What is the nature of the X-ray emission observed in the extreme TvirgulTauri stars?Does it arise in a heavily absorbed but otherwise solar-like corona, in a thindense plasma arising from the accretion shock, or in discrete magnetosphericflaring? These emission mechanisms produce different spectral or temporalsignatures, which can be distinguished using the EPIC imagers in concert withground-based photometry and spectroscopy. If due to accretion, we expect theX-ray flux to correlate with the instantaneous mass accretion rate. Our AO4observations of RU Lupi show a clear correlation between the optical and X-raybrightness, but the interpretation is not yet clear. The result of this programwill be a better understanding of the coronae of the youngest low mass stars.
An XMM-Newton Survey of the Soft X-Ray Background. II. An All-Sky Catalog of Diffuse O VII and O VIII Emission Intensities |Henley, David B., Shelton, Robin L., | ApJS | 202-14 | 2012 | 2012ApJS..202...14H | http://ui.adsabs.harvard.edu/#abs/2012ApJS..202...14H
A systematic cross-search for radio/infrared counterparts of XMM- Newton sources |Combi, J. A., Albacete Colombo, J. F., et al. | Ap&SS | 331-53 | 2011 | 2011Ap&SS.331...53C | http://ui.adsabs.harvard.edu/#abs/2011Ap&SS.331...53C
The Solar Cycle Temporal Variation of the Solar Wind Charge Exchange X-Ray Lines |Qu, Zhijie, Koutroumpa, Dimitra, et al. | ApJ | 930-21 | 2022 | 2022ApJ...930...21Q | http://ui.adsabs.harvard.edu/#abs/2022ApJ...930...21Q
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
2007-03-21T06:48:46Z/2007-03-21T11:27:19Z
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, Prof Frederick Walter, 2008, 'X-rays from the Most Active T Tauri Stars: Accretion Shocks or Magnetic Heating', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-mh43jmt
