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Recurrent low-level luminosity behaviour after a giant outburst in the Be/X-ray transient 4U 0115+63

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arxiv 1907.04724 v2 pith:GWLLYW4P submitted 2019-07-10 astro-ph.HE

A. Rouco Escorial , R. Wijnands , J. van den Eijnden , A. Patruno , N. Degenaar , A. Parikh , L. S. Ootes This is my paper · ORCID
classification astro-ph.HE
keywords outburstsourcebehaviourlow-levelx-raycampaigngiantluminosity
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In 2017, the Be/X-ray transient 4U 0115+63 exhibited a new type-II outburst that was two times fainter than its 2015 giant outburst (in the Swift/BAT count rates). Despite this difference between the two bright events, the source displayed similar X-ray behaviour after these periods. Once the outbursts ceased, the source did not transit towards quiescence directly, but was detected about a factor of 10 above its known quiescent level. It eventually decayed back to quiescence over time scales of months. In this paper we present the results of our Swift monitoring campaign, and an XMM-Newton observation of 4U 0115+63 during the decay of the 2017 type-II outburst, and its subsequent low-luminosity behaviour. We discuss the possible origin of the decaying source emission at this low-level luminosity, which has now been shown as a recurrent phenomenon, in the framework of the two proposed scenarios to explain this faint state: cooling from an accretion-heated neutron-star crust or continuous low-level accretion. In addition, we compare the outcome of our study with the results we obtained from the 2015/2016 monitoring campaign on this source.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Real-time observations of the transition to the quiescent state in an accreting magnetised neutron star: No propeller required?

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    First high-cadence observation of an X-ray pulsar transition to quiescence shows a gradual exponential fade consistent with the disc instability model, without requiring the propeller effect.

  2. Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry

    astro-ph.SR 2026-08 conditional novelty 6.0 of 10

    Bulk interstellar gas motion, not stellar motion, dominates most massive star bow shocks; only about 21% are classical aligned bow shocks.

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