E-BOSS: an Extensive stellar BOw Shock Survey

Peri, C. S.; Benaglia, P.; Brookes, D. P.; Stevens, I. R.; Isequilla, N. L.

doi:10.1051/0004-6361/201118116

Cited by 119 publications

(175 citation statements)

References 61 publications

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“…Our work suggests that bowshocks of runaway stars might constitute a new class of high-energy sources to be explored in the near future. Figure 11 shows the SED for the emission from the bowshock of ζ Oph, along with the sensitivity of the gammaray detectors CTA (Cherenkov Telescope Array-forthcoming-), MAGIC and Fermi, the X-ray satellite XMM-Newton (theoretical upper limit from Hasinger et al 2001), and VLA (upper limit from the NVSS survey -Condon, Cotton, Greisen et al 1998 -, angular resolution is given by Peri et al 2011). For completeness the IR IRAS data are also shown (Van Buren & MacCray 1988).…”

Section: Discussionmentioning

confidence: 99%

“…From the WISE image of the bowshock of ζ Oph it is evident that the midpoint from the star to the bowshock (see Fig. 4 from Peri et al 2011) is in the direction of the star velocity. Figure 8 shows the best fit of ζ Oph bowshock.…”

Section: Bowshock Shapementioning

confidence: 98%

“…Van Buren et al 1995;Noriega-Crespo et al 1997;Kobulnicky et al 2009;Gvaramadze et al 2011;Peri et al 2011). Not all runaway stars produce a bowshock.…”

Section: Introductionmentioning

confidence: 99%

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Non-thermal processes in bowshocks of runaway stars

Valle¹,

Romero²

2012

A&A

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Context. Runaway massive stars are O-and B-type stars with high spatial velocities with respect to the interstellar medium. These stars can produce bowshocks in the surrounding gas. Bowshocks develop as arc-shaped structures, with bows pointing to the same direction as the stellar velocity, while the star moves supersonically through the interstellar gas. The piled-up shocked matter emits thermal radiation and a population of locally accelerated relativistic particles is expected to produce non-thermal emission over a wide range of energies. Aims. We aim to model the non-thermal radiation produced in these sources. Methods. Under some assumptions, we computed the non-thermal emission produced by the relativistic particles and the thermal radiation caused by free-free interactions, for O4I and O9I stars. We applied our model to ζ Oph (HD 149757), an intensively studied massive star seen from the northern hemisphere. This star has spectral type O9.5V and is a well-known runaway. Results. Spectral energy distributions of massive runaways are predicted for the whole electromagnetic spectrum. Conclusions. We conclude that the non-thermal radiation might be detectable at various energy bands for relatively nearby runaway stars, especially at high-energy gamma rays. Inverse Compton scattering with photons from the heated dust gives the most important contribution to the high-energy spectrum. This emission approaches Fermi sensitivities in the case of ζ Oph.

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Section: Discussionmentioning

confidence: 99%

Section: Bowshock Shapementioning

confidence: 98%

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Non-thermal processes in bowshocks of runaway stars

Valle¹,

Romero²

2012

A&A

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“…Both the electron injection index and the fraction of relativistic energy were fitted to the available observational data points. The IR shock widths were taken from Peri et al (2012). However, the nonthermal emission is produced from a smaller region, concentrated in a small knot at the bow shock apex, and hence the final shock width was also obtained from fitting the observational data.…”

Section: Applicationsmentioning

confidence: 99%

Modeling nonthermal emission from stellar bow shocks

Pereira

López‐Santiago

Miceli

et al. 2016

A&A

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Context. Runaway O-and early B-type stars passing through the interstellar medium at supersonic velocities and characterized by strong stellar winds may produce bow shocks that can serve as particle acceleration sites. Previous theoretical models predict the production of high-energy photons by nonthermal radiative processes, but their efficiency is still debated. Aims. We aim to test and explain the possibility of emission from the bow shocks formed by runaway stars traveling through the interstellar medium by using previous theoretical models. Methods. We applied our model to AE Aurigae, the first reported star with an X-ray detected bow shock, to BD+43 3654, in which the observations failed in detecting high-energy emission, and to the transition phase of a supergiant star in the late stages of its life. Results. From our analysis, we confirm that the X-ray emission from the bow shock produced by AE Aurigae can be explained by inverse Compton processes involving the infrared photons of the heated dust. We also predict low high-energy flux emission from the bow shock produced by BD+43 3654, and the possibility of high-energy emission from the bow shock formed by a supergiant star during the transition phase from blue to red supergiant. Conclusions. Bow shocks formed by different types of runaway stars are revealed as a new possible source of high-energy photons in our neighborhood.

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“…van Buren, Noriega-Crespo & Dgani 1995). Nowadays, with the advent of the Spitzer Space Telescope, Wide-field Infrared Survey Explorer (WISE) and Herschel Space Observatory, many hundreds of new astrospheres were revealed (Peri et al 2012;Cox et al 2012; Kobulnicky et al…”

Section: Introductionmentioning

confidence: 99%

An astrosphere around the blue supergiant κ Cas: possible explanation of its filamentary structure

Katushkina

Alexashov

Gvaramadze

et al. 2017

Monthly Notices of the Royal Astronomical Society

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High-resolution mid-infrared observations carried out by the Spitzer Space Telescope allowed one to resolve the fine structure of many astrospheres. In particular, they showed that the astrosphere around the B0.7 Ia star κ Cas (HD 2905) has a clear-cut arc structure with numerous cirrus-like filaments beyond it. Previously, we suggested a physical mechanism for the formation of such filamentary structures. Namely, we showed theoretically that they might represent the non-monotonic spatial distribution of the interstellar dust in astrospheres (viewed as filaments) caused by interaction of the dust grains with the interstellar magnetic field disturbed in the astrosphere due to colliding of the stellar and interstellar winds. In this paper, we invoke this mechanism to explain the structure of the astrosphere around κ Cas. We performed 3D magnetohydrodynamic modelling of the astrosphere for realistic parameters of the stellar wind and space velocity. The dust dynamics and the density distribution in the astrosphere were calculated in the framework of a kinetic model. It is found that the model results with the classical MRN size distribution of dust in the interstellar medium do not match the observations, and that the observed filamentary structure of the astrosphere can be reproduced only if the dust is composed mainly of big (µm-sized) grains. Comparison of the model results with observations allowed us to estimate parameters (number density and magnetic field strength) of the surrounding interstellar medium.

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E-BOSS: an Extensive stellar BOw Shock Survey

Cited by 119 publications

References 61 publications

Non-thermal processes in bowshocks of runaway stars

Non-thermal processes in bowshocks of runaway stars

Modeling nonthermal emission from stellar bow shocks

An astrosphere around the blue supergiant κ Cas: possible explanation of its filamentary structure

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