Binary outflows from young stars: interaction of co-orbital jet and wind

Lynch, Chris J.R.; Smith, Michael D.; Glover, Simon C. O.

doi:10.1093/mnras/stz2985

Cited by 3 publications

(3 citation statements)

References 38 publications

(51 reference statements)

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“…In Paper 1 (Lynch et al 2019), we summarised the interpretations and parameters which have been previously found to be consistent with both models as applied to HH 30. We also detailed the physical, chemical and dynamical modifications to the ZEUS-MP code (Hayes et al 2006), and listed the full set of simulations.…”

Section: Introductionmentioning

confidence: 93%

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The nature of a primary jet within a circumbinary disc outflow in a young stellar system

Lynch

Smith

2020

Monthly Notices of the Royal Astronomical Society

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Most stars form in binaries, and both stars may grow by accreting material from a circumbinary disc onto their personal discs. We suspect that in many cases a wide molecular wind will envelope a collimated atomic jet emanating from close to an orbiting young star. This so-called Circumbinary Scenario is explored here in order to find common identifiable properties. The dynamical set up is studied with three dimensional simulations with chemistry and cooling included. We extract the properties on scales of order 100 AU and compare to the Co-Orbital Scenario in which the wind and jet sources are in orbit. We find that the rapid orbital motion generates a wide ionised sheath around the jet core with a large opening angle at the base. This is independent of the presence of the surrounding molecular outflow. However, the atomic jet is recollimated beyond ∼ 55 AU when the molecular outflow restricts the motion of the ambient medium which, in turn, confines the jet. These physical properties are relayed to the optical Hα imaging, providing a means of distinguishing between models. The high excitation sheath and recollimation region can be explored on these scales through the next generation of instruments. However, in general, the amount and location of the ionised material, whether in the knots or the sheath, will depend on several parameters including the orbital period, axis alignment and pulse amplitude.

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Section: Introductionmentioning

confidence: 93%

“…Both jets were narrow and had a short dynamical flow time so that the long orbital time had little influence. This was remedied in Paper 1 (Lynch et al 2019) where the Co-orbital Scenario was fully explored. In that case, as illustrated in Fig.…”

Section: Introductionmentioning

confidence: 99%

The nature of a primary jet within a circumbinary disc outflow in a young stellar system

Lynch

Smith

2020

Monthly Notices of the Royal Astronomical Society

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“…A prominent example of an edge-on circumbinary disk cavity in the center is HH30. The cavity is supposed to be caused by a binary with 0.31 M and 0.14 M and a separation of 18 au (Lynch et al 2019). Louvet et al (2018) proposed an alternative explanation of the cavity based on the modeling of dust continuum and molecular transition line ALMA (Atacama Large Millimeter/submillimeter Array) observations.…”

Section: Introductionmentioning

confidence: 99%

Selected aspects of the analysis of molecular line observations of edge-on circumbinary disks

Avramenko¹,

Wolf²,

Illenseer³

et al. 2020

A&A

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Context. Inner cavities, accretion arms, and density waves are characteristic structures in the density distribution of circumbinary disks. They are the result of the tidal interaction of the non-axisymmetric gravitational forces of the central binary with the surrounding disk and are most prominent in the inner region, where the asymmetry is most pronounced. Aims. The goal of this study is to test the feasibility of reconstructing the gas density distribution and quantifying properties of structures in the inner regions of edge-on circumbinary disks using multiple molecular line observations. Methods. The density distribution in circumbinary disks is calculated with 2D hydrodynamic simulations. Subsequently, molecular line emission maps are generated with 3D radiative transfer simulations. Based on these, we investigate the observability of characteristic circumbinary structures located in the innermost region for spatially resolved and unresolved disks. Results. We find that it is possible to reconstruct the inner cavity, accretion arms, and density waves from spatially resolved multi-wavelength molecular line observations of circumbinary disks seen edge-on. For the spatially unresolved observations only, an estimate can be derived for the density gradient in the transition area between the cavity and the disk’s inner rim.

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Jets from the Upper Scorpius Variable Young Star System 2MASS J16075796-2040087 via KECK/HIRES Spectro-astrometry

Whelan,

Keppler,

Turner

et al. 2024

ApJ

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2MASS J16075796-2040087 is an ∼5 Myr young star in Upper Sco with evidence for accretion bursts on a timescale of about 15 days and, uncommonly for its age, outflows traced by multicomponent forbidden emission lines (FELs). The accretion bursts may be triggered by a companion at ∼4.6 au. We analyze HIRES spectra optimised for spectro-astrometry to better understand the origin of the several FEL velocity components and determine whether a magnetohydrodynamic (MHD) disk wind is present. The FEL high-velocity component (HVC) traces an asymmetric, bipolar jet ∼700 au long. The jet’s position angle ∼ 277° is not perpendicular to the disk. The lower-velocity emission, classified previously as a disk wind low-velocity component, is found to have more in common with the HVC and overall it is not possible to identify an MHD disk wind component. The spectro-astrometric signal of the low-velocity emission resembles those of jets and its density and ionisation fraction fall into the range of HVCs. We suggest a scenario where the accretion bursts due to the close companion power the jets past the age where such activity ends around most stars. The low-velocity emission here could come from a slow jet launched near the close companion and this emission would be blended with emission from the MHD wind.

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Binary outflows from young stars: interaction of co-orbital jet and wind

Cited by 3 publications

References 38 publications

The nature of a primary jet within a circumbinary disc outflow in a young stellar system

The nature of a primary jet within a circumbinary disc outflow in a young stellar system

Selected aspects of the analysis of molecular line observations of edge-on circumbinary disks

Jets from the Upper Scorpius Variable Young Star System 2MASS J16075796-2040087 via KECK/HIRES Spectro-astrometry

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