Observability of Callisto’s exosphere with MAJIS/JUICE

Abstract

<p>The most direct evidence that the icy Galilean satellite Callisto is able to sustain a significant neutral exosphere dates back to the detection of the CO<sub>2</sub> non-LTE emission at 4.3 μm wavelength, measured by the NIMS instrument onboard the NASA Galileo spacecraft [1]. Other exospheric emissions have been observed in the UV spectral range, basically tracing the ionised exospheric component ([2], [3]). The analysis of such emissions in the framework of exospheric models (see e.g. [4], [5]) allowed to establish an overall composition dominated by O<sub>2</sub> and H<sub>2</sub>O, with minor contributions by CO<sub>2</sub> and CO. However, direct observations of neutral species other than CO<sub>2</sub> are still missing, and their actual abundances, as well as spatial and temporal variability, are poorly constrained.</p> <p>The MAJIS (<em>Moon And Jupiter Imaging Spectrometer</em>, [6]) instrument, on board the ESA JUICE spacecraft, is expected to contribute in this field, by searching for non-LTE emissions falling in its spectral range, from 0.50 to 5.54 μm. In particular, we evaluate the chance of detection of signals at the satellite’s limb emitted by the CO<sub>2</sub> complexes at 4.3 μm and 2.3 μm, by the H<sub>2</sub>O complex at 2.3 μm, by O<sub>2</sub> at 1.27 μm, and by the CO bands at 4.7 μm and 2.3 μm. We calculate the populations of molecular levels by using the GRANADA algorithm [7], then the emissions intensities, for reference abundances of the molecular species and for limb-viewing geometry, by taking advantage of the KOPRA algorithm [8].</p> <p>Detection limits for all the abovementioned species are obtained in the approximation of horizontal uniformity of exospheric layers and adopting a vertical scaling compatible with the scale height in [1]. Surface density detection limits around 6.2 <sup>.</sup>10<sup>6</sup> cm<sup>-3</sup>, 6.6 <sup>.</sup>10<sup>6</sup> cm<sup>-3</sup>, 3.4 <sup>.</sup>10<sup>9</sup> cm<sup>-3</sup>, 3.4 <sup>.</sup>10<sup>7</sup> cm<sup>-3</sup> are found for CO<sub>2</sub>, H<sub>2</sub>O, O<sub>2</sub>, and CO respectively. For both CO<sub>2</sub> and H<sub>2</sub>O, these results indicate a high detection probability during the Callisto flybys planned in the current JUICE trajectory version (crema 5.0, [9]). Detection of O<sub>2</sub> could also be possible if appropriate observing strategies are adopted. Detection of CO is instead very challenging, being its expected abundance well below the detection limit.</p> <p><strong> </strong><strong>Acknowledgements</strong></p> <p>This work is supported by the Italian Space Agency (ASI-INAF grant 2018-25-HH.0). IAA researchers acknowledge financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (CEX2021-001131-S/fund by MICIN/AEI/10.13039/501100011033).</p> <p><strong>References</strong></p> <p><strong>[1]</strong> Carlson,R.W.,1999, <em>Science</em> 283 (5403): 820–21. <strong>[2]</strong> Kliore,A.J., 2002, <em>Journ.Geophys.Res</em>. doi: 10.1029/2002ja009365. <strong>[3] </strong>Cunningham,N.J. et al., 2015, <em>Icarus</em>. doi:10.1016/j.icarus.2015.03.021. <strong>[4]</strong> Vorburger,A., et al., 2015, <em>Icarus</em>. doi:10.1016/j.icarus.2015.07.035. <strong>[5]</strong> Liang, M., 2005, <em>Journ.Geophys.Res</em>. doi:10.1029/2004je002322. <strong>[6]</strong> Guerri I., et al., 2018, Proc.of SPIE Vol.10690 106901L-1. doi: 10.1117/12.2312013.<strong> [7] </strong>Funke,B., et al., 2012, <em>Journ.Quant.Sp.Rad.Tran</em>. doi:10.1016/j.jqsrt.2012.05.001. <strong>[8] </strong>Stiller,G.P., et al., 2002. <em>Journ.Quant.Sp.Rad.Tran</em>. doi:10.1016/s0022-4073(01)00123-6. <strong>[9]</strong> ESA SPICE Service, JUICE Operational SPICE Kernel Dataset, doi:10.5270/esa-ybmj68p.</p>