A resolved, au-scale gas disk around the B[e] star HD 50138

Ellerbroek, L. E.; Benisty, M.; Kraus, Stefan; Perraut, K.; Kluska, J.; Bouquin, J.-B. Le; Fernandes, M. Borges; Souza, A. Domiciano de; Maaskant, K. M.; Kaper, L.; Tramper, F.; Mourard, D.; Tallon–Bosc, I.; Brummelaar, T. ten; Sitko, M. L.; Lynch, D. K.; Russell, R. W.

doi:10.1051/0004-6361/201424143

Cited by 25 publications

(53 citation statements)

References 84 publications

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“…It was included in the sample as a possible protoplanetary disk and is often treated as such in the literature, but see e.g. Ellerbroek et al (2015) for a discussion of its unclear nature. Its CO 6−5 upper limit falls between our R c = 10 and 50 au models, while the [C ] detection is an order of magnitude brighter than any of our Herbig Ae/Be disk models.…”

Section: Herbig Ae/be Systems (Spectral Types B a F)mentioning

confidence: 99%

Observations and modelling of CO and [C i] in protoplanetary disks

Kama

Bruderer

Carney

et al. 2016

A&A

111

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Context. The gas-solid budget of carbon in protoplanetary disks is related to the composition of the cores and atmospheres of the planets forming in them. The principal gas-phase carbon carriers CO, C 0 , and C + can now be observed regularly in disks. Aims. The gas-phase carbon abundance in disks has thus far not been well characterized observationally. We obtain new constraints on the [C]/[H] ratio in a large sample of disks, and compile an overview of the strength of [C ] and warm CO emission. Methods. We carried out a survey of the CO 6-5 line and the [C ] 1-0 and 2-1 lines towards 37 disks with the APEX telescope, and supplemented it with [C ] data from the literature. The data are interpreted using a grid of models produced with the DALI disk code.We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties.

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Section: Herbig Ae/be Systems (Spectral Types B a F)mentioning

confidence: 99%

Observations and modelling of CO and [C i] in protoplanetary disks

Kama

Bruderer

Carney

et al. 2016

A&A

111

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“…The star has a measured rotational speed 90 km s −1 , and is inferred to have a disk inclined at 56 Borges Fernandes et al 2011. Using the spectrointerferometric technique, Ellerbroek et al (2015) resolved its au-scale disk with a measured photocenter offset, possibly caused by an asymmetric structure of the disk or a binary companion. These authors favored a post-main sequence status for HD 50138, because of the presence of high transition lines, such as Paschen, Bracket and Pfund series less commonly observed in PMS stars, and because the star is apparently not associated with an SFR, supported by our assessment.…”

Section: Census Of Neighboring Regionsmentioning

confidence: 99%

“…4 we present an elaborative census of each target in order to rule out the possibility of stellar youth for eight B[e] stars, adding support to their evolved status. Cidale et al (2001); (c) Sheikina et al (2000); (d) Voroshilov et al (1985); (e) Friedemann (1992); ( f ) Ellerbroek et al (2015); (g) Miroshnichenko et al (2003); (h) Miroshnichenko et al (2001); (i) Caratti o Garatti et al (2015); ( j) Malfait et al (1998); (k) Malkov et al (2006); (l) Dyck & Milkey (1972); (m) Zickgraf (2001). Zhang et al (2005), and that of Herbig stars is from de Winter et al (2001).…”

Section: Introductionmentioning

confidence: 98%

Evolutionary status of isolated B[e] stars

Lee

Chen

Liu

2016

A&A

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Aims. We study a sample of eight B[e] stars with uncertain evolutionary status to shed light on the origin of their circumstellar dust. Methods. We performed a diagnostic analysis on the spectral energy distribution beyond infrared wavelengths, and conducted a census of neighboring region of each target to ascertain its evolutionary status. Results. In comparison to pre-main sequence Herbig stars, these B[e] stars show equally substantial excess emission in the nearinfrared, indicative of existence of warm dust, but much reduced excess at longer wavelengths, so the dusty envelopes should be compact in size. Isolation from star-forming regions excludes the possibility of their pre-main sequence status. Six of our targets, including HD 50138, HD 45677, CD−24 5721, CD−49 3441, MWC 623, and HD 85567, have been previously considered as FS CMa stars, whereas HD 181615/6 and HD 98922 are added to the sample by this work. We argue that the circumstellar grains of these isolated B[e] stars, already evolved beyond the pre-main sequence phase, should be formed in situ. This is in contrast to Herbig stars, which inherit large grains from parental molecular clouds. It has been thought that HD 98922, in particular, is a Herbig star because of its large infrared excess, but we propose it being in a more evolved stage. Because dust condenses out of stellar mass loss in an inside-out manner, the dusty envelope is spatially confined, and anisotropic mass flows, or anomalous optical properties of tiny grains, lead to the generally low line-of-sight extinction toward these stars.

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“…Visual-wavelength interferometry, for instance with the CHARA/VEGA instrument, can provide now fundamentally new constraints to distinguish between these models. So far, Hα spectrointerferometry have been reported for only two HAeBe stars, namely AB Aurigae (Rousselet-Perraut et al 2010) and MWC158 (Ellerbroek et al 2014). In both cases, the measurements indicate that the line-emitting region is more extended than what would be expected from a magnetosphere accretion scenario and the measurements appear more consistent with an X-wind or disk-wind geometry, although it should be noted that the measurement uncertainties are still very large in the current data sets.…”

Section: Gas Kinematics Constraintsmentioning

confidence: 65%

“…Such gas kinematics studies can be conducted using AMBER's unique high spectral dispersion mode of R = λ/∆λ = 12 000. For the Herbig B[e] stars V921 Scorpii (Kraus et al 2012a) and MWC158 (Ellerbroek et al 2014), it was found that the Brγ-emitting gas is in Keplerian rotation in the inner disk. Observations on MWC297, on the other hand, had to invoked a more complex disk wind model (Weigelt et al 2011).…”

Section: Gas Kinematics Constraintsmentioning

confidence: 99%

The interferometric view of Herbig Ae/Be stars

Kraus

2015

Astrophys Space Sci

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In this contribution I review how optical interferometry has contributed to shaping our understanding of the class of Herbig Ae/Be stars and of their associated circumstellar disks. I discuss the evidence for an optically-thin cavity in the inner few astronomical units (au) and a "puffed-up rim" near the dust sublimation radius and how these observations helped to establish the current generation of irradiated disk models. Multi-wavelength interferometric observations also revealed systems with clear signatures of grain growth and dynamically-cleared disk gaps, tracing important stages of disk evolution and of ongoing planet formation. I discuss the new opportunities provided by spectro-interferometry, which enables detailed studies on the gas distribution and velocity field on sub-au scales, resulting in constrains on the accretion properties of the system and the disk excitation structure. Finally, I outline some of the open questions and loose ends in current interferometric studies, and how these might point towards new disk physics.

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A resolved, au-scale gas disk around the B[e] star HD 50138

Cited by 25 publications

References 84 publications

Observations and modelling of CO and [C i] in protoplanetary disks

Observations and modelling of CO and [C i] in protoplanetary disks

Evolutionary status of isolated B[e] stars

The interferometric view of Herbig Ae/Be stars

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