4U 0142+61 is a 8.7-s anomalous X-ray pulsar which, in data from our RXTEmonitoring program, shows pulsations that are slowly but steadily gettingbrighter. Since 2000, the pulses have brightened by approximately 50%. Inconcert with the brightening, the pulse profile is clearly evolving on acomparable time scale. This behavior is unprecedented for an AXP and challengesthe current magnetar model. We request two XMM observations of the source inCycle 5 in order to monitor its phase-averaged flux and its spectrum, to try toshed light on the physical origin of this behavior.
Publications
Long-term X-ray Changes in the Emission from the Anomalous X-ray Pulsar 4U 0142+61 |Gonzalez, M. E., Dib, R., et al. | ApJ | 716-1345 | 2010 | 2010ApJ...716.1345G | http://ui.adsabs.harvard.edu/#abs/2010ApJ...716.1345G
The XMM Cluster Survey: optical analysis methodology and the first data release |Mehrtens, Nicola, Romer, A. Kathy, et al. | MNRAS | 423-1024 | 2012 | 2012MNRAS.423.1024M | http://ui.adsabs.harvard.edu/#abs/2012MNRAS.423.1024M
Phase-resolved X-Ray Spectra of Magnetars and the Coronal Outflow Model |Hascoet, Romain, Beloborodov, Andrei M., | ApJ | 786-1 | 2014 | 2014ApJ...786L...1H | http://ui.adsabs.harvard.edu/#abs/2014ApJ...786L...1H
Sunyaev-Zel.dovich effect or not? Detecting the main foreground effect of most galaxy clusters |Xiao, Weike, Chen, Chen, et al. | MNRAS | 432-41 | 2013 | 2013MNRAS.432L..41X | http://ui.adsabs.harvard.edu/#abs/2013MNRAS.432L..41X
Chandra Follow-up of the SDSS DR8 Redmapper Catalog Using the MATCha Pipeline |Hollowood, Devon L., Jeltema, Tesla, et al. | ApJS | 244-22 | 2019 | 2019ApJS..244...22H | http://ui.adsabs.harvard.edu/#abs/2019ApJS..244...22H
Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters |Palmese, A., Annis, J., et al. | MNRAS | 493-4591 | 2020 | 2020MNRAS.493.4591P | http://ui.adsabs.harvard.edu/#abs/2020MNRAS.493.4591P
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
2006-07-28T17:45:03Z/2007-01-13T21:46:00Z
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 Victoria Kaspi, 2008, 'XMM Monitoring of the Evolving AXP 4U 0142+61', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-q30d7hi
