|Title||The late-outburst X-ray emission of the magnetar Swift J1818.0-1607|
|Author||Dr George Younes|
|Description||Swift J1818.0-1607 is a radio-loud magnetar that went into outburst in 2020 March. Its spin period of 1.36 s and its derivative imply a field strength of 4e14 G, a very young age virgul500 years, and a spin down power of 1e36 erg-s, the largest by far among all magnetars, rivaling those of rotation-powered pulsars (RPPs). Hence Swift J1818.0-1607 may represent the ultimate link between the two populations. The source has not reached quiescence yet. Hence, we propose a late-time monitoring campaign to establish its long-term decay trend, reveal the late-time surface thermal pulse shape and pulsed fraction, and derive the radio-X-ray pulse offset and compare it to the early stages of the outburst, all crucial elements to place this unique source within the large family of magnetars and RPPs.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN|
|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, 2022-05-04T00:00:00Z, 090318, 19.17_20220121_1250. https://doi.org/esa-[xxxxxxx]|