Young massive binary θ 1 OriC: Radial velocities of components

Balega, Yu. Yu.; Ченцов, Е. Л.; Леушин, В. В.; Рзаев, А. Х.; Weigelt, G.

doi:10.1134/s1990341314010052

Cited by 19 publications

(24 citation statements)

References 17 publications

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“…This is an important fact for investigating the details of stellar models, which is not possible without photometric information on the components of binary systems. Recent data on these studies and references to previous works can be found in Balega et al (2007Balega et al ( , 2010). Horch et al (2011) presented the results of speckle observations of Hipparcos stars and other selected targets.…”

Section: Speckle Interferometrymentioning

confidence: 97%

“…Horch et al (2011) presented the results of speckle observations of Hipparcos stars and other selected targets. Balega et al (2010) obtained the orbital period of 12.95 ± 0.05 years, the semimajor axis of 197.7 ± 1.6 mas and the dynamical total mass of 1.40±0.56M . Since the first paper in this series (Horch et al 2009), the instru-ment has been upgraded so that it now uses two electron-multiplying CCD cameras.…”

Section: Speckle Interferometrymentioning

confidence: 99%

“…Baron et al (2012) presented the results of Algol observations made between 2006 and 2010 at the CHARA interferometer with the Michigan Infrared Combiner in the H-band. Baron et al (2012) presented the results of Algol observations made between 2006 and 2010 at the CHARA interferometer with the Michigan Infrared Combiner in the H-band.…”

Section: Binary Star Astrometry With Milli and Sub-milli Arcsecond Prmentioning

confidence: 99%

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Binary star astrometry with milli and sub-milli arcsecond precision

2014

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The past several decades have seen accelerating progress in improving binary stars fundamental parameters determinations, as new observational techniques have produced visual orbits of many spectroscopic binaries with a milli arcsecond precision. Modern astrometry is rapidly approaching the goal of sub-milli arcsecond precision, and although presently this precision has been achieved only for a limited number of binary stars, in the near future this will become a standard for very large number of objects. In this paper we review the representative results of techniques which have already allowed the sub-milli arcsecond precision like the optical long baseline interferometry, as well as the precursor techniques such as speckle interferometry, adaptive optics and aperture masking. These techniques provide a step forward from milli to sub-milli arcsecond precision, allowing even short period binaries to be resolved, and often resulting in orbits allowing precisions in stellar dynamical masses better than 1%. We point out that such unprecedented precisions should allow for a significant improvement of our comprehension of stellar physics and other related astrophysical topics.

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Section: Speckle Interferometrymentioning

confidence: 97%

Section: Speckle Interferometrymentioning

confidence: 99%

Section: Binary Star Astrometry With Milli and Sub-milli Arcsecond Prmentioning

confidence: 99%

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Binary star astrometry with milli and sub-milli arcsecond precision

2014

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“…Gurvich et al 2020). The Orion Veil nebula is driven largely by a single young massive star, 1 Ori C, which has a mass of 33 M (Balega et al 2014), with error bars of 5 M that cover the 30 M star we simulate.…”

Section: Comparison With Observationsmentioning

confidence: 98%

“…Pabst et al (2019) find that the X-ray emission rate of the bubble is approximately 4 × 10 31 erg / s. This is roughly an order of magnitude lower than the cooling rate of hot gas in Figure 5, although they claim that many X-rays in Orion are absorbed by Figure 9. Evolution of the wind bubble's maximum radius from the star, w,max and the expansion velocity of the wind bubble w,max in UVWINDPRESS30, the simulation most closely matching 1 Ori C (Balega et al 2014) and its host cloud (Geen et al 2017). w,max is defined as the rate of change in w,max .…”

Section: Bulk Wind Bubble Propertiesmentioning

confidence: 99%

The geometry and dynamical role of stellar wind bubbles in photoionized H ii regions

Geen

Bieri

Rosdahl

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Winds from young massive stars contribute a large amount of energy to their host molecular clouds. This has consequences for the dynamics and observable structure of star-forming clouds. In this paper, we present radiative magnetohydrodynamic simulations of turbulent molecular clouds that form individual stars of 30, 60 and 120 solar masses emitting winds and ultraviolet radiation following realistic stellar evolution tracks. We find that winds contribute to the total radial momentum carried by the expanding nebula around the star at 10% of the level of photoionisation feedback, and have only a small effect on the radial expansion of the nebula. Radiation pressure is largely negligible in the systems studied here. The 3D geometry and evolution of wind bubbles is highly aspherical and chaotic, characterised by fast-moving “chimneys” and thermally-driven “plumes”. These plumes can sometimes become disconnected from the stellar source due to dense gas flows in the cloud. Our results compare favourably with the findings of relevant simulations, analytic models and observations in the literature while demonstrating the need for full 3D simulations including stellar winds. However, more targeted simulations are needed to better understand results from observational studies.

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