Multiple Stellar Flybys Sculpting the Circumstellar Architecture in RW Aurigae

Rodriguez, Joseph E.; Loomis, Ryan A.; Cabrit, S.; Haworth, Thomas J.; Facchini, Stefano; Dougados, C.; Booth, Richard A; Jensen, Eric L. N.; Clarke, C. J.; Stassun, Keivan G.; Dent, W. R. F.; Pety, J.

doi:10.3847/1538-4357/aac08f

Cited by 81 publications

(105 citation statements)

References 59 publications

(127 reference statements)

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“…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. Recently, de Leon et al (2015) and Akiyama et al (2019) presented the Subaru-HiCIAO and ALMA observations of SU Auriage showing that this system also has a tail-like structure extending from its disk for a thousand au.…”

Section: Introductionmentioning

confidence: 84%

The origin of tail-like structures around protoplanetary disks

Vorobyov

Skliarevskii

Elbakyan

et al. 2020

A&A

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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.

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Section: Introductionmentioning

confidence: 84%

The origin of tail-like structures around protoplanetary disks

Vorobyov

Skliarevskii

Elbakyan

et al. 2020

A&A

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“…Rodriguez et al 2013Rodriguez et al , 2016Dai et al 2015). Support for this theory is given by hydrodynamical simulations, and by the ingress and egress time of the dimming events (see summary in Rodriguez et al 2018): assuming a Keplerian velocity for the occulting body, ingress and egress times correspond to a distance of ∼ 180 au.…”

Section: Origin Of the Dimming Eventsmentioning

confidence: 94%

“…where we have taken R out = 58 au (as measured from the ALMA observations by Rodriguez et al 2018). The agreement of the two relevant timescales (periastron passage and sound-crossing time) is suggestive, but not conclusive.…”

Section: Origin Of the Dimming Eventsmentioning

confidence: 96%

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Exploring the dimming event of RW Aurigae A through multi-epoch VLT/X-shooter spectroscopy

Koutoulaki

Facchini

Manara

et al. 2019

A&A

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Context. RW Aur A is a classical T Tauri star that has suddenly undergone three major dimming events since 2010. The reason for these dimming events is still not clear. Aims. We aim to understand the dimming properties, examine accretion variability, and derive the physical properties of the inner disc traced by the CO ro-vibrational emission at near-infrared wavelengths (2.3 µm). Methods. We compared two epochs of X-Shooter observations, during and after the dimming. We modelled the rarely detected CO bandhead emission in both epochs to examine whether the inner disc properties had changed. The spectral energy distribution was used to derive the extinction properties of the dimmed spectrum and compare the infrared excess between the two epochs. Lines tracing accretion were used to derive the mass accretion rate in both states. Results. The CO originates from a region with physical properties of T=3000 K, N CO =1×10 21 cm −2 and v k sin i=113 km/s. The extinction properties of the dimming layer were derived with the effective optical depth ranging from τ e f f ∼2.5-1.5 from the UV to the near-IR. The inferred mass accretion rateṀ acc is ∼ 1.5 × 10 −8 M /yr and ∼ 2 × 10 −8 M /yr after and during the dimming respectively. By fitting the spectral energy distribution, additional emission is observed in the infrared during the dimming event from dust grains with temperatures of 500-700 K. Conclusions. The physical conditions traced by the CO are similar for both epochs, indicating that the inner gaseous disc properties do not change during the dimming events. The extinction curve is flatter than that of the interstellar medium, and large grains of a few hundred microns are thus required. When we correct for the observed extinction, the mass accretion rate is constant in the two epochs, suggesting that the accretion is stable and therefore does not cause the dimming. The additional hot emission in the near-IR is located at about 0.5 au from the star and is not consistent with an occulting body located in the outer regions of the disc. The dimming events could be due to a dust-laden wind, a severe puffing up of the inner rim, or a perturbation caused by the recent star-disc encounter.

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“…Observational evidence of the imprints of dynamical truncations has been reported in several nearby stellar clusters (Olczak et al 2008;Reche et al 2009;de Juan Ovelar et al 2012). Tidal stripping that can be explained by disk-star interactions has been observed in the RW Aurigae system (Cabrit et al 2006;Rodriguez et al 2018;Dai et al 2015) and in the T Tauri binary system AS 205 (Salyk et al 2014). There is also evidence that the Solar System might have been affected by a close encounter with another star during its early stages (Jílková et al 2015;Pfalzner et al 2018).…”

Section: Introductionmentioning

confidence: 94%

External photoevaporation of circumstellar discs constrains the time-scale for planet formation

Concha-Ramírez

Wilhelm

Zwart

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Planet-forming circumstellar disks are a fundamental part of the star formation process. Since stars form in a hierarchical fashion in groups of up to hundreds or thousands, the UV radiation environment that these disks are exposed to can vary in strength by at least six orders of magnitude. This radiation can limit the masses and sizes of the disks. Diversity in star forming environments can have long lasting effects in disk evolution and in the resulting planetary populations. We perform simulations to explore the evolution of circumstellar disks in young star clusters. We include viscous evolution, as well as the impact of dynamical encounters and external photoevaporation. We find that photoevaporation is an important process in destroying circumstellar disks: in regions of stellar density ρ ∼ 100 M pc −3 around 80% of disks are destroyed before 2 Myr of cluster evolution. Our findings are in agreement with observed disk fractions in young star forming regions and support previous estimations that planet formation must start in timescales < 0.1 − 1 Myr.Key words: key 1 key 2 1 G 0 is the FUV field measured in units of the Habing flux, 1.6 × 10 −3 erg s −1 cm −2 (Habing 1968).

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Multiple Stellar Flybys Sculpting the Circumstellar Architecture in RW Aurigae

Cited by 81 publications

References 59 publications

The origin of tail-like structures around protoplanetary disks

The origin of tail-like structures around protoplanetary disks

Exploring the dimming event of RW Aurigae A through multi-epoch VLT/X-shooter spectroscopy

External photoevaporation of circumstellar discs constrains the time-scale for planet formation

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