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

Tiziana Di Salvo, Angelo Francesco Gambino, Rosario Iaria, D'Aì, Riggio, Sanna, Scarano, Burderi

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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.
Lingua originaleEnglish
pagine (da-a)3490-3499
Numero di pagine10
RivistaMonthly Notices of the Royal Astronomical Society
Volume473
Stato di pubblicazionePublished - 2018

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companion stars
eclipses
orbitals
arrival time
arrivals
outburst
leaves
neutron stars
periodicity
mass transfer
periodic variations
quadrupoles
modulation
x rays

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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title = "A possible solution of the puzzling variation of the orbital period of MXB 1659–298",
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.",
keywords = "X-rays: binaries, X-rays: stars, binaries: eclipsing, ephemerides, stars: individual: MXB 1659-298, stars: neutron",
author = "{Di Salvo}, Tiziana and Gambino, {Angelo Francesco} and Rosario Iaria and D'A{\`i} and Riggio and Sanna and Scarano and Burderi",
year = "2018",
language = "English",
volume = "473",
pages = "3490--3499",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",

}

TY - JOUR

T1 - A possible solution of the puzzling variation of the orbital period of MXB 1659–298

AU - Di Salvo, Tiziana

AU - Gambino, Angelo Francesco

AU - Iaria, Rosario

AU - D'Aì, null

AU - Riggio, null

AU - Sanna, null

AU - Scarano, null

AU - Burderi, null

PY - 2018

Y1 - 2018

N2 - 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.

AB - 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.

KW - X-rays: binaries

KW - X-rays: stars

KW - binaries: eclipsing

KW - ephemerides

KW - stars: individual: MXB 1659-298

KW - stars: neutron

UR - http://hdl.handle.net/10447/282147

UR - https://academic.oup.com/mnras/article-abstract/473/3/3490/4628110?redirectedFrom=PDF

M3 - Article

VL - 473

SP - 3490

EP - 3499

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -