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http://hdl.handle.net/20.500.12386/30679
Title: | XMM-Newton observations of PSR J0726-2612, a radio-loud XDINS | Authors: | RIGOSELLI, MICHELA MEREGHETTI, Sandro Valery Suleimanov Alexander Y. Potekhin Roberto Turolla Roberto Taverna Fabio Pintore |
Issue Date: | 2019 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 627 | First Page: | A69 | Abstract: | We present the results of an XMM-Newton observation of the slowly rotating ($P = 3.4$ s), highly magnetized ($B \approx 3 \times 10^{13}$ G) radio pulsar PSR J0726-2612. A previous X-ray observation with the Chandra satellite showed that some of the properties of PSR J0726-2612 are similar to those of the X-ray Dim Isolated Neutron Stars (XDINSs), a small class of nearby slow pulsars characterized by purely thermal X-ray spectra and undetected in the radio band. We confirm the thermal nature of the X-ray emission of PSR J0726-2612, which can be fit by the sum of two blackbodies with temperatures $kT_1 = 0.074_{-0.011}^{+0.006}$ keV and $kT_2 = 0.14_{-0.02}^{+0.04}$ keV and emitting radii $R_1 = 10.4_{-2.8}^{+10.8}$ km and $R_2 = 0.5_{-0.3}^{+0.9}$ km, respectively (assuming a distance of 1 kpc). A broad absorption line modeled with a Gaussian profile centred at $0.39_{-0.03}^{+0.02}$ keV is required in the fit. The pulse profile of PSR J0726-2612 is characterized by two peaks with similar intensity separated by two unequal minima, a shape and pulsed fraction that cannot be reproduced without invoking magnetic beaming of the X-ray emission. The presence of a single radio pulse suggests that in PSR J0726-2612 the angles that the dipole axis and the line of sight make with the rotation axis, $\xi$ and $\chi$ respectively, are similar. This geometry differs from that of the two radio-silent XDINSs with a double peaked pulse profile similar to that of PSR J0726-2612, for which $\xi \sim 90^\circ$ and $\chi \sim 45^\circ$ have been recently estimated. These results strengthen the similarity between PSR J0726-2612 and the XDINSs and support the possibility that the lack of radio emission from the latter might simply be due to an unfavourable viewing geometry. | URI: | http://hdl.handle.net/20.500.12386/30679 | URL: | http://arxiv.org/abs/1906.01372v1 https://www.aanda.org/articles/aa/full_html/2019/07/aa35485-19/aa35485-19.html |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201935485 | Bibcode ADS: | 2019A&A...627A..69R | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Rigoselli_2019_A&A_627_A69.pdf | Pdf editoriale | 2.22 MB | Adobe PDF | View/Open |
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