Search for systemic mass loss in Algols with bow shocks

Mayer, Andreas; Deschamps, Romain; Jorissen, A.

doi:10.1051/0004-6361/201526623

Cited by 7 publications

(5 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Bow shock structures have been observed in the far-IR around different stellar objects, e.g. AGBs, red supergiants and Algols (Ueta et al 2008;Jorissen et al 2011;Cox et al 2012;Mayer et al 2016). First of all, we checked if the velocity direction of HR Car is compatible with the location of the bow shock.…”

Section: Discussionmentioning

confidence: 99%

Exploring the multifaceted circumstellar environment of the luminous blue variable HR Carinae

Buemi

Trigilio

Leto

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a multi-wavelength study of the Galactic Luminous Blue Variable HR Carinae, based on new high resolution mid-infrared (IR) and radio images obtained with the Very Large Telescope (VLT) and the Australia Telescope Compact Array (ATCA), which have been complemented by far-infrared Herschel-PACS observations and ATCA archive data. The Herschel images reveal the large-scale distribution of the dusty emitting nebula, which extends mainly to the North-East direction, up to 70 arcsec from the central star, and is oriented along the direction of the space motion of the star. In the mid-infrared images, the brightness distribution is characterized by two arc-shaped structures, tracing an inner envelope surrounding the central star more closely. At radio wavelengths, the ionized gas emission lies on the opposite side of the cold dust with respect to the position of the star, as if the ionized front was confined by the surrounding medium in the North-South direction. The comparison with previous data indicates significant changes in the radio nebula morphology and in the massloss rate from the central star, which has increased from 6.1×10 −6 M ⊙ yr −1 in 1994-1995 to 1.17 × 10 −5 M ⊙ yr −1 in 2014. We investigate possible scenarios that could have generated the complex circumstellar environment revealed by our multi-wavelength data.

show abstract

Section: Discussionmentioning

confidence: 99%

Exploring the multifaceted circumstellar environment of the luminous blue variable HR Carinae

Buemi

Trigilio

Leto

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The wispy nebula, fanning approximately in the Galactic northsouth direction, may suggest a dusty outflow indicating a systemic mass loss. The nebula bears some resemblance to circum-stellar nebulae observed around some B[e] and Be stars in the infrared images (Mayer et al 2016). The literature on the enviroments around Be stars is sparse, but at least one Be star, SX Aur, also shows the presence of a mid-infrared nebula (Deschamps et al 2015), however, this nebula is more compact and shows a blob-like morphology instead of fine wispy jets.…”

Section: Exo 051910+37377 Nebulamentioning

confidence: 69%

Concerning the occurrence of bow shocks around high-mass X-ray binaries

Prišegen

2019

A&A

View full text Add to dashboard Cite

Context. We investigate the occurrence of stellar bow shocks around high-mass X-ray binaries (HMXBs) in the Galaxy. Aims. We seek to conduct a survey of HMXBs in the mid-infrared to search for the presence of bow shocks around these objects. Methods. Telescopes operating in the mid-infrared, such as the Spitzer Space Telescope or Wide-field Infrared Survey Explorer (WISE), are potent tools for searching for the stellar bow shocks. We used the available archival data from these telescopes to search for bow shock candidates around the confirmed and candidate HMXBs in the Galaxy. Results. We detected extended mid-infrared structures around several surveyed confirmed and candidate HMXBs. Two of these structures, associated with Vela X-1 and 4U 1907+09, are genuine bow shocks that have been studied previously. However, there are no new unambiguous bow shocks among the rest of the objects. The paucity of bow shocks around HMXBs suggests that the majority of these systems still reside within hot, low-density bubbles around their parent star clusters or associations. This also implies that the dynamical ejection of massive binaries is apparently less efficient than the ejections caused by the supernova explosions inside a binary.

show abstract

“…The superimposed propermotion vectors illustrate the classifications by Bodensteiner et al (2018) for γ Cas and π Aqr, respectively. A bow shock can be seen to be associated with π Aqr (see also Mayer et al 2016). However, the apex of the nebula is not aligned with the propermotion vector.…”

Section: Impact Of a Supernova Explosion On Space Velocitymentioning

confidence: 97%

γCas stars: Normal Be stars with discs impacted by the wind of a helium-star companion?

Langer

Baade

Bodensteiner

et al. 2020

A&A

View full text Add to dashboard Cite

γ Cas stars are a ∼1% minority among classical Be stars with hard (≥5-10 keV) but only moderately strong continuous thermal X-ray flux and mostly very early-B spectral type. The X-ray flux has been suggested to originate from matter accelerated via magnetic diskstar interaction, by a rapidly rotating neutron star (NS) companion via the propeller effect, or by accretion onto a white dwarf (WD) companion. In view of the growing number of identified γ Cas stars and the only imperfect matches between these suggestions and the observations, alternative models should be pursued. Two of the three best-observed γ Cas stars, γ Cas itself and π Aqr, have a low-mass companion with low optical flux; interferometry of BZ Cru is inconclusive. Binary-evolution models are examined for their ability to produce such systems. The OB+He-star stage of post-mass transfer binaries, which is otherwise observationally unaccounted, can potentially reproduce many observed properties of γ Cas stars. The interaction of the fast wind of helium stars with the circumstellar disk and/or with the wind of Be stars may give rise to the production of hard X-rays. While not modelling this process, it is shown that the energy budget is favourable, and that the wind velocities may lead to hard X-rays as observed in γ Cas stars. Furthermore, the observed number of these objects appears to be consistent with the evolutionary models. Within the Be+He-star binary model, the Be stars in γ-Cas stars are conventional classical Be stars. They are encompassed by O-star+Wolf-Rayet systems towards higher mass, where no stable Be decretion disks exist, and by Be+sdO systems at lower mass where the sdO winds may be too weak to cause the γ Cas phenomenon. In decreasing order of the helium-star mass, the descendants could be Be+black-hole, Be+NS or Be+WD binaries. The interaction between the helium-star wind and the disk may provide new diagnostics of the outer disk.

show abstract

Search for systemic mass loss in Algols with bow shocks

Cited by 7 publications

References 40 publications

Exploring the multifaceted circumstellar environment of the luminous blue variable HR Carinae

Exploring the multifaceted circumstellar environment of the luminous blue variable HR Carinae

Concerning the occurrence of bow shocks around high-mass X-ray binaries

γCas stars: Normal Be stars with discs impacted by the wind of a helium-star companion?

Contact Info

Product

Resources

About