Cloudlet capture by transitional disk and FU Orionis stars

Dullemond, C. P.; Küffmeier, M.; Goicovic, F. G.; Fukagawa, Misato; Oehl, Veronika; Krämer, Manuel

doi:10.1051/0004-6361/201832632

Cited by 67 publications

(94 citation statements)

References 90 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Bate et al (2010) note that the inner disk could be misaligned with respect to the stellar rotation axis, due to the chaotic nature of star and disk formation. It was recently proposed that the outer disk could be misaligned as a result of late accretion events from material accreted with a misaligned angular momentum (Dullemond et al 2019;Kuffmeier et al 2021), a scenario possibly at play in SU Aur where both a large scale arm (Akiyama et al 2019) and a misaligned inner disk are observed (Ginski et al 2021). In the sample of transition disks that we studied in this paper, two targets within the "ambiguous" subset, HD 100546 and UX Tau A, show extended features in scattered light (Ardila et al 2007;Ménard et al 2020) but in the case of UX Tau A they seem well accounted for by a flyby.…”

Section: Discussionmentioning

confidence: 99%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

View full text Add to dashboard Cite

Context. Transition disks are protoplanetary disks with dust-depleted cavities, possibly indicating substantial clearing of their dust content by a massive companion. For several known transition disks, dark regions interpreted as shadows have been observed in scattered light imaging and are hypothesized to originate from misalignments between distinct regions of the disk. Aims. We aim to investigate the presence of misalignments in transition disks. We study the inner disk (<1 au) geometries of a sample of 20 well-known transition disks with Very Large Telescope Interferometer (VLTI) GRAVITY observations and use complementary 12CO and 13CO molecular line archival data from the Atacama Large Millimeter/submillimeter Array (ALMA) to derive the orientation of the outer disk regions (>10 au). Methods. We fit simple parametric models to the visibilities and closure phases of the GRAVITY data to derive the inclination and position angle of the inner disks. The outer disk geometries were derived from Keplerian fits to the ALMA velocity maps and compared to the inner disk constraints. We also predicted the locations of expected shadows for significantly misaligned systems. Results. Our analysis reveals six disks to exhibit significant misalignments between their inner and outer disk structures. The predicted shadow positions agree well with the scattered light images of HD 100453 and HD 142527, and we find supporting evidence for a shadow in the south of the disk around CQ Tau. In the other three targets for which we infer significantly misaligned disks, V1247 Ori, V1366 Ori, and RY Lup, we do not see any evident sign of shadows in the scattered light images. The scattered light shadows observed in DoAr 44, HD 135344 B, and HD 139614 are consistent with our observations, yet the underlying morphology is likely too complex to be described properly by our models and the accuracy achieved by our observations. Conclusions. The combination of near infrared and submillimeter interferometric observations allows us to assess the geometries of the innermost disk regions and those of the outer disk. Whereas we can derive precise constraints on the potential shadow positions for well-resolved inner disks around Herbig Ae/Be stars, the large statistical uncertainties for the marginally resolved inner disks around the T Tauri stars of our sample make it difficult to extract conclusive constraints for the presence of shadows in these systems.

show abstract

Section: Discussionmentioning

confidence: 99%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…Indeed, close fly-bys of companion, cloudlets, or intruder stars are known to produce tidal tails and mass accretion bursts (e.g. Bonnell & Bastien 1992;Thies et al 2010;Forgan & Rice 2011;Dai et al 2015;Vorobyov et al 2017;Dullemond et al 2019). The ALMA observations by Rodriguez et al (2018) further elaborated the encounter scenario for the formation of tail-like structure by suggesting multiple fly-bys in the RW Aurigae system.…”

Section: Introductionmentioning

confidence: 99%

The origin of tail-like structures around protoplanetary disks

Vorobyov

Skliarevskii

Elbakyan

et al. 2020

A&A

View full text Add to dashboard Cite

Aims. We study the origin of tail-like structures recently detected around the disk of SU Aurigae and several FU Orionis type stars. Methods. Dynamic protostellar disks featuring ejections of gaseous clumps and quiescent protoplanetary disks experiencing a close encounter with an intruder star were modelled using the numerical hydrodynamics code FEOSAD. Both the gas and dust dynamics were taken into account, including dust growth and mutual friction between the gas and dust components. Only plane-of-the-disk encounters were considered. Results. Ejected clumps produce a unique type of tails that are characterized by a bow-shock shape. These tails owe its origin to the supersonic motion of the ejected clumps through the dense envelope, which often surrounds young gravitationally unstable protostellar disks. The ejected clumps either sit at the head of the tail-like structure or disperse if their mass is insufficient to withstand the head wind of the envelope. On the other hand, close encounters with quiescent protoplanetary disks produce three types of the tail-like structures, which we defined as pre-collisional, post-collisional, and spiral tails. These tails can in principle be distinguished by peculiar features of the gas and dust flow in and around them. We found that the brown-dwarf-mass intruders do not capture circumintruder disks during the encounter, while the sub-solar-mass intruders can acquire appreciable circumintruder disks with elevated dust-to-gas ratios, which can ease their observational detection. However, this is true only for prograde collisions; the retrograde intruders fail to collect an appreciable gas and dust from the disk of the target. The masses of gas in the tails vary in the 0.85-11.8 M Jup limits, while the total mass of dust lies in the 1.75-30.1 M ⊕ range, with the spiral tails featuring the highest masses. The predicted mass of dust in the model tail-like structures is therefore higher than what was inferred for similar structures in SU Aur, FU Ori, and Z CMa, making their observational detection feasible. Conclusions. Tail-like structures around protostellar and protoplanetary disks can act as a smoking gun to infer interesting phenomena, such as clump ejection or close encounters. particular, the bow-shock morphology of the tails could point to clump ejections as a possible formation mechanism. Further numerical and observational studies are needed to better understand the detectability and properties of the tails.

show abstract

“…A lateenvelope infall was proposed to account for the similar spiral pattern observed in the disk of AB Aur (Fukagawa et al 2004;Tang et al 2012Tang et al , 2017. Large-scale images of the environment of AB Aur show the presence of a large surrounding cloudlet, which led Dullemond et al (2019) to propose that transitional disks such as AB Aur could all be the result of cloudlet capture. In that case, the spirals might be seen in a different plane than that of the inner rim of the outer disk, i.e., the outer disk would be warped, likeHD100546 for example (e.g., Quillen 2006).…”

Section: Infallmentioning

confidence: 94%

“…An alternative possibility for the origin of the flocculent spiral pattern is infall from a late envelope or a captured cloudlet (e.g., Tang et al 2012;Dullemond et al 2019). A lateenvelope infall was proposed to account for the similar spiral pattern observed in the disk of AB Aur (Fukagawa et al 2004;Tang et al 2012Tang et al , 2017.…”

Section: Infallmentioning

confidence: 99%

SCExAO/CHARIS High-contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk

Uyama

Currie

Christiaens

et al. 2020

ApJ

View full text Add to dashboard Cite

We present Subaru/SCExAO+Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) broadband (JHK-band) integral field spectroscopy of HD 34700 A. CHARIS data recover HD 34700 A's disk ring and confirm multiple spirals discovered by Monnier et al. We set limits on substellar companions of ∼12 M Jup at 0 3 (in the ring gap) and ∼5 M Jup at 0 75 (outside the ring). The data reveal darkening effects on the ring and spiral, although we do not identify the origin of each feature such as shadows or physical features related to the outer spirals. Geometric albedos converted from the surface brightness suggest a greater scale height and/or prominently abundant submicron dust at position angles between ∼45°and 90°. Spiral fitting resulted in very large pitch angles (∼30°-50°); a stellar flyby of HD 34700 B or infall from a possible envelope is perhaps a reasonable scenario to explain the large pitch angles.

show abstract

Cloudlet capture by transitional disk and FU Orionis stars

Cited by 67 publications

References 90 publications

Probing inner and outer disk misalignments in transition disks

Probing inner and outer disk misalignments in transition disks

The origin of tail-like structures around protoplanetary disks

SCExAO/CHARIS High-contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk

Contact Info

Product

Resources

About