Modeled ENA Maps from SHIELD – if utilizing results, please reference the SHIELD Drive Center as well as the original work from which the figures are derived.
ENA sky maps of flux centered on the downwind (tail) direction in units
of 1/(cm^2 s sr keV) for the BU model (left), Moscow model (middle), and IBEX-Hi GDF from the first five years (2009-2013) of observations (right). The BU model is based on the works of Opher et al. (2015) and Michael et al. (2022) and uses a kinetic-MHD model to simulate a short-tail heliosphere. The Moscow model is based on the works of Izmodenov & Alexashov (2015, 2020) and uses a kinetic-MHD model to simulate a long-tail heliosphere. In this figure, the ENA energy band is increasing from top to bottom. The ENA maps have a resolution of 6 deg. x 6 deg. in latitude and longitude. Simulated sky maps do not use any scaling factor. This figure shows that utilizing three PUI populations, including one accelerated via diffusive shock acceleration at the termination shock, can provide good quantiative agreement with IBEX-Hi observations.
Figure credit: Kornbleuth et al. (2023)
ENA sky maps of flux centered on the downwind (tail) direction in units
of 1/(cm^2 s sr keV) for the BU model (left), Moscow model (middle), and INCA
observations averaged over the years 2009-2012 (right). The BU model is based on the works of Opher et al. (2015) and Michael et al. (2022) and uses a kinetic-MHD model to simulate a short-tail heliosphere. The Moscow model is based on the works of Izmodenov & Alexashov (2015, 2020) and uses a kinetic-MHD model to simulate a long-tail heliosphere. In this figure, the ENA energy band is increasing from top to bottom. The ENA maps have a resolution of 6 deg. x 6 deg. in latitude and longitude. The dark blue region in the INCA observations correlates with data gaps related to ENA contamination from Saturn’s magnetosphere. The shaded regions indicate regions with low statistics due to limited viewing time. From top to bottom, the simulated sky maps are scaled up using a scaling factor of 7.5, 3.0, 1.5, and 1.2, respectively. This figure shows the energy gap between modeled and observed ENA maps at high energies (~5-55 keV), which indicates a source of energy-dependent PUI acceleration in the heliosheath, absent from the included ENA model.
Figure credit: Kornbleuth et al. (2023)
Simulated ENA sky maps of flux centered on the downwind (tail) direction
in units of 1/(cm^2 s sr keV) for the BU model (left) and Moscow model (right) at the 80 keV energy band. The BU model is based on the works of Opher et al. (2015) and Michael et al. (2022) and uses a kinetic-MHD model to simulate a short-tail heliosphere. The Moscow models is based on the works of Izmodenov & Alexashov (2015, 2020) and uses a kinetic-MHD model to simulate a long-tail heliosphere.The simulated maps have a resolution of 4 deg. x 4 deg. in latitude and longitude. This figure indicates that at approximately 80 keV, which will be energy observable by IMAP-Ultra, the heliotail length can potentially be distinguished.
Figure credit: Kornbleuth et al. (2023)