A dataset provided by the European Space Agency

Name: Why are millisecond pulsar magnetic fields low and how do their X-rays arise?
Published: 2009-06-10T00:00:00Z

Proposal ID	050319
Title	Why are millisecond pulsar magnetic fields low and how do their X-rays arise?
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0503190301 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0503190401
DOI	https://doi.org/10.5270/esa-0669brp
Principal Investigator, PI	Dr Natalie Webb
Abstract	Binary millisecond pulsars (MSPs) found in the field are thought to berecycled 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.
Publications	Exospheric solar wind charge exchange as seen by XMM-Newton \|Carter J. A. Semba S. \| AN \| 333-313 \| 2012 \| 2012AN....333..313C \| http://ui.adsabs.harvard.edu/#abs/2012AN....333..313C 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 The Second Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars \|Abdo A. A. Ajello M. et al. \| ApJS \| 208-17 \| 2013 \| 2013ApJS..208...17A \| http://ui.adsabs.harvard.edu/#abs/2013ApJS..208...17A Serendipitous UV source catalogues for 10 years of XMM and 5 years of Swift \|Yershov V. N. \| Ap&SS \| 354-97 \| 2014 \| 2014Ap&SS.354...97Y \| http://ui.adsabs.harvard.edu/#abs/2014Ap&SS.354...97Y 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 The Million Optical - Radio/X-ray Associations (MORX) Catalogue \|Flesch Eric W. \| PASA \| 33-52 \| 2016 \| 2016PASA...33...52F \| http://ui.adsabs.harvard.edu/#abs/2016PASA...33...52F 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 X-Ray Census of Millisecond Pulsars in the Galactic Field \|Lee Jongsu Hui C. Y. et al. \| ApJ \| 864-23 \| 2018 \| 2018ApJ...864...23L \| http://ui.adsabs.harvard.edu/#abs/2018ApJ...864...23L Classification of 4XMM-DR9 sources by machine learning \|Zhang Yanxia Zhao Yongheng \| MNRAS \| 503-5263 \| 2021 \| 2021MNRAS.503.5263Z \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.503.5263Z 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 From Active Stars to Black Holes: A Discovery Tool for Galactic X-Ray Sources \|Rodriguez Antonio C. \| PASP \| 136-054201 \| 2024 \| 2024PASP..136e4201R \| http://ui.adsabs.harvard.edu/#abs/2024PASP..136e4201R 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.
Creator Contact	https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published	2009-06-10T00:00:00Z
Last Update	2025-01-27
Keywords	"arise ?.", "magnetic field evolution", "differing models describing", "short periods", "xmm newton", "accreting pulsars", "XMM-Newton", "low msp values", "energy emission", "msp xray", "XMM", "energy emission origin"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Natalie Webb, 2009, 'Why are millisecond pulsar magnetic fields low and how do their X-rays arise?', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-0669brp