The recent detection of magnetic fields in massive stars has profoundly changedour understanding of the structure and evolution of these objects. In addition,detailed modelling shows that intense magnetic fields can have a strong impacton the X-ray emission. Currently, only a few tens of magnetic hot stars areknown, not all of them have been observed at high energies. The observeddiversity of behaviours in the few studied objects actually prevent us fromrecognizing the overall trends. By extending the sample size, we will be able toundertake such a systematic study of the X-ray properties of magnetic massivestars, which will help us better understand which parameters govern theirhigh-energy emission.
B fields in OB stars (BOB): FORS 2 spectropolarimetric follow-up of the two rare rigidly rotating magnetosphere stars HD 23478 and HD 345439 |Hubrig, S., Scholler, M., et al. | A&A | 578-3 | 2015 | 2015A&A...578L...3H | http://ui.adsabs.harvard.edu/#abs/2015A&A...578L...3H
The detection of variable radio emission from the fast rotating magnetic hot B-star HR\u00A07355 and evidence for its X-ray aurorae |Leto, P., Trigilio, C., et al. | MNRAS | 467-2820 | 2017 | 2017MNRAS.467.2820L | http://ui.adsabs.harvard.edu/#abs/2017MNRAS.467.2820L
Exploring the end states of massive stars using the X-ray emission of neutron stars and supernova remnants |Prinz, Tobias, | PhDT | 0-305 | 2013 | 2013PhDT.......305P | http://ui.adsabs.harvard.edu/#abs/2013PhDT.......305P
Discovery of extraordinary X-ray emission from magnetospheric interaction in the unique binary stellar system \\u03f5 Lupi |Das, B., Petit, V., et al. | MNRAS | 522-5805 | 2023 | 2023MNRAS.522.5805D | http://ui.adsabs.harvard.edu/#abs/2023MNRAS.522.5805D
Discovery of magnetospheric interactions in the doubly magnetic hot binary \\u03f5 Lupi |Biswas, Ayan, Das, Barnali, et al. | MNRAS | 523-5155 | 2023 | 2023MNRAS.523.5155B | http://ui.adsabs.harvard.edu/#abs/2023MNRAS.523.5155B
The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII, O VIII, and Fe L-shell Transitions |Pan, Zeyang, Qu, Zhijie, et al. | ApJS | 271-62 | 2024 | 2024ApJS..271...62P | http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P
Robust constraints on feebly interacting particles using XMM-Newton |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-L101305 | 2024 | 2024PhRvD.109j1305L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L
Multimessenger search for electrophilic feebly interacting particles from supernovae |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-103028 | 2024 | 2024PhRvD.109j3028L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L
Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints |De la Torre Luque, Pedro, Balaji, Shyam, | ApJ | 968-46 | 2024 | 2024ApJ...968...46D | http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2012-08-10T23:04:55Z/2013-03-05T01:12:21Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Dr Yael Naze, 2014, 'Characterizing the X-ray properties of the earliest magnetic stars', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-7gbs3b9
