Dips and eclipses in the X-ray binary Swift J1858.6-0814 observed with NICER

We present the discovery of eclipses in the X-ray light curves of the X-ray binary Swift J1858.6-0814. From these, we find an orbital period of $P=76841.3-{-1.4}{+1.3}$ s (≈21.3 h) and an eclipse duration of $t-{ m ec}=4098-{-18}{+17}$ s (≈1.14 h). We also find several absorption dips during the pre...

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Detalles Bibliográficos
Autores: Buisson, D .J. K., Altamirano, D., Armas Padilla, M., Arzoumanian, Z., Bult, P., Castro Segura, N., Charles, P. A., Degenaar, N., DÍaz Trigo, M., Van Den Eijnden, J., Fogantini, Federico Adrián, Gandhi, P., Gendreau, K., Hare, J., Homan, J., Knigge, C., Malacaria, C., Mendez, M., Muñoz Darias, T., Özbey Arabacl, M., Remillard, R., Strohmayer, T. E., Tombesi, F., Tomsick, J. A., Vincentelli, F., Walton, D. J.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:Argentina
Institución:Consejo Nacional de Investigaciones Científicas y Técnicas
Repositorio:CONICET Digital (CONICET)
Idioma:inglés
OAI Identifier:oai:ri.conicet.gov.ar:11336/211849
Acceso en línea:http://hdl.handle.net/11336/211849
Access Level:acceso abierto
Palabra clave:ACCRETION, ACCRETION DISCS
STARS: NEUTRON
X-RAYS: BINARIES
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
Descripción
Sumario:We present the discovery of eclipses in the X-ray light curves of the X-ray binary Swift J1858.6-0814. From these, we find an orbital period of $P=76841.3-{-1.4}{+1.3}$ s (≈21.3 h) and an eclipse duration of $t-{ m ec}=4098-{-18}{+17}$ s (≈1.14 h). We also find several absorption dips during the pre-eclipse phase. From the eclipse duration to orbital period ratio, the inclination of the binary orbit is constrained to i > 70°. The most likely range for the companion mass suggests that the inclination is likely to be closer to this value than 90. The eclipses are also consistent with earlier data, in which strong variability ('flares') and the long orbital period prevent clear detection of the period or eclipses. We also find that the bright flares occurred preferentially in the post-eclipse phase of the orbit, likely due to increased thickness at the disc-accretion stream interface preventing flares being visible during the pre-eclipse phase. This supports the notion that variable obscuration is responsible for the unusually strong variability in Swift J1858.6-0814.

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