Revealing the inner circumstellar disk of the T Tauri star S Coronae Australis N using the VLTI

Vural, Jasmin; Kreplin, Alexander; Kraus, Stefan; Weigelt, G.; Driebe, T.; Benisty, M.; Dugué, M.; Massi, F.; Monin, Jean‐Louis; Vannier, M.

doi:10.1051/0004-6361/201218892

Cited by 17 publications

(21 citation statements)

References 33 publications

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“…The extended halo component contributes with 13 ± 2% (DDN model)/16 ± 4% (geometric model) to the total flux, similar as found in other young stellar objects with extended halo emission (∼9-16%, e.g. Monnier et al 2006;Chen et al 2012;Vural et al 2012Vural et al , 2014a that is interpreted as scattered emission from the outer disk surface or material outside the disk plane, for example, a dusty disk wind (e.g., Bans & Königl 2012).…”

Section: Discussionsupporting

confidence: 80%

Resolving the inner disk of UX Orionis

Kreplin

Madlener

Chen

et al. 2016

A&A

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Aims. The cause of the UX Ori variability in some Herbig Ae/Be stars is still a matter of debate. Detailed studies of the circumstellar environment of UX Ori objects (UXORs) are required to test the hypothesis that the observed drop in photometry might be related to obscuration events. Methods. Using near-and mid-infrared interferometric AMBER and MIDI observations, we resolved the inner circumstellar disk region around UX Ori. Results. We fitted the K-, H-, and N-band visibilities and the spectral energy distribution (SED) of UX Ori with geometric and parametric disk models. The best-fit K-band geometric model consists of an inclined ring and a halo component. We obtained a ring-fit radius of 0.45 ± 0.07 AU (at a distance of 460 pc), an inclination of 55.6 ± 2.4 • , a position angle of the system axis of 127.5 ± 24.5 • , and a flux contribution of the over-resolved halo component to the total near-infrared excess of 16.8 ± 4.1%. The best-fit N-band model consists of an elongated Gaussian with a HWHM ∼ 5 AU of the semi-major axis and an axis ration of a/b ∼ 3.4 (corresponding to an inclination of ∼72 • ). With a parametric disk model, we fitted all near-and mid-infrared visibilities and the SED simultaneously. The model disk starts at an inner radius of 0.46 ± 0.06 AU with an inner rim temperature of 1498 ± 70 K. The disk is seen under an nearly edge-on inclination of 70 ± 5 • . This supports any theories that require high-inclination angles to explain obscuration events in the line of sight to the observer, for example, in UX Ori objects where orbiting dust clouds in the disk or disk atmosphere can obscure the central star.

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Section: Discussionsupporting

confidence: 80%

Resolving the inner disk of UX Orionis

Kreplin

Madlener

Chen

et al. 2016

A&A

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“…The size derived for the continuum (r = 0.108 au) of S CrA N, is in excellent agreement with the values found by Vural et al (2012) (r∼0.11 au) and Anthonioz et al (2015) (r∼0.108 au). Moreover our estimates of the disk orientation and inclination (PA =0…”

Section: Continuum Emissionsupporting

confidence: 87%

The wind and the magnetospheric accretion onto the T Tauri star S Coronae Australis at sub-au resolution

Lopez¹,

Perraut²,

Garatti³

et al. 2017

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Aims. To investigate the inner regions of protoplanetary disks, we performed near-infrared interferometric observations of the classical T Tauri binary system S CrA. Methods. We present the first VLTI-GRAVITY high spectral resolution (R ∼ 4000) observations of a classical T Tauri binary, S CrA (composed of S CrA N and S CrA S and separated by ∼1 . 4), combining the four 8-m telescopes in dual-field mode. Results. Our observations in the near-infrared K-band continuum reveal a disk around each binary component, with similar half-flux radii of about 0.1 au at d∼130 pc, inclinations (i =28±3• and i =22±6 • ), and position angles (PA=0 • ±6• and PA=-2 • ±12• ), suggesting that they formed from the fragmentation of a common disk. The S CrA N spectrum shows bright He i and Brγ line emission exhibiting inverse P-Cygni profiles, typically associated with infalling gas. The continuum-compensated Brγ line visibilities of S CrA N show the presence of a compact Brγ emitting region the radius of which is about ∼0.06 au, which is twice as big as the truncation radius. This component is mostly tracing a wind. Moreover, a slight radius change between the blue-and red-shifted Brγ line components is marginally detected. Conclusions. The presence of an inverse P-Cygni profile in the He i and Brγ lines, along with the tentative detection of a slightly larger size of the blue-shifted Brγ line component, hint at the simultaneous presence of a wind and magnetospheric accretion in S CrA N.

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“…Malbet et al 2005;Eisner et al 2007;Ragland et al 2012;Vural et al 2012;Wang et al 2012). However, this technique is not directly applicable to deeplyembedded objects, as the SED is dominated by the circumstellar envelope (rather than the central star and disk) at all wavelengths.…”

Section: Model Fits To the Visibilities And Correlated Fluxesmentioning

confidence: 99%

A multi-wavelength interferometric study of the massive young stellar object IRAS 13481-6124

Boley

Kraus

Wit

et al. 2016

A&A

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We present new mid-infrared interferometric observations of the massive young stellar object IRAS 13481-6124, using VLTI/MIDI for spectrally-resolved, long-baseline measurements (projected baselines up to ∼120 m) and GSO/T-ReCS for aperture-masking interferometry in five narrow-band filters (projected baselines of ∼1.8−6.4 m) in the wavelength range of 7.5−13 μm. We combine these measurements with previously-published interferometric observations in the K and N bands in order to assemble the largest collection of infrared interferometric observations for a massive YSO to date. Using a combination of geometric and radiativetransfer models, we confirm the detection at mid-infrared wavelengths of the disk previously inferred from near-infrared observations. We show that the outflow cavity is also detected at both near-and mid-infrared wavelengths, and in fact dominates the mid-infrared emission in terms of total flux. For the disk, we derive the inner radius (∼1.8 mas or ∼6.5 AU at 3.6 kpc), temperature at the inner rim (∼1760 K), inclination (∼48• ) and position angle (∼107 • ). We determine that the mass of the disk cannot be constrained without high-resolution observations in the (sub-)millimeter regime or observations of the disk kinematics, and could be anywhere from ∼10 −3 to 20 M . Finally, we discuss the prospects of interpreting the spectral energy distributions of deeply-embedded massive YSOs, and warn against attempting to infer disk properties from the spectral energy distribution.

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Revealing the inner circumstellar disk of the T Tauri star S Coronae Australis N using the VLTI

Cited by 17 publications

References 33 publications

Resolving the inner disk of UX Orionis

Resolving the inner disk of UX Orionis

The wind and the magnetospheric accretion onto the T Tauri star S Coronae Australis at sub-au resolution

A multi-wavelength interferometric study of the massive young stellar object IRAS 13481-6124

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