The Prototype Colliding‐Wind Pinwheel WR 104

Tuthill, P. G.; Monnier, John D.; Lawrance, Nicholas; Danchi, W. C.; Owocki, Stan; Gayley, K. G.

doi:10.1086/527286

Cited by 124 publications

(148 citation statements)

References 65 publications

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“…Cases in which inconsistent distances have been reported in the literature are discussed further in Appendix B. Tuthill et al (2008), (5) Hillenbrand et al (1993), (6) Djurašević et al (2001), (7)Smith (2006), (8) Hur, Sung & Bessell (2012), (9) Davies et al (2012a), (10) Cappa et al (2010), (11) Lundström & Stenholm (1984), (12) Vazquez et al (1995), (13) Kothes & Dougherty (2007), (14) Koumpia & Bonanos (2012), (15) Martín, Cappa & Testori (2007), (20) Esteban & Rosado (1995), (21) Schweickhardt et al (1999). Distance references (1-22 as in Table 1): (23) Arnal et al (1999), (24)Crowther, Smith & Hillier (1995b), (25) Tovmassian, Navarro & Cardona (1996), (26) Howarth & Schmutz (1995), (27) Cappa et al (1999), (28) , (29) Garmany & Stencel (1992), (30) Bohannan & Crowther (1999).…”

Section: Calibration Samplementioning

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

128

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: Calibration Samplementioning

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

128

143

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“…The ring-like and possible spiral structure in NaSt1 brings to mind the specific cases of WR 98a and WR 104 (Monnier et al , 2002Tuthill et al 1999Tuthill et al , 2008, which are CWBs containing WC stars surrounded by striking Archimedean spirals of hot dust emission viewed nearly face on (the so-called 'pinwheel' nebulae). The dust in these systems is thought to be produced when a carbon-rich wind from a WC star mixes with the H-rich wind of a less-evolved OB companion, creating chemistry suitable for the formation of graphite or silicates.…”

Section: Dust Formation From Colliding Winds?mentioning

confidence: 99%

Multiwavelength observations of NaSt1 (WR 122): equatorial mass loss and X-rays from an interacting Wolf–Rayet binary

Mauerhan

Smith

Dyk

et al. 2015

Monthly Notices of the Royal Astronomical Society

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NaSt1 (aka Wolf-Rayet 122) is a peculiar emission-line star embedded in an extended nebula of [N ii] emission with a compact dusty core. This object was characterized by Crowther & Smith (1999) as a Wolf-Rayet (WR) star cloaked in an opaque nebula of CNO-processed material, perhaps analogous to η Car and its Homunculus nebula, albeit with a hotter central source. To discern the morphology of the [N ii] nebula we performed narrowband imaging using the Hubble Space Telescope and Wide-field Camera 3. The images reveal that the nebula has a disk-like geometry tilted ≈12 • from edge-on, composed of a bright central ellipsoid surrounded by a larger clumpy ring. Ground-based spectroscopy reveals radial velocity structure (±10 km s −1 ) near the outer portions of the nebula's major axis, which is likely to be the imprint of outflowing gas. Near-infrared adaptive-optics imaging with Magellan AO has resolved a compact ellipsoid of K s -band emission aligned with the larger [N ii] nebula, which we suspect is the result of scattered He i line emission (λ2.06 µm). Observations with the Chandra X-ray Observatory have revealed an X-ray point source at the core of the nebula that is heavily absorbed at energies < 1 keV and has properties consistent with WR stars and colliding-wind binaries. We suggest that NaSt1 is a WR binary embedded in an equatorial outflow that formed as the result of non-conservative mass transfer. NaSt1 thus appears to be a rare and important example of a stripped-envelope WR forming through binary interaction, caught in the brief Roche-lobe overflow phase.

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“…5). The infrared emission is very well-matched by an Archimedean spiral, although its brightest point is shifted by 13 milli-arcsec from its centre, possibly because dust formation is inhibited at smaller radii (Tuthill et al 2008. The WR wind is hostile to dust formation owing to its high temperature, low density, and absence of hydrogen (Cherchneff et al 2000).…”

Section: Introductionmentioning

confidence: 99%

“…The wind velocity to use is unclear. Tuthill et al (2008) took the speed of the dominant wind v 1 (dominant in the sense thatṀ 1 v 1 ≥Ṁ 2 v 2 ), whereas Parkin & Pittard (2008) assumed that it is the slower wind that determines the step of the spiral but focus their study on binaries with equal wind velocities. Simple dynamical models of the shocked layer have been developed for use with radiative transfer codes, assuming that the double shock structure is infinitely thin (thin shell hypothesis) and that the material is ballistic (Harries et al 2004;Parkin & Pittard 2008).…”

Section: Introductionmentioning

confidence: 99%

Impact of orbital motion on the structure and stability of adiabatic shocks in colliding wind binaries

Lamberts

Dubus

Lesur

et al. 2012

A&A

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Context. The collision of winds from massive stars in binaries results in the formation of a double-shock structure with observed signatures from radio to X-rays. Aims. We study the structure and stability of the colliding wind region as it turns into a spiral owing to the orbital motion. We focus on adiabatic winds, where mixing between the two winds is expected to be restricted to the Kelvin-Helmholtz instability. Mixing of the Wolf-Rayet wind with hydrogen-rich material is important for dust formation in pinwheel nebulae such as WR 104, where the spiral structure has been resolved in infrared. Methods. We use the hydrodynamical code RAMSES to solve the equations of hydrodynamics on an adaptive grid. A wide range of binary systems with different wind velocities and mass-loss rates are studied with two-dimensional simulations. A specific threedimensional simulation is performed to model WR 104. Results. Orbital motion leads to the formation of two distinct spiral arms where the Kelvin-Helmholtz instability develops differently. We find that the spiral structure is destroyed when there is a large velocity gradient between the winds, unless the collimated wind is much faster. We argue that the Kelvin-Helmholtz instability plays a major role in determining whether the structure is maintained. We discuss the consequences for various colliding-wind binaries. When their spiral structure is stable, there is no straightforward relationship between the spatial step of the spiral, the wind velocities, and the orbital period. Our 3D simulation of WR 104 indicates that the colder, well-mixed trailing arm has more favourable conditions for dust formation than the leading arm. The single-arm infrared spiral follows more closely the mixing map than the density map, suggesting that the dust-to-gas ratio may vary between the leading and trailing density spirals. However, the density is much lower than what dust formation models require. Including radiative cooling would lead to higher densities, and also to thin shell instabilities whose impact on the large-scale structure remains unknown.

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The Prototype Colliding‐Wind Pinwheel WR 104

Cited by 124 publications

References 65 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

Multiwavelength observations of NaSt1 (WR 122): equatorial mass loss and X-rays from an interacting Wolf–Rayet binary

Impact of orbital motion on the structure and stability of adiabatic shocks in colliding wind binaries

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