RX J0529.8−6556: a BeXRB pulsar with an evolving optical period and out of phase X-ray outbursts

Author:

Treiber H12ORCID,Vasilopoulos G1ORCID,Bailyn C D1,Haberl F3ORCID,Gendreau K C4,Ray P S5ORCID,Maitra C3ORCID,Maggi P6ORCID,Jaisawal G K7ORCID,Udalski A8ORCID,Wilms J9,Monageng I M1011ORCID,Buckley D A H10ORCID,König O9,Carpano S3

Affiliation:

1. Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA

2. Department of Physics and Astronomy, Amherst College, C025 New Science Center, 25 East Dr., Amherst, MA 01002-5000, USA

3. Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany

4. X-Ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

5. Space Science Division, U.S. Naval Research Laboratory, Washington, DC 20375, USA

6. Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, F-67000 Strasbourg, France

7. National Space Institute, Technical University of Denmark, Elektrovej 327-328, DK-2800 Lyngby, Denmark

8. Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, P-00-478 Warszawa, Poland

9. Observatory and Erlangen Centre for Astroparticle Physics, Sternwartstr. 7, D-96049 Bamberg, Germany

10. South African Astronomical Observatory, PO Box 9, Observatory, Cape Town 7935, South Africa

11. Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa

Abstract

ABSTRACT We report the results of eROSITA and NICER observations of the 2020 June outburst of the Be/X-ray binary pulsar RX J0529.8−6556 in the Large Magellanic Cloud, along with the analysis of archival X-ray and optical data from this source. We find two anomalous features in the system’s behaviour. First, the pulse profile observed by NICER during maximum luminosity is similar to that observed by XMM–Newton in 2000, despite the fact that the X-ray luminosity was different by two orders of magnitude. In contrast, a modest decrease in luminosity in the 2020 observations generated a significant change in pulse profile. Secondly, we find that the historical optical outbursts are not strictly periodic, as would be expected if the outbursts were triggered by periastron passage, as is generally assumed. The optical peaks are also not coincident with the X-ray outbursts. We suggest that this behaviour may result from a misalignment of the Be star disc and the orbital plane, which might cause changes in the timing of the passage of the neutron star through the disc as it precesses. We conclude that the orbital period of the source remains unclear.

Funder

ESA

NASA

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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