The eccentric short-period orbit of the supergiant fast X-ray transient HD 74194 (=LM Vel)

Supernova explosion and the associated neutron star natal kicks are important events on a pathway of a binary to become a gravitational wave source, an X-ray binary or a millisecond radio pulsar. Weak natal kicks often lead to binary survival, while strong kicks frequently disrupt the binary. In this article, we aim to further constrain neutron star natal kicks in binaries. We explore binary population synthesis models by varying prescription for natal kick, remnant mass and mass accretion efficiency. We introduce a robust statistical technique to analyse combined observations of different nature. Using this technique, we further test different models using parallax and proper motion measurements for young isolated radio pulsars and similar measurements for Galactic Be X-ray binaries. Our best model for natal kicks is consistent with both measurements and contains a fraction of w = 0.2 ± 0.1 weak natal kicks with $\sigma _1 = 45^{+25}_{-15}$ km s−1, the remaining natal kicks are drawn from the high-velocity component, same as in previous works: σ2 = 336 km s−1. We found that currently used models for natal kicks of neutron stars produced by electron capture supernova (combination of maxwellian σ = 265 km s−1 and σ = 30 km s−1 for electron capture) are inconsistent or marginally consistent with parallaxes and proper motions measured for isolated radio pulsars. We suggest a new model for natal kicks of ecSN, which satisfy both observations of isolated radio pulsars and Be X-ray binaries.

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“…HD 74194 also known as LM Vel is supergiant system (Gamen et al 2015). This system is excluded from analysis.…”

Section: Data Availability Statementmentioning

confidence: 99%

Combined analysis of neutron star natal kicks using proper motions and parallax measurements for radio pulsars and Be X-ray binaries

Igoshev

Chruślińska

Andris

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…[23]), but nevertheless they can occur also at other orbital phases ( [24], [6]) and remarkably, in all sources but IGR J11215-5259, not every periastron passage triggers luminous flares. For example, after the recent determination of the orbital geometry in IGR J08408-4503 ( [23]), it is now evident that the long X-ray observation performed with Suzaku by [25] covered a large orbital phase interval just around periastron, and no bright flares were caught. However, it is important to remark that in a few SFXTs the orbital period has been discovered thanks to a periodic modulation in their long-term X-ray light curve (sometimes still present after removing bright flares).…”

Section: Pos(multif2017)052mentioning

confidence: 97%

“…Supergiant Fast X-ray Transients -A short review Lara Sidoli [27] 2.7 [28] 9.5436 [23] 0.63 [23] -285 ± 10 [23] IGR J11215-5952 B0.5Ia [29], [30], [31] >7 [31] 164.6 ,[32, 21, 33] >0.8 [31] 187 [34,15] -IGR J16328-4726 O8Iafpe [35], [36], [37] 7.2 [38] 10.068 [39], [40] ---IGR J16418-4532 OB Sg ∼13 [41] 3.753 [42] -1212 [43] 14.6842 [44], [45] IGR J16465-4507 O9.5Ia [46] 9.5 [47] 30.243 [48], [49] -228 [50] -IGR J16479-4514 O8.5I, O9.5Iab [51], [52] 4.9, 2.8 [51], [52] 3.3194 [53], [22] --11.880 [44], [45] XTE J1739-302…”

