|Title||Stellar Cycle Sampling: the X-Ray Expansion|
|Author||Dr Bradford Wargelin|
|Description||Within the past two years, the number of M stars known to have stellar cycles has grown from a handful to a few dozen, including several fully convective stars which, it was generally believed, are not capable of supporting magnetic cycles. And of the hundreds of stars with cycles, only seven have been monitored in X rays (one of them a late M stars), but their results tentatively point toward a surprisingly simple relationship between X-ray cycle amplitude and Rossby number (Ro). These observational discoveries have occurred at the same time as significant advances in theoretical models, some of which predict that fully convective stars CAN sustain cycles. We request observations of four stars that span a wide range of Ro and spectral type and will expand the X-ray perspective.|
|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, 2020-05-24T22:00:00Z, 082279, 19.17_20220121_1250. https://doi.org/10.5270/esa-jcpt375|