Relation between the Luminosity of Young Stellar Objects and Their Circumstellar Environment

Vinković, Dejan; Jurkić, Tomislav

doi:10.1086/511327

Cited by 56 publications

(68 citation statements)

References 108 publications

(197 reference statements)

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“…However, the angular size of a centrally heated source of flux is dependent upon both the luminosity of central object and the distance to it (angular size ∝ √ L d , see e.g. Vinković & Jurkić 2007). We find that the resolved objects generally have a higher value of √ L d than the unresolved objects.…”

Section: Observational Resultsmentioning

confidence: 63%

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

Wheelwright

Wit

Oudmaijer

et al. 2012

A&A

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Context. Massive stars form whilst they are still embedded in dense envelopes. As a result, the roles of rotation, mass loss and accretion in massive star formation are not well understood. Aims. This study evaluates the source of the Q-band, λ c = 19.5 μm, emission of massive young stellar objects (MYSOs). This allows us to determine the relative importance of rotation and outflow activity in shaping the circumstellar environments of MYSOs on 1000 AU scales. Methods. We obtained diffraction limited mid-infrared images of a sample of 20 MYSOs using the VLT/VISIR and Subaru/COMICS instruments. For these 8 m class telescopes and the sample selected, the diffraction limit, ∼0.6 , corresponds to approximately 1000 AU. We compare the images and the spectral energy distributions (SEDs) observed to a 2D, axis-symmetric dust radiative transfer model that reproduces VLTI/MIDI observations of the MYSO W33A. We vary the inclination, mass infall rate, and outflow opening angle to simultaneously recreate the behaviour of the sample of MYSOs in the spatial and spectral domains. Results. The mid-IR emission of 70 percent of the MYSOs is spatially resolved. In the majority of cases, the spatial extent of their emission and their SEDs can be reproduced by the W33A model featuring an in-falling, rotating dusty envelope with outflow cavities. There is independent evidence that most of the sources which are not fit by the model are associated with ultracompact H ii regions and are thus more evolved. Conclusions. We find that, in general, the diverse ∼20 μm morphology of MYSOs can be attributed to warm dust in the walls of outflow cavities seen at different inclinations. This implies that the warm dust in the outflow cavity walls dominates the Q-band emission of MYSOs. In turn, this emphasises that outflows are an ubiquitous feature of massive star formation.

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Section: Observational Resultsmentioning

confidence: 63%

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

Wheelwright

Wit

Oudmaijer

et al. 2012

A&A

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“…For this case, the derived inclination of V1026 Sco is still within the range predicted for UXOrs (45 • -68 • ) by Natta & Whitney (2000). Dust clouds in centrifugally-driven disk winds (Vinković & Jurkić 2007;Bans & Königl 2012) can also explain the UX Ori type variability of V1026 Sco, as they also are consistent with intermediate to high disk inclinations.…”

Section: Figmentioning

confidence: 77%

The inner circumstellar disk of the UX Orionis star V1026 Scorpii

Vural

Kreplin

Kishimoto

et al. 2014

A&A

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Context. The UX Ori type variables (named after the prototype of their class) are intermediate-mass pre-main sequence objects. One of the most likely causes of their variability is the obscuration of the central star by orbiting dust clouds. Aims. We investigate the structure of the circumstellar environment of the UX Ori star V1026 Sco (HD 142666) and test whether the disk inclination is large enough to explain the UX Ori variability. Methods. We observed the object in the low-resolution mode of the near-infrared interferometric VLTI/AMBER instrument and derived H-and K-band visibilities and closure phases. We modeled our AMBER observations, published Keck Interferometer observations, archival MIDI/VLTI visibilities, and the spectral energy distribution using geometric and temperature-gradient models. • approximately agrees with the inclination derived with the geometric model (49 ± 5 • in the K band and 50 ± 11 • in the H band). The position angle of the fitted geometric and temperaturegradient models are 163 ± 9 • (K band; 179 ± 17 • in the H band) and 169.3 +4.2 −6.7• , respectively. Conclusions. The narrow width of the inner ring-shaped model disk and the disk gap might be an indication for a puffed-up inner rim shadowing outer parts of the disk. The intermediate inclination of ∼50 • is consistent with models of UX Ori objects where dust clouds in the inclined disk obscure the central star.

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“…Vinković & Jurkić (2007) propose that this phenomenon may contribute to the infrared variability of young stellar objects. Bans & Königl (2012) adapt it to explain the NIR brightening of HD 163296.…”

Section: Optical Fading Nir Brightening: Dust In the Wind?mentioning

confidence: 94%

Relating jet structure to photometric variability: the Herbig Ae star HD 163296

Ellerbroek

Podio

Dougados

et al. 2014

A&A

131

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Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded by circumstellar dust disks. Some are observed to produce jets, whose appearance as a sequence of shock fronts (knots) suggests a past episodic outflow variability. This "jet fossil record" can be used to reconstruct the outflow history. We present the first optical to near-infrared (NIR) spectra of the jet from the Herbig Ae star HD 163296, obtained with VLT/X-shooter. We determine the physical conditions in the knots and also their kinematic "launch epochs". Knots are formed simultaneously on either side of the disk, with a regular interval of ∼16 yr. The velocity dispersion versus jet velocity and the energy input are comparable between both lobes. However, the mass-loss rate, velocity, and shock conditions are asymmetric. We findṀ jet /Ṁ acc ∼ 0.01−0.1, which is consistent with magneto-centrifugal jet launching models. No evidence of any dust is found in the high-velocity jet, suggesting a launch region within the sublimation radius (<0.5 au). The jet inclination measured from proper motions and radial velocities confirms that it is perpendicular to the disk. A tentative relation is found between the structure of the jet and the photometric variability of the central source. Episodes of NIR brightening were previously detected and attributed to a dusty disk wind. We report for the first time significant optical fadings lasting from a few days up to a year, coinciding with the NIR brightenings. These are very likely caused by dust lifted high above the disk plane, and this supports the disk wind scenario. The disk wind is launched at a larger radius than the high-velocity atomic jet, although their outflow variability may have a common origin. No significant relation between outflow and accretion variability could be established. Our findings confirm that this source undergoes periodic ejection events, which may be coupled with dust ejections above the disk plane.

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Relation between the Luminosity of Young Stellar Objects and Their Circumstellar Environment

Cited by 56 publications

References 108 publications

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

The inner circumstellar disk of the UX Orionis star V1026 Scorpii

Relating jet structure to photometric variability: the Herbig Ae star HD 163296

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