Year-end Sale % OFF 
Abstract
AbstractSoft X‐ray imagers can be used to study the mesoscale and macroscale density structures that occur whenever and wherever the solar wind encounters neutral atoms at comets, the Moon, and both magnetized and unmagnetized planets. Charge exchange between high charge state solar wind ions and exospheric neutrals results in the isotropic emission of soft X‐ray photons with energies from 0.1 to 2.0 keV. At Earth, this process occurs primarily within the magnetosheath and cusps. Through providing a global view, wide field‐of‐view imaging can determine the significance of the various proposed solar wind‐magnetosphere interaction mechanisms by evaluating their global extent and occurrence patterns. A summary of wide field‐of‐view (several to tens of degrees) soft X‐ray imaging is provided including slumped micropore microchannel reflectors, simulated images, and recent flight results.
Highlights
Microscale processes in magnetospheric and planetary systems often have global consequences. To fully understand these processes, one must observe them over a range of scale sizes
A statistical study of XMM-Newton observations from 0.5 to 0.7 keV found the majority of solar wind charge exchange detections to occur when the spacecraft viewed through the dayside magnetosheath [Carter et al, 2011]
The galactic sources, including diffuse emission as well as point sources, have been well characterized by the ROSAT All Sky Survey [Kuntz and Snowden, 2000; Voges et al, 1999]. These components are spatially variable, the distribution and intensity are well known and relatively constant in time, so they can be subtracted off from a magnetospheric emission that varies on short time scales (~minutes)
Summary
Microscale processes in magnetospheric and planetary systems often have global consequences. Reconnection can be initiated in the electron diffusion region spanning ~10 km at the magnetopause This microscale process changes magnetic topology, facilitating large-scale magnetospheric and ionospheric convection. Within the heliosphere, flowing plasma in the solar wind routinely encounters environments of dense neutrals surrounding comets, moons, and planets In these regions, high charge state heavy ions from the solar wind charge exchange with neutrals from the body’s exosphere. The highest fluxes of soft X-rays surrounding the Earth are emitted from regions with dense plasma of solar wind origin such as the dayside magnetosheath and the cusps. A statistical study of XMM-Newton observations from 0.5 to 0.7 keV found the majority of solar wind charge exchange detections to occur when the spacecraft viewed through the dayside magnetosheath [Carter et al, 2011]. These fronts can pass each other while propagating and can create ambiguity in interpreting time variability of the results
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
