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http://hdl.handle.net/20.500.12386/24740
Titolo: | A Deep Campaign to Characterize the Synchronous Radio/X-Ray Mode Switching of PSR B0943+10 | Autori: | MEREGHETTI, Sandro Kuiper, L. Tiengo, A. Hessels, J. Hermsen, W. Stovall, K. POSSENTI, ANDREA Rankin, J. Esposito, P. Turolla, R. Mitra, D. Wright, G. Stappers, B. Horneffer, A. Oslowski, S. Serylak, M. Grießmeier, J. -M. |
Data pubblicazione: | 2016 | Rivista: | THE ASTROPHYSICAL JOURNAL | Numero: | 831 | Fascicolo: | 1 | Da pagina:: | 21 | Abstract: | Observations of PSR B0943+10 with XMM-Newton and the LOFAR, LWA, and Arecibo radio telescopes in 2014 November confirm the synchronous X-ray/radio switching between a radio-bright (B) mode and a radio-quiet (Q) mode, in which the X-ray flux is a factor ∼2.4 higher than in the B-mode. We discovered X-ray pulsations during the B-mode (0.5-2 keV pulsed fraction of (38 ± 5)%) and confirm their presence in the Q-mode, where the pulsed fraction increases with energy from ∼20% to ∼65% at 2 keV. We found marginal evidence for an increase in the X-ray pulsed fraction during the B-mode on a timescale of hours. The X-ray spectrum during the Q-mode requires a fit with either a power law plus blackbody or the sum of two blackbodies, while in the B-mode it is well fit by a single blackbody (a single power law is rejected). In the Q-mode, the pulsed emission has a blackbody spectrum with temperature ∼ 3.4× {10}<SUP>6</SUP> K and the unpulsed emission is a power law with photon index ∼2.5, while during the B-mode both the pulsed and unpulsed emission can be fit by either a blackbody or a power law with similar values of temperature and index. A Chandra image does not show diffuse X-ray emission. These results support a scenario in which unpulsed non-thermal emission, likely magnetospheric, and pulsed thermal emission from a small polar cap (∼1500 m<SUP>2</SUP>) with a non-dipolar field (∼10<SUP>14</SUP> G) are present during both modes and vary in a correlated way. This is broadly consistent with the partially screened gap model and does not necessarily imply global magnetospheric rearrangements to explain the mode switching. | URI: | http://hdl.handle.net/20.500.12386/24740 | URL: | https://iopscience.iop.org/article/10.3847/0004-637X/831/1/21 | ISSN: | 0004-637X | DOI: | 10.3847/0004-637X/831/1/21 | Bibcode ADS: | 2016ApJ...831...21M | Fulltext: | open |
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