718l..53b&link_type=abstract

The Astrophysical Journal Letters, Volume 718, Issue 2, pp. L53-L57 (2010).

Astronomy and Astrophysics

Astronomy

3

Planets And Satellites: Individual: Triton

Scientific paper

Spectra of Triton between 1.8 and 5.5 μm, obtained in 2007 May and 2009 November, have been analyzed to determine the global surface composition. The spectra were acquired with the grism and the prism of the Infrared Camera on board AKARI with spectral resolutions of 135 and 22, respectively. The data from 4 to 5 μm are shown in this Letter and compared to the spectra of N2, CO, and CO2, i.e., all the known ices on this moon that have distinct bands in this previously unexplored wavelength range. We report the detection of a 4σ absorption band at 4.76 μm (2101 cm-1), which we attribute tentatively to the presence of solid HCN. This is the sixth ice to be identified on Triton and an expected component of its surface because it is a precipitating photochemical product of Triton's thin N2 and CH4 atmosphere. It is also formed directly by irradiation of mixtures of N2 and CH4 ices. Here we consider only pure HCN, although it might be dissolved in N2 on the surface of Triton because of the evaporation and recondensation of N2 over its seasonal cycle. The AKARI spectrum of Triton also covers the wavelengths of the fundamental (1-0) band of β-phase N2 ice (4.296 μm, 2328 cm-1), which has never been detected in an astronomical body before, and whose presence is consistent with the overtone (2-0) band previously reported. Fundamental bands of CO and CO2 ices are also present.
This work is based on observations with AKARI, a JAXA project with the participation of ESA.

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