Detection of nonthermal emission from the bow shock of a massive runaway star

Benaglia, P.; Romero, Gustavo E.; Martı́, Josep; Peri, C. S.; Araudo, Anabella T.

doi:10.1051/0004-6361/201015232

Cited by 80 publications

(174 citation statements)

References 20 publications

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“…Benaglia et al (2010) detected radio emission from the bow shock produced by the runaway star BD+43 3654, consistent with synchrotron radiation produced by the interaction of the relativistic electrons with the magnetic field of the acceleration region. Later, del Valle & Romero (2012) presented a nonthermal emission model that predicted the production of high-energy photons in these acceleration regions in sufficiently large numbers to be detected in X-rays.…”

Section: Introductionmentioning

confidence: 63%

“…The most massive object is now seen as an O4If. BD+43 3654 has been reported to have formed a bow shock detected in the IR (Comerón & Pasquali 2007) and in radio (Benaglia et al 2010). These two observations are coincident and extensive.…”

Section: Bd+43 3654mentioning

confidence: 99%

“…Further details on the nonthermal processes are also found in Adams (1980), Kelner et al (2006), Longair (2011) or Rybicki & Lightman (1979). Other contributions to explain the high-energy emission from the bow shocks produced by runaway stars are those of Benaglia et al (2010), Terada et al (2012), and del Valle & Romero (2014). …”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 63%

Section: Bd+43 3654mentioning

confidence: 99%

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Modeling nonthermal emission from stellar bow shocks

Pereira

López‐Santiago

Miceli

et al. 2016

A&A

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“…As a result, this study does not concern massive X-ray and/or γ-ray binaries or microquasars that include a compact object (Fender & Maccarone 2004;Khangulyan & Aharonian 2005;Bosch-Ramon 2007;Bosch-Ramon & Rieger 2011) and is neither related to supernova remnants, known to be efficient particle accelerators (Romero 2004;Reynolds 2011;Vink 2013). Moreover, the class of objects debated does not include rapidlymoving runaway massive stars whose stellar wind interacts with the interstellar medium, producing strong shocks likely to accelerate particles (Benaglia et al 2010b;Romero et al 2011;Peri et al 2011;del Valle & Romero 2012).…”

Section: The Cataloguementioning

confidence: 99%

Catalogue of particle-accelerating colliding-wind binaries

Becker

Raucq

2013

A&A

115

138

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Massive systems made of two or more stars are known to be the site for interesting physical processes -including at least in some cases -particle acceleration. Over the past decade, this topic motivated a particular effort to unveil the properties of these systems and characterize the circumstances responsible for the acceleration of particles and the potential role of pre-supernova massive stars in the production of high energy particles in our Galaxy. Although previous studies on this topic were mostly devoted to processes in general, or to a few individual objects in particular, a unified target-oriented census of particle-accelerating colliding-wind binaries (hereafter PACWBs) does not exist yet. This paper aims at making a general and unified census of these systems, emphasizing their main properties. A general discussion includes energetic considerations along with wind properties in relation with non-thermal emission processes that are likely at work in colliding-wind binaries. Finally, some guidelines for future observational and theoretical studies are drawn.

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“…Benaglia et al (2010) have reported non-thermal radio emission from the bowshock of the runaway star BD +43 • 3654. This emission is thought to be synchrotron radiation generated by the interaction of relativistic electrons with the magnetic field of the source.…”

Section: Introductionmentioning

confidence: 99%

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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Detection of nonthermal emission from the bow shock of a massive runaway star

Cited by 80 publications

References 20 publications

Modeling nonthermal emission from stellar bow shocks

Modeling nonthermal emission from stellar bow shocks

Catalogue of particle-accelerating colliding-wind binaries

Non-thermal processes in bowshocks of runaway stars

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