Wolf--Rayet and O star runaway populations from supernovae

Dray, Lynnette; Dale, James E.; Beer, Martin E.; Napiwotzki, R.; King, Andrew

doi:10.1111/j.1365-2966.2005.09536.x

Cited by 37 publications

(41 citation statements)

References 56 publications

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“…Dray et al (2005) estimate that 2 /3 of massive runaways are produced this way. Isserstedt, Moffat & Niemela (1983) show that kick velocities of ∼ 150 kms −1 may be imparted on a surviving star, and that this star and the resulting supernova remnant may remain bound if less than half the total system mass is lost during the supernova.…”

Section: Wr Stars At Large Distances From the Galactic Diskmentioning

confidence: 99%

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Rosslowe

Crowther

2015

Monthly Notices of the Royal Astronomical Society

123

143

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We construct revised near-infrared absolute magnitude calibrations for 126 Galactic Wolf-Rayet (WR) stars at known distances, based in part upon recent large scale spectroscopic surveys. Application to 246 WR stars located in the field, permits us to map their Galactic distribution. As anticipated, WR stars generally lie in the thin disk (∼40 pc half width at half maximum) between Galactocentric radii 3.5-10 kpc, in accordance with other star formation tracers. We highlight 12 WR stars located at vertical distances of 300 pc from the midplane. Analysis of the radial variation in WR subtypes exposes a ubiquitously higher N W C /N W N ratio than predicted by stellar evolutionary models accounting for stellar rotation. Models for non-rotating stars or accounting for close binary evolution are more consistent with observations. We consolidate information acquired about the known WR content of the Milky Way to build a simple model of the complete population. We derive observable quantities over a range of wavelengths, allowing us to estimate a total number of 1200 +300 −100 Galactic WR stars, implying an average duration of ∼ 0.25 Myr for the WR phase at the current Milky Way star formation rate. Of relevance to future spectroscopic surveys, we use this model WR population to predict follow-up spectroscopy to K S ≃ 13 mag will be necessary to identify 95% of Galactic WR stars. We anticipate that ESA's Gaia mission will make few additional WR star discoveries via low-resolution spectroscopy, though will significantly refine existing distance determinations. Appendix A provides a complete inventory of 322 Galactic WR stars discovered since the VIIth catalogue (313 including Annex), including a revised nomenclature scheme.

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Section: Wr Stars At Large Distances From the Galactic Diskmentioning

confidence: 99%

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Rosslowe

Crowther

2015

Monthly Notices of the Royal Astronomical Society

123

143

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“…)favourably directed SN kick or the post-MS evolution of the primary leading to the spiral-in of both components and the formation of a Thorne-Zytkow object (TZO). Given that Dray et al (2005) suggest that ∼1% of SNe kicks may result in the production of TZOs, our above estimate of ∼100 SNe to date and the presence of four highly luminous RSGs within Wd 1, it would be of interest to search these for the abundance anomalies predicted for TZOs (e.g. the 30 Si/ 28 Si ratio) by van Paradijs et al (1995).…”

Section: Stellar Mass Accretorsmentioning

confidence: 87%

“…Indeed, the role of a SN kick in a massive binary is a matter of considerable ongoing debate (e.g. Pfahl et al 2002), with recent Monte Carlo simulations by Dray et al (2005) demonstrating that different kick prescriptions may yield post-SN binary fractions ranging from 0.2%−40.2%, with a large number of surviving binaries having orbital parameters that preclude significant mass accretion onto the relativistic companion. Moreover, van den Heuvel et al (2000) find a mean tangental velocity of 42 ± 14km s −1 for SG HMXBs imparted by the SN kick.…”

Section: Stellar Mass Accretorsmentioning

confidence: 99%

Unveiling the X-ray point source population of the Young Massive Cluster Westerlund 1

Clark¹,

Muno

Negueruela

et al. 2007

A&A

193

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Aims. We investigate the nature of the X-ray point source population within the Young Massive Cluster Westerlund 1. Methods. Chandra observations of 18 ks and 42 ks were used to determine the X-ray properties of emitters within Wd 1, while a comprehensive multiwavelength dataset was employed to constrain their nature. Results. We find X-ray emission from a multitude of different stellar sources within Wd 1, including both evolved high mass and low mass pre-MS stars. We attribute the X-ray emission from the high mass component to both single stars and colliding wind binaries on the basis of their observed flux and spectral properties, with binaries being systematically harder and more luminous than single stars. We are able to infer a high binary fraction for both WN (10/16) and WC stars (7/8), resulting in a combined Wolf Rayet binary fraction of > ∼ 70%. These represent the most stringent limits currently placed on the binary fraction of very massive (>45 M ) stars. We place the first observational constraints on X-ray emission from stars transitioning between the Main Sequence and Wolf Rayet phases, finding that both hot (B hypergiants) and cool (yellow hypergiants and red supergiants) spectral types appear to be intrinsically X-ray faint. The B[e] star W9 is found to be X-ray bright and shows similarities to both the X-ray binary SS433 and the Luminous Blue Variable η Carinae. Globally, we find the point source population to be systematically fainter than those found in younger massive star forming regions such as NGC 3603 and R136/30 Doradus, consistent with a loss of the most massive stars to SNe and a reduction in emissivity from the low mass pre-Main Sequence stars. No unambiguous evidence for X-ray emission due to accretion onto relativistic objects of any mass is found, although the current data do not exclude the presence of either a High Mass X-ray Binary or an Intermediate Mass Black Hole accreting at a low rate. Finally, we suggest the progenitor mass for the magnetar CXOU J164710.2-455216 is comparable to that of SGR 1806-20 (∼55 M ), while that for SGR 1900+14 appears significantly lower (∼15 M ), implying that magnetars may form from stars with a wide range of initial masses.

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“…There are two models for the ejection of runaway stars (Gies & Bolton 1986). When the most massive member of a binary explodes as a supernova, the orbital motion of the companion can be converted into linear motion (Tauris & Takens 1998;Hoogerwerf et al 2000Hoogerwerf et al , 2001Dray et al 2005). Alternatively, ejections can occur by N-body interactions in dense clusters, interactions between single stars and binaries, binaries and binaries, or the dynamical decay of non-hierarchical groups (Gualandris et al 2004;Gvaramadze & Gualandris 2011).…”

Section: Ejection Of Runaway Stars: Bn Source I and Source Nmentioning

confidence: 99%

The ALMA View of the OMC1 Explosion in Orion

Bally¹,

Ginsburg²,

Arce

et al. 2017

ApJ

103

157

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Most massive stars form in dense clusters where gravitational interactions with otherstars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of ∼29 and ∼13 km s −1 about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred 12 CO J=2−1 streamers with velocities extending from V LSR =−150 to +145 km s −1 . The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a "Hubble Flow" confined to within 50″ of the explosion center. They point toward the high proper-motion, shockexcited H 2 and [Fe II] "fingertips" and lower-velocity CO in the H 2 wakes comprising Orionʼs "fingers." In some directions, the H 2 "fingers" extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N-body interaction that ejected the stars and produced the explosion. This ∼10 48 erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.

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Wolf--Rayet and O star runaway populations from supernovae

Cited by 37 publications

References 56 publications

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Unveiling the X-ray point source population of the Young Massive Cluster Westerlund 1

The ALMA View of the OMC1 Explosion in Orion

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