MXB 1659-298 is a transient neutron-star low-mass X-ray binary system that shows eclipses with a periodicity of 7.1 h. MXB 1659-298 went to outburst in 2015 August, after 14 years of quiescence. We investigate the orbital properties of this source with a baseline of 40 years, obtained by combining the eight eclipse arrival times present in the literature with 51 eclipse arrival times collected during the last two outbursts. A quadratic ephemeris does not fit the delays associated with the eclipse arrival times and the addition of a sinusoidal term with a period of 2.31 +/- 0.02 yr is required. We infer a binary orbital period of P = 7.1161099(3) h and an orbital period derivative of. P = -8.5(1.2) x 10(-12) s s(-1). We show that the large orbital period derivative can be explained with a highly non-conservative mass-transfer scenario, in which more than 98 per cent of the mass provided by the companion star leaves the binary system. We predict an orbital period derivative value of. P = -6(3) x 10(-12) s s(-1) and constrain the companion-star mass between 0.3 and 1.2 M-circle dot. Assuming that the companion star is in thermal equilibrium, the periodic modulation can be due to either a gravitational quadrupole coupling arising from variations of the oblateness of the companion star or the presence of a third body of mass M-3 > 21 Jovian masses.

Iaria, R., Gambino, A.F., Di Salvo, T., Burderi, L., Matranga, M., Riggio, A., et al. (2018). A possible solution of the puzzling variation of the orbital period of MXB 1659–298. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 473(3), 3490-3499 [10.1093/mnras/stx2529].

A possible solution of the puzzling variation of the orbital period of MXB 1659–298

Iaria, R.
;
Gambino, A. F.;Di Salvo, T.;
2018-01-01

Abstract

MXB 1659-298 is a transient neutron-star low-mass X-ray binary system that shows eclipses with a periodicity of 7.1 h. MXB 1659-298 went to outburst in 2015 August, after 14 years of quiescence. We investigate the orbital properties of this source with a baseline of 40 years, obtained by combining the eight eclipse arrival times present in the literature with 51 eclipse arrival times collected during the last two outbursts. A quadratic ephemeris does not fit the delays associated with the eclipse arrival times and the addition of a sinusoidal term with a period of 2.31 +/- 0.02 yr is required. We infer a binary orbital period of P = 7.1161099(3) h and an orbital period derivative of. P = -8.5(1.2) x 10(-12) s s(-1). We show that the large orbital period derivative can be explained with a highly non-conservative mass-transfer scenario, in which more than 98 per cent of the mass provided by the companion star leaves the binary system. We predict an orbital period derivative value of. P = -6(3) x 10(-12) s s(-1) and constrain the companion-star mass between 0.3 and 1.2 M-circle dot. Assuming that the companion star is in thermal equilibrium, the periodic modulation can be due to either a gravitational quadrupole coupling arising from variations of the oblateness of the companion star or the presence of a third body of mass M-3 > 21 Jovian masses.
2018
Settore FIS/05 - Astronomia E Astrofisica
Iaria, R., Gambino, A.F., Di Salvo, T., Burderi, L., Matranga, M., Riggio, A., et al. (2018). A possible solution of the puzzling variation of the orbital period of MXB 1659–298. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 473(3), 3490-3499 [10.1093/mnras/stx2529].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10447/282147
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