A Parsec-Size Bow Shock around Betelgeuse

Noriega-Crespo, A.; Buren, D. van; Cao, Yu; Dgani, Ruth

doi:10.1086/118517

Cited by 78 publications

(89 citation statements)

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“…The AKARI flux is 10.7 Jy and 6.9 Jy at 65 μm and 90 μm, respectively (Ueta et al 2008, private comm. ), and the IRAS fluxes are significantly greater with 110 ± 20 Jy and 40 ± 10 Jy at 60 μm and 100 μm, respectively (Noriega-Crespo et al 1997). The derived luminosities are given in Table 4 and show that, while the IRAS luminosities exceed the theoretical upper limit, the AKARI values are consistent given the uncertainties.…”

Section: Luminosity Of the Bow Shockmentioning

confidence: 58%

“…Thus, to decrease the shell mass from a steady state value of 0.05 M to 0.0033 M requires that we decrease the mass-loss rate by a factor of 15, i.e.Ṁ = 2×10 −7 M yr −1 , somewhat below the lowest estimate of Young et al (1993a). The latter was derived from CO observations, which tends to underestimate the true massloss rate due to incomplete CO synthesis in Betelgeuse's stellar wind (Noriega-Crespo et al 1997). Although this lower massloss rate and a higher wind velocity cannot be excluded, they are outlying values in the range of observations so must be considered unlikely.…”

Section: Comparison With Previous Studiesmentioning

confidence: 86%

“…Stencel et al 1988;Young et al 1993b). However, because the star is so bright at these wavelengths, it was only in 1997 that the bow shock was imaged successfully using IRAS at 60 and 100 μm (Noriega-Crespo et al 1997). More recently, Ueta et al (2008) have imaged the bow shock with AKARI at higher spatial resolution in the 65, 90, 140, and 160 μm bands.…”

Section: Introductionmentioning

confidence: 99%

“…(3) Bernat et al (1979). (4) Noriega-Crespo et al (1997). (5) Observed ISM density of the Orion Nebulae Complex (ONC), Frisch et al (1990).…”

Section: Introductionmentioning

confidence: 99%

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3D simulations of Betelgeuse’s bow shock

Mohamed

Mackey²,

Langer³

2012

A&A

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Betelgeuse, the bright, cool red supergiant in Orion, is moving supersonically relative to the local interstellar medium. The star emits a powerful stellar wind that collides with this medium, forming a cometary structure, a bow shock, pointing in the direction of motion. We present the first 3D hydrodynamic simulations of the formation and evolution of Betelgeuse's bow shock. The models include realistic low-temperature cooling and cover a range of plausible interstellar medium densities of 0.3-1.9 cm −3 and stellar velocities of 28-73 km s −1 . We show that the flow dynamics and morphology of the bow shock differ substantially because of the growth of Rayleigh-Taylor or Kelvin-Helmholtz instabilities. The former dominate the models with slow stellar velocities resulting in a clumpy bow shock substructure, whereas the latter produce a smoother, more layered substructure in the fast models. If the mass in the bow shock shell is low, as seems to be implied by the AKARI luminosities (∼3 × 10 −3 M ), then Betelgeuse's bow shock is very young and is unlikely to have reached a steady state. The circular nature of the bow shock shell is consistent with this conclusion. Thus, our results suggest that Betelgeuse only entered the red supergiant phase recently.

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Section: Luminosity Of the Bow Shockmentioning

confidence: 58%

Section: Comparison With Previous Studiesmentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

“…(3) Bernat et al (1979). (4) Noriega-Crespo et al (1997). (5) Observed ISM density of the Orion Nebulae Complex (ONC), Frisch et al (1990).…”

Section: Introductionmentioning

confidence: 99%

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3D simulations of Betelgeuse’s bow shock

Mohamed

Mackey²,

Langer³

2012

A&A

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“…A few of them are identified as evolved massive stars and three of them are red supergiants with detected bow shocks, i.e. Betelgeuse (Noriega-Crespo et al 1997;Decin et al 2012), µ Cep (Cox et al 2012) and IRC−10414 . Consequently, and because these stars will explode as core-collapse supernova, their circumstellar medium is of prime interest in the study of aspherical supernova remnants.…”

Section: Introductionmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Astrospheres of Planet-Hosting Cool Stars and Beyond ⋅ When Modeling Meets Observations

et al. 2022

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Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope, Kepler, and TESS, we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer $\text{H}\upalpha$ H α projections to $1~\text{pc}$ 1 pc , we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations.

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A Parsec-Size Bow Shock around Betelgeuse

Cited by 78 publications

References 0 publications

3D simulations of Betelgeuse’s bow shock

3D simulations of Betelgeuse’s bow shock

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Astrospheres of Planet-Hosting Cool Stars and Beyond ⋅ When Modeling Meets Observations

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