A triple star in disarray

Kasper, Markus; Santhakumari, Kalyan Kumar Radhakrishnan; Herbst, Tom; Boekel, R. van; Ménard, F.; Gratton, R. G.; Holstein, R. van; Langlois, M.; Ginski, C.; Boccaletti, A.; Benisty, M.; Boer, J. de; Delorme, P.; Desidera, S.; Dominik, C.; Hagelberg, J.; Henning, Thomas; Heidt, J.; Köhler, Rainer H.; Mesa, D.; Messina, S.; Pavlov, A.; Petit, Cyril; Rickman, E. L.; Roux, A.; Rigal, F.; Vigan, A.; Wahhaj, Z.; Zurlo, A.

doi:10.1051/0004-6361/202039186

Cited by 4 publications

(1 citation statement)

References 49 publications

(97 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The binary Sa,Sb is accreting from the circumbinary disk and drives an outflow; star N is also accreting. The kinematics of the gas and stars is complex, indicating that this system is misaligned and 'in disarray', using the words of Kasper et al [89]. Most of the mass is concentrated in the component S hosting the inner subsystem, suggestive of the inside-out formation scenario by the DI+CF or CF+CF mechanisms.…”

Section: Young Hierarchiesmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

View full text Add to dashboard Cite

Accumulation of new data on stellar hierarchical systems and the progress in numerical simulations of their formation open the door to genetic classification of these systems, where properties of a certain group (family) of objects are tentatively related to their formation mechanisms and early evolution. A short review of the structure and statistical trends of known stellar hierarchies is given. Like binaries, they can be formed by the disk and core fragmentation events happening sequentially or simultaneously and followed by the evolution of masses and orbits driven by continuing accretion of gas and dynamical interactions between stars. Several basic formation scenarios are proposed and associated qualitatively with the architecture of real systems, although quantitative predictions for these scenarios are still pending. The general trend of increasing orbit alignment with decreasing system size points to the critical role of the accretion-driven orbit migration, which also explains the typically comparable masses of stars belonging to the same system. The architecture of some hierarchies bears imprints of chaotic dynamical interactions. Characteristic features of each family are illustrated by several real systems.

show abstract

Section: Young Hierarchiesmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

View full text Add to dashboard Cite

show abstract

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Garufi

Podio

Codella

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Planet-forming disks are not isolated systems. Their interaction with the surrounding medium affects their mass budget and chemical content. In the context of the ALMA-DOT program, we obtained high-resolution maps of assorted lines from six disks that are still partly embedded in their natal envelope. In this work, we examine the SO and SO2 emission that is detected from four sources: DG Tau, HL Tau, IRAS 04302+2247, and T Tau. The comparison with CO, HCO+, and CS maps reveals that the SO and SO2 emission originates at the intersection between extended streamers and the planet-forming disk. Two targets, DG Tau and HL Tau, offer clear cases of inflowing material inducing an accretion shock on the disk material. The measured rotational temperatures and radial velocities are consistent with this view. In contrast to younger Class 0 sources, these shocks are confined to the specific disk region impacted by the streamer. In HL Tau, the known accreting streamer induces a shock in the disk outskirts, and the released SO and SO2 molecules spiral toward the star in a few hundred years. These results suggest that shocks induced by late accreting material may be common in the disks of young star-forming regions with possible consequences for the chemical composition and mass content of the disk. They also highlight the importance of SO and SO2 line observations in probing accretion shocks from a larger sample.

show abstract

The SPHERE view of the Taurus star-forming region

Garufi,

Ginski,

van Holstein

et al. 2024

A&A

Self Cite

View full text Add to dashboard Cite

The sample of planet-forming disks observed by high-contrast imaging campaigns over the last decade is mature enough to enable the demographical analysis of individual star-forming regions. We present the full census of Taurus sources with VLT/SPHERE polarimetric images available. The whole sample sums up to 43 targets (of which 31 have not been previously published) corresponding to one-fifth of the Class II population in Taurus and about half of such objects that are observable. A large fraction of the sample is apparently made up of isolated faint disks (equally divided between small and large self-shadowed disks). Ambient signal is visible in about one-third of the sample. This probes the interaction with the environment and with companions or the outflow activity of the system. The central portion of the Taurus region almost exclusively hosts faint disks, while the periphery also hosts bright disks interacting with their surroundings. The few bright disks are found around apparently older stars. The overall picture is that the Taurus region is in an early evolutionary stage of planet formation. Yet, some objects are discussed individually, as in an intermediate or exceptional stage of the disk evolution. This census provides a first benchmark for the comparison of the disk populations in different star forming regions.

show abstract

A triple star in disarray

Cited by 4 publications

References 49 publications

Architecture of Hierarchical Stellar Systems and Their Formation

Architecture of Hierarchical Stellar Systems and Their Formation

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

The SPHERE view of the Taurus star-forming region

Contact Info

Product

Resources

About