First NIR interferometrically resolved high-order Brackett and forbidden Fe lines of a B[e] star: V921 Sco

Kreplin, Alexander; Kraus, Stefan; Тамбовцева, Л. В.; Гринин, В. П.; Hone, Edward

doi:10.1093/mnras/stz3346

Cited by 6 publications

(4 citation statements)

References 24 publications

(33 reference statements)

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“…Such a model allows us to not only to build up a picture of the temperature profile, but also approximate the position of the inner radius. The TGM is based upon T R = T 0 (R/R 0 ) −Q where T 0 is the temperature at the inner radius of the disk R 0 , and Q is the exponent of the temperature gradient (Kreplin et al 2020;Eisner & Hillenbrand 2011). A TGM represents an intrinsically geometrically thin disk.…”

Section: Disk Temperature Structure and Geometrymentioning

confidence: 99%

Viscous heating in the disk of the outbursting star FU Orionis

Labdon

Kraus

Davies

et al. 2021

A&A

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Context. FU Orionis is the archetypal FUor star, a subclass of young stellar object (YSO) that undergo rapid brightening events, often gaining 4-6 magnitudes on timescales of days. This brightening is often associated with a massive increase in accretion; one of the most ubiquitous processes in astrophysics from planets and stars to super-massive black holes. We present multi-band interferometric observations of the FU Ori circumstellar environment, including the first J-band interferometric observations of a Y SO. Aims. We investigate the morphology and temperature gradient of the innermost regions of the accretion disk around FU Orionis. We aim to characterise the heating mechanisms of the disk and comment on potential outburst triggering processes. Methods. Recent upgrades to the MIRC-X instrument at the CHARA array allowed the first dual-band J and H observations of YSOs. Using baselines up to 331 m, we present high angular resolution data of a YSO covering the near-infrared bands J, H, and K. The unprecedented spectral range of the data allows us to apply temperature gradient models to the innermost regions of FU Ori. Results. We spatially resolve the innermost astronomical unit of the disk and determine the exponent of the temperature gradient of the inner disk to T ∝ r −0.74±0.02. This agrees with theoretical work that predicts T ∝ r −0.75 for actively accreting, steady state disks, a value only obtainable through viscous heating within the disk. We find a disk which extends down to the stellar surface at 0.015 ± 0.007 au where the temperature is found to be 5800 ± 700 K indicating boundary layer accretion. We find a disk inclined at 32 ± 4 • with a minor-axis position angle of 34 ± 11 •. Conclusions. We demonstrate that J-band interferometric observations of YSOs are feasible with the MIRC-X instrument at CHARA. The temperature gradient power-law derived for the inner disk is consistent with theoretical predictions for steady-state, optically thick, viciously heated accretion disks.

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Section: Disk Temperature Structure and Geometrymentioning

confidence: 99%

Viscous heating in the disk of the outbursting star FU Orionis

Labdon

Kraus

Davies

et al. 2021

A&A

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“…Hen 3-1330 has previously been classified as a WR+O binary system (Richardson et al 2011). V921 Sco has been classified as both a supergiant and as a Herbig Be star (Kreplin et al 2020). WRAY 15-535 has been classified as a supergiant B[e] star (Domiciano de Souza et al 2007).…”

Section: Systems With Stellar Masses >8 M Ementioning

confidence: 99%

Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager

Rich¹,

Monnier²,

Aarnio³

et al. 2022

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We present the complete sample of protoplanetary disks from the Gemini- Large Imaging with the Gemini Planet Imager Herbig/T Tauri Survey, which observed bright Herbig Ae/Be stars and T Tauri stars in near-infrared polarized light to search for signatures of disk evolution and ongoing planet formation. The 44 targets were chosen based on their near- and mid-infrared colors, with roughly equal numbers of transitional, pre-transitional, and full disks. Our approach explicitly did not favor well-known, “famous” disks or those observed by the Atacama Large Millimeter/submillimeter Array, resulting in a less-biased sample suitable to probe the major stages of disk evolution during planet formation. Our optimized data reduction allowed polarized flux as low as 0.002% of the stellar light to be detected, and we report polarized scattered light around 80% of our targets. We detected point-like companions for 47% of the targets, including three brown dwarfs (two confirmed, one new), and a new super-Jupiter-mass candidate around V1295 Aql. We searched for correlations between the polarized flux and system parameters, finding a few clear trends: the presence of a companion drastically reduces the polarized flux levels, far-IR excess correlates with polarized flux for nonbinary systems, and systems hosting disks with ring structures have stellar masses <3 M⊙. Our sample also included four hot, dusty “FS CMa” systems, and we detected large-scale ( >100 au) scattered light around each, signs of extreme youth for these enigmatic systems. Science-ready images are publicly available through multiple distribution channels using a new FITS file standard that has been jointly developed with members of the Very Large Telescope Spectro-polarimetric High-contrast Exoplanet Research team.

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“…. GEOMETRIC MODELLING inner radius of the disk 0 , and is the exponent of the temperature gradient (Kreplin et al 2020;Eisner and Hillenbrand 2011). A TGM represents an intrinsically geometrically thin disk.…”

Section: Temperature Gradient Modelsmentioning

confidence: 99%

“…Such a model allows us to not only to build up a picture of the temperature profile, but also approximate the position of the inner radius. The TGM is based upon = 0 ( / 0 ) − where 0 is the temperature at the inner radius of the disk 0 , and is the exponent of the temperature gradient (Kreplin et al 2020;Eisner and Hillenbrand 2011). While a model lacks any flaring, in this case it traces the surface layers of the disk as observed in the infrared.…”

Section: Disk Temperature Structure and Geometrymentioning

confidence: 99%