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Coordinated X-ray, Ultraviolet, Optical, and Radio Observations of the PSR J1023+0038 System in a Low-mass X-ray Binary State | Slavko Bogdanov
; Anne M. Archibald
; Cees Bassa
; Adam Deller
; Jules P. Halpern
; George Heald
; Jason W. T. Hessels
; Gemma H. Janssen
; Andrew G.Lyne
; Javier Moldon
; Zsolt Paragi
; Alessandro Patruno
; Benetge Perera
; Ben W. Stappers
; Shriharsh P. Tendulkar
; Caroline R. D'Angelo
; Rudy Wijnands
; | Date: |
16 Dec 2014 | Abstract: | The PSR J1023+0038 binary system hosts a neutron star and a low-mass,
main-sequence-like star. It switches on year timescales between states as an
eclipsing radio millisecond pulsar and a low-mass X-ray binary. We present a
multi-wavelength observational campaign of PSR J1023+0038 in its most recent
low-mass X-ray binary state. Two long XMM-Newton observations reveal that the
system spends ~70% of the time in a ~$3 imes10^{33}$ erg/s X-ray luminosity
mode, which, as shown in Archibald et al. (2014), exhibits coherent X-ray
pulsations. This emission is interspersed with frequent lower flux mode
intervals with ~$5 imes 10^{32}$ erg/s and sporadic flares reaching up to
~$10^{34}$ erg/s, with neither mode showing significant X-ray pulsations. The
switches between the three flux modes occur on timescales of order 10 s. In the
UV and optical, we observe occasional intense flares coincident with those
observed in X-rays. Our radio timing observations reveal no pulsations at the
pulsar period during any of the three X-ray modes, presumably due to complete
quenching of the radio emission mechanism by the accretion flow. Radio imaging
detects highly variable, flat-spectrum continuum emission from PSR J1023+0038,
which likely originates in a weak jet-like outflow. Our concurrent X-ray and
radio continuum data sets do not exhibit any correlated behavior. The available
observational evidence we present bears qualitative resemblance to the behavior
predicted by some existing propeller mode and trapped disk accretion models
although none can fully account for all aspects of the rich phenomenology of
this system. | Source: | arXiv, 1412.5145 | Services: | Forum | Review | PDF | Favorites |
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