A1 Refereed original research article in a scientific journal
The remarkable outburst of the highly evolved post-period-minimum dwarf nova SSS J122221.7-311525
Authors: V. V. Neustroev, R. R. Marsh, S. V. Zharikov, C. Knigge, E. Kuulkers, J. P. Osborne, K. L. Page, D. Steeghs, V. F. Suleimanov, G. Tovmassian, E. Breedt, A. Frebel, Ma. T. García-Díaz, F.-J. Hambsch, H. Jacobson, S. G. Parsons, T. Ryu, L. Sabin, G. Sjoberg, A. S. Miroshnichenko, D. E. Reichart, J. B. Haislip, K. M. Ivarsen, A. P. LaCluyze, J. P. Moore
Publisher: OXFORD UNIV PRESS
Publication year: 2017
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume: 467
Issue: 1
First page : 597
Last page: 618
Number of pages: 22
ISSN: 0035-8711
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/stx084
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/20712075
We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7-311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d(-1), and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B -I similar or equal to 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess less than or similar to 0.8 per cent, indicating a very low mass ratio q less than or similar to 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a nearmain- sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7-311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim.
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