The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37

Ankay, A.; Kaper, L.; Bruijne, J. H. J. de; Dewi, Jasinta; Hoogerwerf, R.; Savonije, G. J.

doi:10.1051/0004-6361:20010192

Cited by 62 publications

(70 citation statements)

References 33 publications

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“…The detection of QPOs and the absence of pulsation (Dolan, 2011) favour a black hole compact object while the hard X-ray spectral shape is typical for an accreting pulsar. The binary may have escaped the Sco OB1 association 2 millions years ago (Ankay et al, 2001). High-ionisation lines have been observed also during eclipses, indicating that the stellar wind is very inhomogeneous (Boroson et al, 2003).…”

Section: Discussionmentioning

confidence: 97%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: Discussionmentioning

confidence: 97%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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“…It was suggested by Walborn (1973) that the object could be physically related to the runaway HMXB HD 153919/4U1700-37 (see Ankay et al 2001), that is at a projected linear distance of ∼24 pc. Note that SIMBAD lists HD 153426 wrongly as a B9II-III star.…”

Section: Hd 153426mentioning

confidence: 99%

“…We would like to note that the field O star population defined in this way contains three confirmed runaway stars, viz. HD 66811 (ζ Pup, e.g., Chlebowski 1989), HD 75222 (Hoogerwerf et al 2001) and HD 153919 (Ankay et al 2001). We have marked them in Table 2 with an asterisk.…”

Section: Sample Selectionmentioning

confidence: 99%

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The origin of massive O-type field stars

Wit¹,

Testi²,

Palla³

et al. 2004

A&A

110

136

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Abstract. We present a study aimed at clarifying the birthplace for 43 massive O-type field stars. In this first paper we present the observational part: a search for stellar clusters near the target stars. We derive stellar density maps at two different resolving scales, viz. ∼0.25 pc and ∼1.0 pc from NTT and TNG imaging and the 2MASS catalogue. These scales are typical for cluster sizes. The main result is that the large majority of the O-type field population are isolated stars: only 12% (5 out of 43) of the O-type field stars is found to harbour a small-scale stellar cluster. We review the literature and aim at characterizing the stellar field of each O-type field star with the emphasis on star formation and the presence of known young stellar clusters. An analysis of the result of this paper and a discussion of the O-type field population as products of a dynamical ejection event is presented in an accompanying paper.

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“…Hoogerwerf et al (2001) expand the database to 21 of 56 runaways traceable to specific clusters and remark that the former binary, consisting of z Oph and the progenitor of PSR J1932, once lived in the Sco OB2 association. Other Sco OB fugitives include the runaway neutron star RX J18535Ϫ3743 (Walter 2001), and the high-mass X-ray binary 4U 1700Ϫ37 p HD 153919 (Ankay et al 2001), which departed about 2 million years ago. Because the star that actually exploded in the "supernova runaway" mechanism is always by then the less massive of the pair (remember Roche lobe overflow), it is at least as easy to make a runaway binary as a runaway single, and both require non-spherical ejection of something during the explosion.…”

Section: Runawaystars and Walk-on Clustersmentioning

confidence: 99%

Astrophysics in 2001

Trimble¹,

Aschwanden²

2002

PUBL ASTRON SOC PAC

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ABSTRACT. During the year, astronomers provided explanations for solar topics ranging from the multiple personality disorder of neutrinos to cannibalism of CMEs (coronal mass ejections) and extrasolar topics including quivering stars, out-of-phase gaseous media, black holes of all sizes (too large, too small, and too medium), and the existence of the universe. Some of these explanations are probably probably true, though the authors are not betting large sums on any one. The data ought to remain true forever, though this requires a careful definition of "data" (think of the Martian canals).

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The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37

Cited by 62 publications

References 33 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

The origin of massive O-type field stars

Astrophysics in 2001

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