|Title||Covering one Full Orbit of RZ Cas with XMM-Newton|
|Author||Mr Marc Audard|
|Description||We propose to observe the eclipsing Algol-type system RZ Cas with XMM-Newton. Simultaneous observations with the radio VLA will be requested. Thanks to its short rotational and orbital period (P = 1.195d), a 110 ksec observation will cover the whole binary phase. We will address the following issues: i) the eclipse of the late-type component (K3IV) by the non-magnetic primary (A3V) will be monitored in the X-ray and radio ranges, allowing us to reconstruct and compare the geometry of the corona of the magnetically active star in the thermal and non-thermal regimes; ii) signatures for accretion flow material will be looked for, in particular an excess absorption column density; iii) the primary eclipse will provide constraints on the emission from the A star.|
|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, 2004-09-28T00:00:00Z, 014904, 17.56_20190403_1200. https://doi.org/10.5270/esa-4u0q99v|