To see or not to see a bow shock

Brown, D.; Bomans, D. J.

doi:10.1051/0004-6361:20041054

Cited by 35 publications

(30 citation statements)

References 27 publications

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“…Hα observations by Brown & Bomans (2005). A multiwavelength study of the O5 star HD 192281 by Arnal et al (2011) revealed an Hi structure consistent with formation by a bow shock, with counterparts seen in infrared, radio continuum and CO (1-0) observations.…”

Section: Introductionmentioning

confidence: 88%

Modelling multiwavelength observational characteristics of bow shocks from runaway early-type stars

Acreman

Stevens

Harries

2015

Mon. Not. R. Astron. Soc.

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We assess the multi-wavelength observable properties of the bow shock around a runaway early type star using a combination of hydrodynamical modelling, radiative transfer calculations and synthetic imaging. Instabilities associated with the forward shock produce dense knots of material which are warm, ionised and contain dust. These knots of material are responsible for the majority of emission at far infra-red, Hα and radio wavelengths. The large scale bow shock morphology is very similar and differences are primarily due to variations in the assumed spatial resolution. However infra-red intensity slices (at 22 microns and 12 microns) show that the effects of a temperature gradient can be resolved at a realistic spatial resolution for an object at a distance of 1 kpc.

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Section: Introductionmentioning

confidence: 88%

Modelling multiwavelength observational characteristics of bow shocks from runaway early-type stars

Acreman

Stevens

Harries

2015

Mon. Not. R. Astron. Soc.

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“…van Buren & McCray 1988;van Buren et al 1995;Paper I;Gvaramadze et al 2010d,b), but can also be detected in the optical (e.g. Kaper et al 1997;Brown & Bomans 2005; Paper I) and radio (Benaglia et al 2010) wavebands. It should be noted that only a minority ( 20 per cent) of runaway OB stars are associated with (detectable) bow shocks (van Buren 1993;van Buren et al 1995;Huthoff & Kaper 2002;Gvaramadze et al 2010d).…”

Section: Search For Bow Shocksmentioning

confidence: 98%

Search for OB stars running away from young star clusters

Gvaramadze

Kniazev

Kroupa

et al. 2011

A&A

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Dynamical few-body encounters in the dense cores of young massive star clusters are responsible for the loss of a significant fraction of their massive stellar content. Some of the escaping (runaway) stars move through the ambient medium supersonically and can be revealed via detection of their bow shocks (visible in the infrared, optical or radio). In this paper, which is the second of a series of papers devoted to the search for OB stars running away from young ( < ∼ several Myr) Galactic clusters and OB associations, we present the results of the search for bow shocks around the star-forming region NGC 6357. Using the archival data of the Midcourse Space Experiment (MSX) satellite and the Spitzer Space Telescope, and the preliminary data release of the Wide-Field Infrared Survey Explorer (WISE), we discovered seven bow shocks, whose geometry is consistent with the possibility that they are generated by stars expelled from the young (∼1-2 Myr) star clusters, Pismis 24 and AH03 J1725-34.4, associated with NGC 6357. Two of the seven bow shocks are driven by the already known OB stars, HD 319881 and [N78] 34. Follow-up spectroscopy of three other bow-shockproducing stars showed that they are massive (O-type) stars as well, while the 2MASS photometry of the remaining two stars suggests that they could be B0 V stars, provided that both are located at the same distance as NGC 6357. Detection of numerous massive stars ejected from the very young clusters is consistent with the theoretical expectation that star clusters can effectively lose massive stars at the very beginning of their dynamical evolution (long before the second mechanism for production of runaway stars, based on a supernova explosion in a massive tight binary system, begins to operate) and lends strong support to the idea that probably all field OB stars have been dynamically ejected from their birth clusters. A by-product of our search for bow shocks around NGC 6357 is the detection of three circular shells typical of luminous blue variable and late WN-type Wolf-Rayet stars.

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“…O stars are luminous radiation sources, and so even though only a small fraction of the stellar radiation is absorbed by dust, the re-emitted radiation is often more luminous than that of all gas-cooling radiation (Meyer et al 2014). This explains why infrared surveys (van Buren et al 1995;Gvaramadze et al 2010bGvaramadze et al , 2011bPeri et al 2012) have been much more successful at finding bow shocks than optical searches (Brown & Bomans 2005). It may also indicate that the outer boundary of a SWB is more easily detected in IR than in optical observations.…”

Section: Introductionmentioning

confidence: 99%

Detecting stellar-wind bubbles through infrared arcs in H ii regions

Mackey

Haworth

Gvaramadze

et al. 2016

A&A

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Mid-infrared arcs of dust emission are often seen near ionizing stars within H  regions. A possible explanations for these arcs is that they could show the outer edges of asymmetric stellar wind bubbles. We use two-dimensional, radiation-hydrodynamics simulations of wind bubbles within H  regions around individual stars to predict the infrared emission properties of the dust within the H  region.We assume that dust and gas are dynamically well-coupled and that dust properties (composition, size distribution) are the same in the H  region as outside it, and that the wind bubble contains no dust. We post-process the simulations to make synthetic intensity maps at infrared wavebands using the  code. We find that the outer edge of a wind bubble emits brightly at 24 µm through starlight absorbed by dust grains and re-radiated thermally in the infrared. This produces a bright arc of emission for slowly moving stars that have asymmetric wind bubbles, even for cases where there is no bow shock or any corresponding feature in tracers of gas emission. The 24 µm intensity decreases exponentially from the arc with increasing distance from the star because the dust temperature decreases with distance. The size distribution and composition of the dust grains has quantitative but not qualitative effects on our results. Despite the simplifications of our model, we find good qualitative agreement with observations of the H  region RCW 120, and can provide physical explanations for any quantitative differences. Our model produces an infrared arc with the same shape and size as the arc around CD −38• 11636 in RCW 120, and with comparable brightness. This suggests that infrared arcs around O stars in H  regions may be revealing the extent of stellar wind bubbles, although we have not excluded other explanations.

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To see or not to see a bow shock

Cited by 35 publications

References 27 publications

Modelling multiwavelength observational characteristics of bow shocks from runaway early-type stars

Modelling multiwavelength observational characteristics of bow shocks from runaway early-type stars

Search for OB stars running away from young star clusters

Detecting stellar-wind bubbles through infrared arcs in H ii regions

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