Binary millisecond pulsars (MSPs) found in the field are thought to be.recycled. from accreting pulsars. These MSPs have short periods, low spindownrates (Pdot) and consequently low surface magnetic fields (Bs) as Bs isproportional to (Pdot P)^0.5. It is unclear, however, how the MSP surfacemagnetic field can evolve from the high fields observed in pulsars to the lowMSP values. Two models have been proposed to explain this. Also, the origin ofthe high energy emission is unclear as too few MSP X-ray observations have beenmade to differentiate between competing models. With these XMM-Newtonobservations of four MSPs previously unobserved in X-rays, we will discriminatebetween differing models describing the magnetic field evolution and the high energy emission origin.
Six millisecond pulsars detected by the Fermi Large Area Telescope and the radio/gamma-ray connection of millisecond pulsars |Espinoza, C. M., Guillemot, L., et al. | MNRAS | 430-571 | 2013 | 2013MNRAS.430..571E | http://ui.adsabs.harvard.edu/#abs/2013MNRAS.430..571E
Revealing the broad iron Kalpha line in Cygnus X-1 through simultaneous XMM-Newton, RXTE, and INTEGRAL observations |Duro, Refiz, Dauser, Thomas, et al. | A&A | 589-14 | 2016 | 2016A&A...589A..14D | http://ui.adsabs.harvard.edu/#abs/2016A&A...589A..14D
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
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
2008-02-17T10:05:04Z/2008-04-20T20:32:30Z
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 Natalie Webb, 2009, 'Why are millisecond pulsar magnetic fields low and how do their X-rays arisequestionMark', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-0669brp
