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http://hdl.handle.net/20.500.12386/25186
Title: | Multiwavelength study of RX J2015.6+3711: a magnetic cataclysmic variable with a 2-h spin period | Authors: | Coti Zelati, F. Rea, N. CAMPANA, Sergio DE MARTINO, Domitilla PAPITTO, ALESSANDRO Safi-Harb, S. Torres, D. F. |
Issue Date: | 2016 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 456 | Issue: | 2 | First Page: | 1913 | Abstract: | The X-ray source RX J2015.6+3711 was discovered by ROSAT in 1996 and recently proposed to be a cataclysmic variable (CV). Here, we report on an XMM-Newton observation of RX J2015.6+3711 performed in 2014, where we detected a coherent X-ray modulation at a period of 7196 ± 11 s and discovered other significant (>6σ) small-amplitude periodicities which we interpret as the CV spin period and the sidebands of a possible ∼12-h periodicity, respectively. The 0.3-10 keV spectrum can be described by a power law (Γ = 1.15 ± 0.04) with a complex absorption pattern, a broad emission feature at 6.60 ± 0.01 keV, and an unabsorbed flux of (3.16 ± 0.05) × 10<SUP>-12</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>. We observed a significant spectral variability along the spin phase, which can be ascribed mainly to changes in the density of a partial absorber and the power law normalization. Archival X-ray observations carried out by the Chandra satellite, and two simultaneous X-ray and UV/optical pointings with Swift, revealed a gradual fading of the source in the soft X-rays over the last 13 yr, and a rather stable X-ray-to-optical flux ratio (F<SUB>X</SUB>/F<SUB>V</SUB> ≈ 1.4-1.7). Based on all these properties, we identify this source with a magnetic CV, most probably of the intermediate polar type. The 2-h spin period makes RX J2015.6+3711, the second slowest rotator of the class, after RX J0524+4244 (`Paloma'; P<SUB>spin</SUB> ∼ 2.3 h). Although we cannot unambiguously establish the true orbital period with these observations, RX J2015.6+3711 appears to be a key system in the evolution of magnetic CVs. | URI: | http://hdl.handle.net/20.500.12386/25186 | URL: | https://academic.oup.com/mnras/article/456/2/1913/1070142 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stv2803 | Bibcode ADS: | 2016MNRAS.456.1913C | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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stv2803.pdf | Pdf editoriale | 2.11 MB | Adobe PDF | View/Open |
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