The 17-min orbital period in the ultracompact X-ray binary 4U 0513-40

Fiocchi, M.; Bazzano, A.; Natalucci, L.; Landi, R.; Ubertini, P.

doi:10.1111/j.1745-3933.2011.01051.x

Cited by 13 publications

(9 citation statements)

References 19 publications

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“…Far ultraviolet photometry obtained by HST revealed a 17 min orbital modulation (Zurek et al 2009). Observations with BeppoSAX, Chandra, XMM-Newton, INTE-GRAL confirmed the 17 min periodic sinusoidal signal in soft X-ray (Fiocchi et al 2011). The system is known to be an X-ray burster (Galloway et al 2008;Homer et al 2001;Fiocchi et al 2011) which indicates that the primary is a neutron star.…”

Section: U 0513-40mentioning

confidence: 79%

“…Observations with BeppoSAX, Chandra, XMM-Newton, INTE-GRAL confirmed the 17 min periodic sinusoidal signal in soft X-ray (Fiocchi et al 2011). The system is known to be an X-ray burster (Galloway et al 2008;Homer et al 2001;Fiocchi et al 2011) which indicates that the primary is a neutron star. The short orbital period suggests a low mass white dwarf secondary of ∼ 0.05M ⊙ , as implied from mass-radius relation for 17 min period binaries from Deloye & Bildsten (2003).…”

Section: U 0513-40mentioning

confidence: 79%

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On the Dynamics of Ultra Compact X-Ray Binaries: 4u 1850-087, 4u 0513-40, and M15 X-2

Prodan

Murray²

2015

ApJ

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In this work we extend our dynamical study of Ultra Compact X-ray Binaries (UCXB) 4U 1820-30 from Prodan & Murray (2012) to three more UCXBs in globular clusters: 4U 1850-087, 4U 0513-40 and M15 X-2. These three UCXBs have orbital periods 20 min. Two of them, 4U 1850-087 and 4U 0513-40, have suspected luminosity variations of order of ∼ 1 yr. There is insufficient observational data to make any statements regarding the long periodicity in the light curve of M15 X-2 at this point. The properties of these three systems are quite similar to 4U 1820-30, which prompt us to model their dynamics in the same manner. As in the case of 4U 1820-30, we interpret the suspected long periods as the period of small oscillations around a stable fixed point in the Kozai resonance. We provide a lower limit on the tidal dissipation factor Q which is in agreement with results obtained for the case of 4U 1820-30.

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Section: U 0513-40mentioning

confidence: 79%

Section: U 0513-40mentioning

confidence: 79%

On the Dynamics of Ultra Compact X-Ray Binaries: 4u 1850-087, 4u 0513-40, and M15 X-2

Prodan

Murray²

2015

ApJ

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“…4U 0513-40 is located at a distance of ≈ 12.2 kpc (Kuulkers et al 2003) and has an observed orbital period of 17 min (Fiocchi et al 2011). It has been observed 2 and 3, respectively.…”

Section: U 0513-40mentioning

confidence: 96%

X-ray diagnostics of chemical composition of the accretion disc and donor star in UCXBs – II. XMM–Newton observations

Koliopanos

Gilfanov

Bildsten

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We search for the Fe Kα line in spectra of Ultra Compact X-ray Binaries (UCXBs). For this purpose we have analyzed XMM-Newton observations of five confirmed UCXBs. We find that the object 2S 0918-549 -whose optical spectrum bears tentative signatures of a C/O accretion disk -is devoid of any emission features in the 6-7 keV range, with an upper limit of less than 10 eV for the equivalent width (EW) of the iron line. 4U 1916-05 -whose optical spectrum is consistent with reflection from a He-rich accretion disk -exhibits a bright broad iron emission line. This behavior is in agreement with the theoretical predictions presented in Koliopanos, Gilfanov & Bildsten (2013). Namely, we expect strong suppression of the Fe Kα emission line in spectra originating in moderately bright (LogL x less than ≈ 37.5) UCXBs with C/O or O/Ne/Mg-rich donors. On the other hand the EW of the iron line in spectra from UCXBs with He-rich donors is expected to retain its nominal value of ≈ 100 eV. Our analysis also reveals a strong Fe Kα line in the spectrum of 4U 0614+091. This detection points towards a He-rich donor and seems to be at odds with the source's classification as C/O-rich. Nevertheless, a He-rich donor would explain the bursting activity reported for this system. Lastly, based on our theoretical predictions, we attribute the lack of a strong iron emission line -in the two remaining UCXB sources in our sample (XTE J1807-294, 4U 0513-40) -as an indication of a C/O or O/Ne/Mg white dwarf donor. From the upper limits of the Fe Kα line EW in 4U 0513-40, 2S 0918-549 and XTE J1807-294 we obtain a lower limit on the oxygen-to-iron ratio, O/Fe 10 × [O/Fe] ⊙ .

