|Title||Disruption of coronal activity due to a massive hot Jupiter.|
|Author||Dr Ignazio Pillitteri|
|Description||In the young system of WASP-18 the coronal emission is almost two orders of magnitude lower than expected for a star of its spectral type (F6) and age ( 800 Myr). The puzzling behavior could be explained as due to tidal interaction with its very massive hot Jupiter (10 M J ) that prevents the formation of a magnetic dynamo in the shallow convective zone of the star and of thus of the corona. Here we want to observe the system of KELT-24 which is very similar to WASP-18. It is formed by an F5 star orbited by a massive hot Jupiter every 5 days. A measurement of its X-ray flux and luminosity derived from a 25 ks XMM-EPIC exposure can tell us if KELT-24 behaves like a young F type star of Hyades or if its X-ray activity is quenched by the interaction with its 5 M_J hot Jupiter.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, 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, 2021-05-28T00:00:00Z, 086156, 18.02_20200221_1200. https://doi.org/esa-[xxxxxxx]|