Searching for orbital period modulation in X-ray observations of the symbiotic X-ray binary GX 1+4

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作者：
Klawin, Moritz [1 ]
Ducci, Lorenzo [1 ,2 ,3 ]
Mirac Serim, M. [1 ]
Santangelo, Andrea [1 ]
Ferrigno, Carlo [2 ,3 ]
Bozzo, Enrico [2 ]
机构：
[1] Institut für Astronomie und Astrophysik, Sand 1, Tübingen,72076, Germany
[2] ISDC Data Center for Astrophysics, Université de Genève, 16 chemin d'Écogia, Versoix,1290, Switzerland
[3] INAF -Osservatorio Astronomico di Brera, via Bianchi 46 (LC), Merate,23807, Italy
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Astronomy and Astrophysics | 2024年 / 692卷
关键词：
The symbiotic X-ray binary GX 1+4 possesses a number of peculiar properties that have been studied since the early 1970s. In particular; the orbital period has been a point of debate for many years; until radial velocity measurements were able to settle the debate. These radial velocity findings have so far not been confirmed using X-ray data; even though multiple factors would cause a periodic variation on the same timescale as the orbital period at these energies. Because the orbit of GX 1+4 is eccentric and not seen face-on; changes in the accretion rate and column density along the line of sight could cause a periodic variation in the spin-frequency measurements; X-ray light curves; and hardness ratios of the source. Furthermore; for a high inclination of the orbital plane; the neutron star could be eclipsed by the companion; which would lead to periodic decreases in brightness. We used data from a number of different X-ray telescopes to search directly for periodicity by applying the Lomb-Scargle and epoch-folding approaches to long-term light-curve and spin-frequency measurement data of the source. We support our findings using folded light curves; hardness ratios; and images. We find that our results agree with the radial velocity findings; and we form a self-consistent model that is supported by folded hardness-ratios and light curves. We find that the source is clearly detected in X-rays during the predicted eclipse. Motivated by this absence of an eclipse in the system; we constrain the inclination of the system to ≈76°-84° and the mass of the neutron star in the system to ≈1.23 M˙-1.45M˙ using the constraints on the red giant mass and surface gravity provided in the literature. Furthermore; we constrain the radius of the red giant to ≈60 R˙-150R˙ © The Authors 2024;
D O I：
10.1051/0004-6361/202452031
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