Section: Pos(multif2017)052mentioning

confidence: 99%

Supergiant Fast X-ray Transients - A short review

Sidoli¹

2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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I present a brief up-to-date review of the current understanding of Supergiant Fast X-ray Transients, with an emphasis on the observational point of view. After more than a decade since their discovery, a remarkable progress has been made in getting the picture of their phenomenology at X-ray energies. However, a similar in-depth investigation of the properties of the supergiant companions is needed, but has started more recently. A multifrequency approach is the key to fully understand the physical mechanism driving the SFXT behaviour, still under debate.In this short review paper I will concentrate on the most recent achievements about Supergiant Fast X-ray Transients (SFXTs), emphasizing an observational standpoint. The X-ray window will be looked at in particular, but with an eye also to observations at other frequencies, especially for what concerns the future directions. I will mainly focus on advances on the topic obtained thanks to systematic investigations of SFXT class as a whole, while I refer the reader to [1] for a summary of the properties of the single sources. For a unique, comprehensive and detailed review of the current understanding of the interplay between the outflowing wind from massive stars and accretion processes in wind-fed supergiant HMXBs, I refer the reader to [2].SFXTs ([3], [4]) are a sub-class of High Mass X-ray Binaries (HMXBs) where a compact object (typically a neutron star) accretes a fraction of the clumpy wind from the blue supergiant companion, triggering rare and short (less than a few days) outbursts, made of a number of bright X-ray flares (each flare with a duration of ∼thousands seconds). Most SFXTs were discovered by the INTEGRAL satellite (launched in 2002; [5]) as hard (above 17 keV) X-ray sources detected only during a short duration (a few hours) X-ray activity. Thanks to X-ray sky positions refined at arcsec level at soft X-rays (1-10 keV), they were quickly associated with O or B-type supergiants. The identification of these X-ray transients with massive X-ray binaries was somehow surprising, since the classical HMXBs with supergiant companion (SgHMXBs) known since the birth of Xray astronomy are persistent X-ray emitters, with a limited range of intensity variability (around a factor of ∼10). Fig. 1 shows the comparison between long-term X-ray INTEGRAL light curve of an SFXT and Vela X-1, the prototype of persistent HMXBs.Since their discovery, more than a decade ago, a huge observational effort has involved both long-term, X-ray monitoring investigations (summarized by [6] using RXT E, by [7] and [8] using INTEGRAL, by [9] and [10] using Swift) and deep, very sensitive, X-ray pointings (by Chandra, e.g. [11], and XMM-Newton, starting from the pioneering observations discussed by [12], to the more recent works by [13], [14], [15], ending with the latest published paper on SFXTs with XMM-Newton [16]).These X-ray observations led to the characterization of the SFXT properties, as follows:1. low duty cycle ( < ∼ 5%) in bright X-ray flares (at L X > ∼ 10 36 erg s −1...

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“…The results of our magnetic field measurements, those for the entire spectrum or only the hydrogen lines are presented in Table 1. The orbital phases of IGR J08408−4503 were calculated relative to a zero phase corresponding to the periastron passage at T per = 2454654.04 (Gamen et al 2015). The same zero phase as in the work of Lorenzo et al (2014) corresponding to the date of the first FEROS observation was adopted for IGR J11215−5952.…”

Section: Observations and Magnetic Field Measurementsmentioning

confidence: 99%

“…The optical counterpart of the system IGR J08408−4503 is the O-type supergiant star HD 74194 with spectral classification O8.6 Ib-II(f)p (Sota et al 2014). The orbital solution (P orb = 9.5436 ± 0.002 d, e = 0.63 ± 0.03) was for the first time determined by Gamen et al (2015). This work also indicated that the equivalent width of the Hα line is not modulated entirely with the orbital period, but seemed to vary with a superorbital period (P = 285 ± 10 d) nearly 30 times longer than the orbital one.…”

Section: Introductionmentioning

confidence: 96%

A search for the presence of magnetic fields in the two supergiant fast X-ray transients, IGR J08408−4503 and IGR J11215−5952

Hubrig

Sidoli

Постнов

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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A significant fraction of high-mass X-ray binaries are supergiant fast X-ray transients (SFXTs). The prime model for the physics governing their X-ray behaviour suggests that the winds of donor OB supergiants are magnetized. To investigate if magnetic fields are indeed present in the optical counterparts of such systems, we acquired low-resolution spectropolarimetric observations of the two optically brightest SFXTs, IGR J08408−4503 and IGR J11215−5952 with the ESO FORS 2 instrument during two different observing runs. No field detection at a significance level of 3σ was achieved for IGR J08408−4503. For IGR J11215−5952, we obtain 3.2σ and 3.8σ detections ( B z hydr = −978 ± 308 G and B z hydr = 416 ± 110 G) on two different nights in 2016. These results indicate that the model involving the interaction of a magnetized stellar wind with the neutron star magnetosphere can indeed be considered to characterize the behaviour of SFXTs. We detected long-term spectral variability in IGR J11215−5952, while for IGR J08408−4503 we find an indication of the presence of short-term variability on a time scale of minutes.

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The eccentric short-period orbit of the supergiant fast X-ray transient HD 74194 (=LM Vel)

Cited by 25 publications

References 27 publications

Combined analysis of neutron star natal kicks using proper motions and parallax measurements for radio pulsars and Be X-ray binaries

Combined analysis of neutron star natal kicks using proper motions and parallax measurements for radio pulsars and Be X-ray binaries

Supergiant Fast X-ray Transients - A short review

A search for the presence of magnetic fields in the two supergiant fast X-ray transients, IGR J08408−4503 and IGR J11215−5952

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