|Title||How Does the Solar Wind Drive Jupiter.s X-ray Aurora?|
|Author||Mr William Dunn|
|Description||The Juno spacecraft.s approach to Jupiter presents the opportunity to utilise simultaneous remote X-ray and in situ observations to address three fundamental open questions in X-ray and magnetospheric physics: 1) What processes at Jupiter.s magnetopause (the source for ions that generate Jupiter.s soft X-ray aurora) drive the X-ray emission? 2) What is the nature of the global interaction between Jupiter and the solar wind? 3) How does the X-ray emission connect with UV and Radio emissions? To address these long-standing questions, we propose XMM-Newton EPIC and RGS observations of Jupiter during May and June 2016 when Juno is in the solar wind and crossing the magnetopause. The next opportunity to conduct observations like these will not be until 2030.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2017-06-15T22:00:00Z, 078183, 17.56_20190403_1200. https://doi.org/10.5270/esa-68ghekv|