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Ionization Processes in the Atmosphere of Titan (Research Note). III. Ionization by High-Z Nuclei Cosmic RaysContext. The Cassini-Huygens mission has revealed the importance of particle precipitation in the atmosphere of Titan thanks to in-situ measurements. These ionizing particles (electrons, protons, and cosmic rays) have a strong impact on the chemistry, hence must be modeled. Aims. We revisit our computation of ionization in the atmosphere of Titan by cosmic rays. The high-energy high-mass ions are taken into account to improve the precision of the calculation of the ion production profile. Methods. The Badhwahr and O Neill model for cosmic ray spectrum was adapted for the Titan model. We used the TransTitan model coupled with the Planetocosmics model to compute the ion production by cosmic rays. We compared the results with the NAIRAS/HZETRN ionization model used for the first time for a body that differs from the Earth. Results. The cosmic ray ionization is computed for five groups of cosmic rays, depending on their charge and mass: protons, alpha, Z = 8 (oxygen), Z = 14 (silicon), and Z = 26 (iron) nucleus. Protons and alpha particles ionize mainly at 65 km altitude, while the higher mass nucleons ionize at higher altitudes. Nevertheless, the ionization at higher altitude is insufficient to obscure the impact of Saturn s magnetosphere protons at a 500 km altitude. The ionization rate at the peak (altitude: 65 km, for all the different conditions) lies between 30 and 40/cu cm/s. Conclusions. These new computations show for the first time the importance of high Z cosmic rays on the ionization of the Titan atmosphere. The updated full ionization profile shape does not differ significantly from that found in our previous calculations (Paper I: Gronoff et al. 2009, 506, 955) but undergoes a strong increase in intensity below an altitude of 400 km, especially between 200 and 400 km altitude where alpha and heavier particles (in the cosmic ray spectrum) are responsible for 40% of the ionization. The comparison of several models of ionization and cosmic ray spectra (in intensity and composition) reassures us about the stability of the altitude of the ionization peak (65 km altitude) with respect to the solar activity.
Document ID
20110016358
Document Type
Reprint (Version printed in journal)
Authors
Gronoff, G. (NASA Langley Research Center Hampton, VA, United States)
Mertens, C. (NASA Langley Research Center Hampton, VA, United States)
Lilensten, J. (Grenoble-1 Univ. France)
Desorgher, L. (Bern Univ. Bern, Switzerland)
Fluckiger, E. (Bern Univ. Bern, Switzerland)
Velinov, P. (Bulgarian Academy of Sciences Sofia, Bulgaria)
Date Acquired
August 25, 2013
Publication Date
May 1, 2011
Publication Information
Publication: Journal of Astronomy and Astrophysics
Volume: 529
Subject Category
Astronomy
Report/Patent Number
NF1676L-13565
Funding Number(s)
CONTRACT_GRANT: No. 228319
WBS: WBS 389018.02.15.02.94
CONTRACT_GRANT: Swiss NSF 200020/113704
CONTRACT_GRANT: COST-724/C05.0034
Distribution Limits
Public
Copyright
Other