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Superhumps linked to X-ray emission : the superoutbursts of SSS J122221.7−311525 and GW Lib |
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| Author: | Neustroev, V. V.1,2; Page, K. L.3; Kuulkers, E.4; |
| Organizations: |
1Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland 2Astronomy Research Unit, PO Box 3000, 90014 University of Oulu, Finland 3Department of Physics & Astronomy, University of Leicester, University Rd, Leicester LE1 7RH, UK
4European Space Astronomy Centre (ESA/ESAC), Science Operations Department, 28691 Villanueva de la Cañada, Madrid, Spain
5School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK 6Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 7Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany 8Kazan (Volga Region) Federal University, Kremlevskaya str. 18, Kazan 420008, Russia 9Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, Ensenada, 22800 Baja California, Mexico |
| Format: | article |
| Version: | published version |
| Access: | open |
| Online Access: | PDF Full Text (PDF, 0.7 MB) |
| Persistent link: | http://urn.fi/urn:nbn:fi-fe201804116494 |
| Language: | English |
| Published: |
EDP Sciences,
2018
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| Publish Date: | 2018-04-11 |
| Description: |
AbstractContext: We present more than 4 years of Swift X-ray observations of the 2013 superoutburst, subsequent decline and quiescence of the WZ Sge-type dwarf nova SSS J122221.7-311525 (SSS J122222) from 6 days after discovery. Aims: Only a handful of WZ Sge-type dwarf novae have been observed in X-rays, and until recently GW Lib was the only binary of this type with complete coverage of an X-ray light curve throughout a superoutburst. We collected extensive X-ray data of a second such system to understand the extent to which the unexpected properties of GW Lib are common to the WZ Sge class. Methods: We collected 60 Swift-XRT observations of SSS J122222 between 2013 January 6 and 2013 July 1. Four follow-up observations were performed in 2014, 2015, 2016 and 2017. The total exposure time of our observations is 86.6 ks. We analysed the X-ray light curve and compared it with the behaviour of superhumps which were detected in the optical light curve. We also performed spectral analysis of the data. The results were compared with the properties of GW Lib, for which new X-ray observations were also obtained. Results: SSS J122222 was variable and around five times brighter in 0.3–10 keV X-rays during the superoutburst than in quiescence, mainly because of a significant strengthening of a high-energy component of the X-ray spectrum. The post-outburst decline of the X-ray flux lasted at least 500 d. The data show no evidence of the expected optically thick boundary layer in the system during the outburst. SSS J122222 also exhibited a sudden X-ray flux change in the middle of the superoutburst, which occurred exactly at the time of the superhump stage transition. A similar X-ray behaviour was also detected in GW Lib. Conclusions: We show that the X-ray flux exhibits changes at the times of changes in the superhump behaviour of both SSS J122222 and GW Lib. This result demonstrates a relationship between the outer disc and the white dwarf boundary layer for the first time, and suggests that models for accretion discs in high mass ratio accreting binaries are currently incomplete. The very long decline to X-ray quiescence is also in strong contrast to the expectation of low viscosity in the disc after outburst. see all
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| Series: |
Astronomy and astrophysics |
| ISSN: | 0004-6361 |
| ISSN-E: | 1432-0746 |
| ISSN-L: | 0004-6361 |
| Volume: | 611 |
| Article number: | A13 |
| DOI: | 10.1051/0004-6361/201731719 |
| OADOI: | https://oadoi.org/10.1051/0004-6361/201731719 |
| Type of Publication: |
A1 Journal article – refereed |
| Field of Science: |
115 Astronomy and space science |
| Subjects: | |
| Funding: |
K.L.P., J.P.O. and A.P.B. acknowledge the support of the UK Space Agency. TRM is supported by the STFC under grant ST/L000733. The work was supported by the Deutsche Forschungs-Gemeinschaft (DFG) grant WE 1312/51-1 and the Russian Foundation for Basic Research grant 16-02-01145-a (V.F.S.). The work of V.F.S. was also funded by the subsidy allocated to Kazan Federal University for the state assignment in the sphere of scientific activities (3.9780.2017/8.9). S.V.Z. acknowledges PAPIIT grant IN-100617 for resources provided towards this research. |
| Copyright information: |
© ESO 2018. Published in this repository with the kind permission of the publisher. |