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“…The origin of the X-ray modulation in the high/soft state that was observed for instance in the UCXB 4U 0513−40 (Fiocchi et al 2011) or UCXB 4U 1820−30 (Stella et al 1987) has not yet been established. In the case of the 4U 0513−40 a periodic modulation is visible when the source is in the high/soft state (Fiocchi et al 2011). In 4U 1820−30 a periodic modulation with an amplitude of ≈ 10% was found when the source was in the high/soft state.…”

Section: X-ray Modulationmentioning

confidence: 99%

“…In one out of 12 optical data sets the authors found a strong periodic signal at ≈ 50 min. The modulations with the orbital periods in the UCXBs were reported not only in optical but also X-ray light curves (Fiocchi et al 2011;Stella et al 1987). As far as 4U 0614+091 is concerned a periodic modulation of ≈ 25 min was found in one EXOSAT light curve (Hakala et al 2011), when the source was in a high flux state.…”

mentioning

confidence: 92%

Time-resolved X-Shooter spectra and RXTE light curves of the ultra-compact X-ray binary candidate 4U 0614+091★

Madej¹,

Jonker²,

Groot³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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In this paper we present X-Shooter time resolved spectroscopy and RXTE PCA light curves of the ultra-compact X-ray binary candidate 4U 0614+091. The X-Shooter data are compared to the GMOS data analyzed previously by Nelemans et al. (2004). We confirm the presence of C III and O II emission features at ≈ 4650 Å and ≈ 5000 Å. The emission lines do not show evident Doppler shifts that could be attributed to the motion of the donor star/hot spot around the center of mass of the binary. We note a weak periodic signal in the red-wing/blue-wing flux ratio of the emission feature at ≈ 4650 Å. The signal occurs at P = 30.23 ± 0.03 min in the X-Shooter and at P = 30.468 ± 0.006 min in the GMOS spectra when the source was in the low/hard state. Due to aliasing effects the period in the GMOS and X-Shooter data could well be the same. We deem it likely that the orbital period is thus close to 30 min, however, as several photometric periods have been reported for this source in the literature already, further confirmation of the 30 min period is warranted. We compare the surface area of the donor star and the disc of 4U 0614+091 with the surface area of the donor star and the disc in typical hydrogen-rich low-mass X-ray binaries and the class of AM Canum Venaticorum stars and argue that the optical emission in 4U 0614+091 is likely dominated by the disc emission. Assuming that the accretion disc in 4U 0614+091 is optically thick and the opening angle of the disc is similar to the one derived for the hydrogen-rich low-mass X-ray binaries we conclude that the donor star may in fact stay in the disc shadow. Additionally, we search for periodic signals in all the publicly available RXTE PCA light curves of 4U 0614+091 which could be associated with the orbital period of this source. A modulation at the orbital period with an amplitude of ≈ 10% such as those that have been found in other ultra-compact X-ray binaries (4U 0513−40, 4U 1820−30) is not present in 4U 0614+091. We propose that the X-ray modulation found in 4U 0513−40 and 4U 1820−30 could be a signature of an outflow launched during the high/soft state near the stream impact region.

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The 17-min orbital period in the ultracompact X-ray binary 4U 0513-40

Cited by 13 publications

References 19 publications

On the Dynamics of Ultra Compact X-Ray Binaries: 4u 1850-087, 4u 0513-40, and M15 X-2

On the Dynamics of Ultra Compact X-Ray Binaries: 4u 1850-087, 4u 0513-40, and M15 X-2

X-ray diagnostics of chemical composition of the accretion disc and donor star in UCXBs – II. XMM–Newton observations

Time-resolved X-Shooter spectra and RXTE light curves of the ultra-compact X-ray binary candidate 4U 0614+091★

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