On the origin of the o and b-type stars with high velocities II runaway stars and pulsars ejected from the nearby young stellar groups

By R. Hoogerwerf, J. Bruijne, P. de Zeeuw. 2000

288 citations recorded by the source corpus.

We use milli-arcsecond accuracy astrometry (proper motions and parallaxes) from Hipparcos and from radio observations to retrace the orbits of 56 runaway stars and nine compact objects with distances less than 700 pc, to identify the parent stellar group. It is possible to deduce the specific formation scenario with near certainty for two cases. (i) We find that the runaway star ζ Ophiuchi and the pulsar PSR J1932+1059 originated about 1 Myr ago in a supernova explosion in a binary in the Upper Scorpius subgroup of the Sco OB2 association. The pulsar received a kick velocity of �350 km s −1 in this event, which dissociated the binary, and gave ζ Oph its large space velocity. (ii) Blaauw & Morgan and Gies & Bolton already postulated a common origin for the runaway-pair AE Aur andCol, possibly involving the massive highly-eccentric binary ι Ori, based on their equal and opposite velocities. We demonstrate that these three objects indeed occupied a very small volume �2.5 Myr ago, and show that they were ejected from the nascent Trapezium cluster. We identify the parent group for two more pulsars: both likely originate in the � 50 Myr old association Per OB3, which contains the open cluster α Persei. At least 21 of the 56 runaway stars in our sample can be linked to the nearby associations and young open clusters. These in- clude the classical runaways 53 Arietis (Ori OB1), ξ Persei (Per OB2), and λ Cephei (Cep OB3), and fifteen new iden- tifications, amongst which a pair of stars running away in opposite directions from the region containing the λ Ori cluster. Other currently nearby runaways and pulsars orig- inated beyond 700 pc, where our knowledge of the parent groups is very incomplete.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6d139513619d9c2538edb6cbda078719ff6f723d

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Citations in the corpus

A Galactic O Star Catalog (2003, background): “(1) Stars listed as runaways in Hoogerwerf et al. (2001) or Mason et al. (1998) have a " yes " on that column.”
Slow Star Formation in Dense Gas: Evidence and Implications (2006, background): “…because there is no correlation between the age and spatial distribution for stars in the ONC (Huff & Stahler 2006) and because there must have been a system sufficiently dense to lead to dynamical interactions and ejection of massive stars 2.5 Myr ago (Hoogerwerf et al. 2001; Tan et al. 2006).”
Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars (2005, background): “High velocity O-stars were probably ejected by close encounters between binaries in dense clusters and by supernova explosions in close binaries (Hoogerwerf et al. 2001), and their ejection velocities generally exceed the escape velocity binding any wide, orbiting companion.”
A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun (2010, methodology): “Four of the seven runaway candidates listed by Hoogerwerf et al. (2001) (HIP 20330, 86768, 92609, 103206) are not recognised as runaway stars by us due to different input data (especially π) as Hoogerwerf et al. (2001) used the old Hipparcos reduction (Perryman et al. 1997) (smaller π in all four…”
Stellar and wind parameters of Galactic O-stars - The influence of line-blocking/blanketing (2004, methodology): “Additionally, we adopted a larger uncertainty in absolute magnitude, ±0.5 mag. ξ Per has the largest relative error in the measured parallax and the absolute magnitudes found in the literature do not match its spectral classification (Humphreys 1978; de Zeeuw et al. 1999; Hoogerwerf et al. 2001).”
Equilibrium Star Cluster Formation (2006, background): “This is consistent with observations that massive stars are not always the last to form in their clusters (e.g. Eisenhauer et al. 1998; Hoogerwerf et al. 2001), and theoretical work showing that clumpiness greatly inhibits gas dispersal (Tan & McKee 2004; Dale et al. 2005).”
The difficulty of getting high escape fractions of ionizing photons from high-redshift galaxies: A view from the FIRE cosmological simulations (2015, background): “There is plenty of evidence that a considerable fraction of O and B stars have high velocities and can travel far from their birth clouds during their lifetime (the “runaway” stars, e.g. Blaauw 1961; Stone 1991; Hoogerwerf et al. 2001; Tetzlaff et al. 2011).”
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, background): “About (10 - 30)% of O/early-B stars are “runaway stars” that have large peculiar velocities v ≈ 50 - 200 km s−1 and are found in isolation removed from young clusters/associations (Gies 1987; Stone 1991; Hoogerwerf et al. 2001).”
THE GALACTIC O-STAR SPECTROSCOPIC SURVEY (GOSSS). II. BRIGHT SOUTHERN STARS (2013, background): “Spectrograms are shown in Figure 11. µ Col = HD 38 666. µ Col is a runaway star, likely ejected from the Trapezium 2.5 Ma ago (Hoogerwerf et al. 2001).”
TOWARD COMPLETE STATISTICS OF MASSIVE BINARY STARS: PENULTIMATE RESULTS FROM THE CYGNUS OB2 RADIAL VELOCITY SURVEY (2014, background): ““Runaway” or “high-velocity stars also owe their extreme kinematics to hard interactions with massive binary systems (Blaauw 1961; Gies & Bolton 1986; Hoogerwerf et al. 2001).”
ESCAPE FRACTION OF IONIZING PHOTONS DURING REIONIZATION: EFFECTS DUE TO SUPERNOVA FEEDBACK AND RUNAWAY OB STARS (2014, background): “The runaway OB stars are normally defined by their peculiar motion (vpec ≥ 30kms−1, Blaauw 1961), and roughly 30% of OB stars are classified as runaways in the Milky Way (Stone 1991; Hoogerwerf et al. 2001; Tetzlaff et al. 2011).”
O stars with weak winds: the Galactic case (2005, background): “In the scenario where these two stars originated from a binary and were ejected in a dynamical interaction, Hoogerwerf et al. (2001) estimate a travel time of 2.5 Myrs, while van Rensbergen et al. (1996) found travel times of ∼ 3.5 Myrs for HD 38666 and ∼ 2.5 Myrs for HD 34078.”
THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, background): “(e) The supernova explosion of the primary star can break up the binary system, depending on the amount of mass lost from the system and the magnitude and orientation of the birth kick of the compact object (Blaauw 1961; Hoogerwerf et al. 2001).”
Massive runaway and walkaway stars (2018, background): “This finding agrees with the results of Eldridge et al. (2011), but is in potential contrast with the observational results of Hoogerwerf et al. (2001), and needs further investigation.”