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Astrophysics the Origin of the Runaway High-Mass X UvA-DARE (Digital Academic Repository) The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37 Ankay, A.; Kaper, L.; de Bruijne, J.H.J.; Dewi, J.D.M.; Hoogerwerf, R.; Savonije, G.J. Publication date 2001 Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Ankay, A., Kaper, L., de Bruijne, J. H. J., Dewi, J. D. M., Hoogerwerf, R., & Savonije, G. J. (2001). The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37. Astronomy & Astrophysics, 370, 170-175. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:30 Sep 2021 A&A 370, 170–175 (2001) Astronomy DOI: 10.1051/0004-6361:20010192 & c ESO 2001 Astrophysics The origin of the runaway high-mass X-ray binary HD 153919/4U1700-37? A. Ankay1,2,L.Kaper1,J.H.J.deBruijne3,J.Dewi1, R. Hoogerwerf3, and G. J. Savonije1 1 Astronomical Institute “Anton Pannekoek” and Center for High-Energy Astrophysics, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands 2 Middle East Technical University, Physics Department, 06531 Ankara, Turkey 3 Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands Received 8 September 2000 / Accepted 31 January 2001 Abstract. Based on its Hipparcos proper motion, we propose that the high-mass X-ray binary HD 153919/4U1700- 37 originates in the OB association Sco OB1. At a distance of 1.9 kpc the space velocity of 4U1700-37 with respecttoScoOB1is75kms−1. This runaway velocity indicates that the progenitor of the compact X-ray source lost about 7 M during the (assumed symmetric) supernova explosion. The system’s kinematical age is about 2 0.5 million years which marks the date of the supernova explosion forming the compact object. The present age of Sco OB1 is ∼<8 Myr; its suggested core, NGC 6231, seems to be somewhat younger (∼5Myr).If HD 153919/4U1700-37 was born as a member of Sco OB1, this implies that the initially most massive star in the system terminated its evolution within ∼<6 million years, corresponding to an initial mass ∼>30 M .Withthese parameters the evolution of the binary system can be constrained. Key words. stars: early type – stars: mass loss – stars: neutron – stars: individual: HD 153919 – 4U1700-37 – ultraviolet: stars 1. Introduction A neutron star or a black hole, the compact remnant of the initially most massive star (the primary) in the binary The massive stars in the Milky Way are not randomly system, produces X-rays due to the accretion of matter distributed, but are concentrated in loose groups called from the secondary (an OB supergiant or a Be star); see OB associations located in the spiral arms of our galaxy Kaper (1998) for an overview of the OB-supergiant sys- (for a review, see e.g. Brown et al. 1999). About 80% of tems. The binary system remains bound after the super- the O stars are member of an OB association; the kine- nova, if less than 50% of the total system mass is lost matical properties of the remaining 20% of the field pop- during the (assumed symmetric) explosion (Blaauw 1961; ulation suggest that these O stars are runaways, i.e. they Boersma 1961). The latter can be understood if one con- were born in an OB association, but at a certain stage siders the phase of mass transfer occuring when the pri- they escaped from it (Blaauw 1993). The two most popu- mary becomes larger than its critical Roche lobe (e.g. at lar scenarios to explain the existence of runaway stars are the end of core-hydrogen burning when the star expands (i) the dynamical ejection from a young cluster (Poveda to become a supergiant) and matter flows from the pri- et al. 1967) and (ii) the supernova of the companion star mary to the secondary. This results in a change of the in a massive binary (Blaauw 1961). A recent study by mass ratio from larger to smaller than one. A kick exerted Hoogerwerf et al. (2000) based on Hipparcos data demon- on the compact object due to the eventual asymmetry strates that both scenarios are at work, probably at a rate of the supernova explosion has also to be taken into ac- of 1:2, respectively. count when determining whether the binary breaks up or High-mass X-ray binaries (HMXBs) are the descen- remains bound after the supernova. dants of massive binaries (Van den Heuvel & Heise 1972). According to the binary-supernova scenario all Send offprint requests to:L.Kaper, HMXBs should be runaways. Gies & Bolton (1986) did e-mail: [email protected] not find observational evidence supporting this hypothe- ? Based on data obtained with ESA’s astrometric satellite sis on the basis of radial-velocity measurements, though Hipparcos. Van Oijen (1989) found strong indications that HMXBs A. Ankay et al.: The runaway system HD 153919/4U1700-37 171 Fig. 1. O- and B-type stars selected from the Hipparcos cata- Fig. 2. The Hipparcos proper motions of the OB stars shown in logue in the field of HD 153919/4U1700-37 (filled circle). The Fig. 1. The filled diamonds represent the confirmed members confirmed members of Sco OB1 are shown as filled diamonds. of Sco OB1; these stars cluster both in location and in proper The plus symbols correspond to OB stars with a parallax larger motion. The plusses and open circles indicate the OB stars we than 1 mas (i.e. distance smaller than 1 kpc) and were elim- could, or could not exclude on the basis of a distance estimate, inated from the membership analysis. The open circles indi- respectively. The circles with a central dot are stars with sim- cate stars with a (photometric) distance within the range of ilar proper motion and photometric distance as the confirmed Sco OB1; some of them, with a proper motion similar to the cluster members. Also shown is 4U1700-37 (filled circle) which confirmed association members, are indicated by a circle with obviously has a proper motion different from that of Sco OB1 central dot (cf. Fig. 2). The latter close to Sco OB1 might be members as well relates to the amount of mass lost from the system dur- are high-velocity objects. Based on pre-Hipparcos proper ing the supernova explosion (cf. Nelemans et al. 1999). motion measurements, Van Rensbergen et al. (1996) sug- The age of the parent OB association should be equal to gested that the HMXB Vela X-1 is a runaway system pro- the age of the binary system. Consequently, the turn-off duced by the supernova scenario, and that it originates in mass at the time of supernova yields the initial mass of the OB association Vel OB1. The discovery of a wind-bow the primary. Thus, this relatively straigthforward obser- shock around Vela X-1 showed that this system indeed is vation can be used to determine the age of the system, running through interstellar space with a supersonic ve- the time of supernova of the primary, the initial mass of locity, proving the runaway nature of this HMXB (Kaper the primary, and the amount of mass lost from the system et al. 1997). The Hipparcos proper motions of a dozen during the supernova. Combining this information allows HMXBs (Chevalier & Ilovaisky 1998; Kaper et al. 1999) one to put constraints on the initial orbital parameters finally demonstrated that, as expected, likely all HMXBs of the progenitor of the HMXB and on the evolutionary are runaways. The most massive systems (those hosting history of the system. an OB supergiant) have a mean peculiar (i.e. with re- Here we apply this to the system HD 153919/4U1700- spect to their standard of rest) tangential velocity of about 37. HD 153919 (mV =6.6) is the O6.5 Iaf+ companion 40 km s−1, whereas the Be/X-ray binaries have on average to 4U1700-37, most likely a neutron star powered by wind lower velocities (about 15 km s−1). This difference in ve- accretion (Jones et al. 1973; Haberl et al. 1989), although locity is consistent with the predictions of binary evolution no X-ray pulsations have been detected (Gottwald et al. (Van den Heuvel et al. 2000). 1986). According to Brown et al. (1996) 4U1700-37 is a The identification of the “parent” OB association of good candidate for a low-mass black hole. HD 153919 is a HMXB is important, because it provides unique con- the hottest OB companion star known in a HMXB; there- straints on the evolution of high-mass X-ray binaries. fore, the progenitor of 4U1700-37 potentially is a very mas- When the system’s proper motion and parent OB associ- sive star.
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