Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/36257
Title: Ground-based observations of Saturn's auroral ionosphere over three days: Trends in H3+ temperature, density and emission with Saturn local time and planetary period oscillation
Authors: O'Donoghue, J.
Melin, H.
Stallard, T. S.
Provan, G.
Moore, L.
Badman, S. V.
Cowley, Stanley William Herbert
Baines, K. H.
Miller, S.
Blake, J. S. D.
First Published: 29-Apr-2015
Publisher: Elsevier for Academic Press Inc.
Citation: Icarus, 2016, 263, pp. 44-55 (12)
Abstract: On 19–21 April 2013, the ground-based 10-m W.M. Keck II telescope was used to simultaneously measure View the MathML sourceH3+ emissions from four regions of Saturn’s auroral ionosphere: (1) the northern noon region of the main auroral oval; (2) the northern midnight main oval; (3) the northern polar cap and (4) the southern noon main oval. The View the MathML sourceH3+ emission from these regions was captured in the form of high resolution spectral images as the planet rotated. The results herein contain twenty-three View the MathML sourceH3+ temperatures, column densities and total emissions located in the aforementioned regions – ninety-two data points in total, spread over timescales of both hours and days. Thermospheric temperatures in the spring-time northern main oval are found to be cooler than their autumn-time southern counterparts by tens of K, consistent with the hypothesis that the total thermospheric heating rate is inversely proportional to magnetic field strength. The main oval View the MathML sourceH3+ density and emission is lower at northern midnight than it is at noon, in agreement with a nearby peak in the electron influx in the post-dawn sector and a minimum flux at midnight. Finally, when arranging the northern main oval View the MathML sourceH3+ parameters as a function of the oscillation period seen in Saturn’s magnetic field – the planetary period oscillation (PPO) phase – we see a large peak in View the MathML sourceH3+ density and emission at ∼115° northern phase, with a full-width at half-maximum (FWHM) of ∼44°. This seems to indicate that the influx of electrons associated with the PPO phase at 90° is responsible at least in part for the behavior of all View the MathML sourceH3+ parameters. A combination of the View the MathML sourceH3+ production and loss timescales and the ±10° uncertainty in the location of a given PPO phase are likely, at least in part, to be responsible for the observed peaks in View the MathML sourceH3+ density and emission occurring at a later time than the peak precipitation expected at 90° PPO phase.
DOI Link: 10.1016/j.icarus.2015.04.018
ISSN: 0019-1035
Links: http://www.sciencedirect.com/science/article/pii/S001910351500161X
http://hdl.handle.net/2381/36257
Embargo on file until: 29-Apr-2017
Version: Post-print
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2015 Elsevier Inc. All rights reserved. This manuscript version is made available after the end of the embargo period under the CC-BY-NC-ND 4.0 license http://creativecommons.org/licenses/by-nc-nd/4.0/ 
Description: The file associated with this record is under a 24-month embargo from publication in accordance with the publisher's self-archiving policy, available at https://www.elsevier.com/about/company-information/policies/sharing. The full text may be available through the publisher links provided above.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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