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Angular momentum transport via gravitational instability in the Elias 2–27 disc
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-05-28 , DOI: 10.1051/0004-6361/202450187 C. Longarini , G. Lodato , C. J. Clarke , J. Speedie , T. Paneque-Carreño , E. Arrigoni , P. Curone , C. Toci , C. Hall
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-05-28 , DOI: 10.1051/0004-6361/202450187 C. Longarini , G. Lodato , C. J. Clarke , J. Speedie , T. Paneque-Carreño , E. Arrigoni , P. Curone , C. Toci , C. Hall
Gravitational instability is thought to be one of the main drivers of angular momentum transport in young protoplanetary discs. The disc around Elias 2−27 offers a unique example of gravitational instability at work. It is young and massive, displaying two prominent spiral arms in dust continuum emission and global non-axisymmetric kinematic signatures in molecular line data. In this work, we used archival ALMA observations of 13CO line emission to measure the efficiency of angular momentum transport in the Elias 2−27 system through the kinematic signatures generated by gravitational instability, known as “GI wiggles”. Assuming the angular momentum is transported by the observed spiral structure and leveraging previously-derived dynamical disc mass measurements, the amount of angular momentum transport we found corresponds to an α-viscosity of α = 0.038 ± 0.018. This value implies an accretion rate onto the central star of log10 Ṁ⋆ = −6.99 ± 0.17 M⊙ yr−1, which reproduces the one observed value of log10 Ṁ⋆,obs = −7.2 ± 0.5 M⊙ yr−1 very well. The excellent agreement we have found serves as further proof that gravitational instability is the main driver of angular momentum transport acting in this system.
更新日期：2024-05-28
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