The interactions of winds from massive young stellar objects: X-ray emission, dynamics and cavity evolution

Parkin, E. R.; Pittard, J. M.; Hoare, M. G.; Wright, N. J.; Drake, J. J.

doi:10.1111/j.1365-2966.2009.15504.x

Cited by 26 publications

(28 citation statements)

References 81 publications

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“…The overall structure of the S 106 system is very similar to bipolar nebulae formed by a combination of stellar outflows and a circumstellar disk. That the central star is undergoing significant mass loss has long been known (e.g., Drew et al 1993;Gibb & Hoare 2007;Parkin et al 2009) which is consistent with the idea that the large ionized lobes were sculpted in this way. However the origin of the central dark lane has been more controversial.…”

Section: S 106supporting

confidence: 71%

HerschelPACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050

Stock

Wolfire

Peeters

et al. 2015

A&A

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Context. Photodissociation regions (PDRs) contain a large portion of all of the interstellar matter in galaxies. Classical examples include the boundaries between ionized regions and molecular clouds in regions of massive star-formation, marking the point where all of the photons that are energetic enough to ionize hydrogen have been absorbed. Aims. To determine the physical properties of the PDRs associated with the star-forming regions IRAS 23133+6050 and S 106 and present them in the context of other Galactic PDRs associated with massive star-forming regions. Methods. We employ Herschel PACS and SPIRE spectroscopic observations to construct a full 55-650 μm spectrum of each object from which we measure the PDR cooling lines, other fine-structure lines, CO lines, and the total far-infrared flux. These measurements (and combinations thereof) are then compared to standard PDR models. Subsequently, detailed numerical PDR models are compared to these predictions, yielding additional insight into the dominant thermal processes in the PDRs and their structures. Results. We find that the PDRs of each object are very similar and can be characterized by a two-phase PDR model with a very dense, highly UV irradiated phase (n ∼ 10 6 cm −3 , G 0 ∼ 10 5 ) interspersed within a lower density, weaker radiation field phase (n ∼ 10 4 cm −3 , G 0 ∼ 10 4 ). We employed two different numerical models to investigate the data. We first used RADEX models to fit the peak of the 12 CO ladder, which in conjunction with the properties derived, yielded a temperature of around 300 K. Subsequent numerical modeling with a full PDR model revealed that the dense phase has a filling factor of around 0.6 in both objects. The shape of the 12 CO ladder was consistent with these components, with heating dominated by grain photoelectric heating. An extra excitation component for the hightest-J lines (J > 20) is required for S 106.

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Section: S 106supporting

confidence: 71%

HerschelPACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050

Stock

Wolfire

Peeters

et al. 2015

A&A

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“…It is a first-order differential equation and can be solved numerically. We imposed the boundary condition ω = 4.5 × 10 15 cm at z = 0, which is similar to those used by Parkin et al (2009). The results are not sensitive to the choice of this boundary condition.…”

Section: Shape Of the Outflow Cavitymentioning

confidence: 99%

Turbulent entrainment origin of protostellar outflows

Qiu

Wyrowski

et al. 2013

A&A

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Protostellar outflow is a prominent process that accompanies the formation of stars. It is generally agreed that wide-angled protostellar outflows come from the interaction between the wind from a forming star and the ambient gas. However, it is still unclear how the interaction takes place. In this work, we theoretically investigate the possibility that the outflow results from interaction between the wind and the ambient gas in the form of turbulent entrainment. In contrast to the previous models, turbulent motion of the ambient gas around the protostar is taken into account. In our model, the ram-pressure of the wind balances the turbulent ram-pressure of the ambient gas, and the outflow consists of the ambient gas entrained by the wind. The calculated outflow from our modelling exhibits a conical shape. The total mass of the outflow is determined by the turbulent velocity of the envelope as well as the outflow age, and the velocity of the outflow is several times higher than the velocity dispersion of the ambient gas. The outflow opening angle increases with the strength of the wind and decreases with the increasing ambient gas turbulence. The outflow exhibits a broad line width at every position. We propose that the turbulent entrainment process, which happens ubiquitously in nature, plays a universal role in shaping protostellar outflows.

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“…This way several numerical studies have succeeded in creating stars with masses of ≳30 M ⊙ (e.g. Yorke & Sonnhalter 2002; Krumholz et al 2009), while it has been shown that the fast bipolar winds should strongly influence the infalling material from the envelope (Parkin et al 2009). The observational evidence to support this scenario however is limited and circumstantial.…”

Section: Introductionmentioning

confidence: 99%

The circumstellar disc, envelope and bipolar outflow of the massive young stellar object W33A

Davies

Lumsden

Hoare

et al. 2010

Monthly Notices of the Royal Astronomical Society

109

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The young stellar object (YSO) W33A is one of the best known examples of a massive star still in the process of forming. Here we present Gemini North Altitude conjugate Adaptive optics for the Infrared (ALTAIR)/Near‐Infrared Integral Field Spectrograph laser‐guide star adaptive‐optics assisted K‐band integral‐field spectroscopy of W33A and its inner reflection nebula. In our data, we make the first detections of a rotationally flattened outer envelope and fast bipolar jet of a massive YSO at near‐infrared wavelengths. The predominant spectral features observed are Br γ, H2 and a combination of emission and absorption from CO gas. We perform a 3D spectro‐astrometric analysis of the line emission, the first study of its kind. We find that the object's Br γ emission reveals evidence for a fast bipolar jet on sub‐milliarcsecond scales, which is aligned with the larger scale outflow. The hybrid CO features can be explained as a combination of hot CO emission arising in a disc close to the central star, while cold CO absorption originates in the cooler outer envelope. Kinematic analysis of these features reveals that both structures are rotating and consistent with being aligned perpendicular to both the ionized jet and the large‐scale outflow. Assuming Keplerian rotation, we find that the circumstellar disc orbits a central mass of ≳10 M⊙, while the outer envelope encloses a mass of ∼15 M⊙. Our results suggest a scenario of a central star accreting material from a circumstellar disc at the centre of a cool extended rotating torus, while driving a fast bipolar wind. These results therefore provide strong supporting evidence for the hypothesis that the formation mechanism for high‐mass stars is qualitatively similar to that of low‐mass stars.

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The interactions of winds from massive young stellar objects: X-ray emission, dynamics and cavity evolution

Cited by 26 publications

References 81 publications

HerschelPACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050

HerschelPACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050

Turbulent entrainment origin of protostellar outflows

The circumstellar disc, envelope and bipolar outflow of the massive young stellar object W33A

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