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Schedule Notes Viewer Vn 3.2
ESR: DXL 2022 01 09 0600 - 2022 01 09 0830
Scheduled for 0430 - 0830
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This proposal requests EISCAT time for a campaign to measure the global structure of the magnetospheric cusp. Although the community has measured the cusp in a variety of ways through in-situ rockets and spacecraft as well as through ground-based imaging and probing of the footprint, it has never before been possible to create an instantaneous three- dimensional (latitude, longitude, and altitude) global picture. It is proposed to make this global measurement through a coordinated study with the EISCAT Svalbard Radar and the NASA- funded DXL sounding rocket. Launching from Wallops Flight Facility in January 2022, the Diffuse X-rays of the Local galaxy (DXL) sounding rocket will measure emission from the high and mid-altitude cusp with soft X-rays emitted from charge-exchange. The EISCAT Svalbard Radar will provide the necessary low-altitude constraints on the morphology of the cusp footprint and convection within the ionosphere. This global picture will provide information of the true spatial extent, structure, and morphology, which in turn describes how energy and plasma is entering the magnetosphere from the solar wind. The proposed project will be a pathfinder for the ESA-SMILE mission to launch in 2024 that will be measuring the same charge-exchange X-rays from the cusps. DXL – The Diffuse X-rays from the Local galaxy (DXL) sounding rocket will measure soft X-rays within the high-altitude cusp emitted through charge exchange. Whenever and wherever high charge state solar wind ions (e.g., O+7, C+6, Mg+10, Fe+10) encounter neutrals, charge exchange occurs, resulting in the emission of soft X-rays (0.1-2keV). This process has been observed in a number of regions of space including comets [Cravens et al., 2002], the moon [Wargelin et al., 2004; Collier et al., 2014], Mars [Holmström et al., 2001; Dennerl, 2002], and Venus [Dennerl, 2008]. Now we are trying to make the same measurements around our own planet. The entire set of measurements from the rocket will be made over 5 minutes. The launch is managed by Wallops Flight Facility from the Wallops launch range during the window from January 4 to 15, 2022. The launch period is restricted based on the view angles between the cusp and the moon (>20°) and the sun (>90°). On the rocket, the X-rays will be measured through a proportional counter. The rocket payload has performed successfully on two previous flights (2012, 2015 - both from White Sands, NM) and thus ensures a high likelihood of success [previous results Thomas et al., 2013; Galeazzi et al., 2012, 2014; Collier et al., 2015]. Now we are trying to make the first coordinated observations with a ground- based radar under the polar cusp. EISCAT Svalbard Radar (ESR) will provide altitude profiles up to 600 km in real-time of the ionospheric electron density, electron temperature, ion temperature, and ion velocity along the magnetic field line under the cusp. The ESR observations will fill in the low altitude cusp that is unobservable by the sounding rocket. The ESR measurements will also provide a time-series of evolving dynamics in the cusp prior, during and after the DXL sounding rocket flight. This is a necessary feature due to the convergence of the cusp at low altitude. Since the structures will fill a smaller spatial region, a higher spatial resolution is needed to resolve them. We therefore request operation of the ESR 42 m antenna only. Our preferred experiment mode is IPY, which outputs data of both the incoherent scatter ion and plasma lines in the E and F regions. Proposing Team - The team has a broad set of expertise, designed to handle the range of observing tools and science objectives. Dr. Qudsi is an expert in solar wind-magnetosphere coupling and solar wind dynamics. Dr. Galeazzi is an X-ray astrophysicist and will coordinate the rocket launch and analysis and calibration of the DXL rocket data [Galeazzi et al., 2012]. Dr. Zou has a background in magnetosphere-ionosphere coupling through a variety of experimental tools including spacecraft, all-sky imagers, and radar systems [Zou et al., 2016]. She will participate in planning and analysis of the radar measurements. Dr. Kuntz is an expert in soft X-ray generation physics and will advise in signal generation. Lastly Dr. Walsh has background in soft X-rays and magnetospheric dynamics, focusing on the magnetopause and in the cusp [Walsh et al., 2016a; 2016b; 2017]. Prof. Oksavik has extensive experience on the polar ionosphere, including EISCAT campaigns targeted towards the cusp aurora [Oksavik et al., 2004; 2012]. He will coordinate the team and participate in data analysis. Our preferred EISCAT experiment is IPY on 42 m antenna, with both ion and plasma lines.
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