|Title||Testing Models for Stellar Magnetic Dynamos with Slow Rotators in Praesepe|
|Author||Dr Alejandro Nunez|
|Description||In solar-type stars, rotational shear at the tachocline is thought to power a dynamo, generating a magnetic field that heats the star.s corona, which produces X-rays. X-ray flux and rotation rates measurements therefore provide insight into the strength of the underlying magnetic field and its dependence on rotation. But this rotation-activity relation remains unconstrained for the slowest rotators (i.e., Rossby number > 0.8). We propose to observe six 700-Myr-old solar-type slowly rotating Praesepe stars, for a total of 157 ks of exposure with the EPIC camera. Our data will provide invaluable information on the rotation-activity relation for the slow rotators, enabling tests of dynamo theory in a largely unconstrained regime.|
|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, 2022-05-18T00:00:00Z, 086371, 19.16_20210326_1200. https://doi.org/esa-[xxxxxxx]|