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1. The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

   https://doi.org/10.3847/2041-8213/aaf744  

   Zhang, Shangjia; Zhu, Zhaohuan; Huang, Jane; Guzmán, Viviana V.; Andrews, Sean M.; Birnstiel, Tilman; Dullemond, Cornelis P.; Carpenter, John M.; Isella, Andrea; Pérez, Laura M.; et al (December 2018, The Astrophysical Journal)
2. The Disk Substructures at High Angular Resolution Program (DSHARP). VIII. The Rich Ringed Substructures in the AS 209 Disk

   https://doi.org/10.3847/2041-8213/aaedae  

   Guzmán, Viviana V.; Huang, Jane; Andrews, Sean M.; Isella, Andrea; Pérez, Laura M.; Carpenter, John M.; Dullemond, Cornelis P.; Ricci, Luca; Birnstiel, Tilman; Zhang, Shangjia; et al (December 2018, The Astrophysical Journal)
3. Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence

   https://doi.org/10.3847/1538-4357/acbd47  

   Staff, Jan E.; Tanaka, Kei E. I.; Ramsey, Jon P.; Zhang, Yichen; Tan, Jonathan C. (April 2023, The Astrophysical Journal)

   Abstract Star formation is ubiquitously associated with the ejection of accretion-powered outflows that carve bipolar cavities through the infalling envelope. This feedback is expected to be important for regulating the efficiency of star formation from a natal prestellar core. These low-extinction outflow cavities greatly affect the appearance of a protostar by allowing the escape of shorter-wavelength photons. Doppler-shifted CO line emission from outflows is also often the most prominent manifestation of deeply embedded early-stage star formation. Here, we present 3D magnetohydrodynamic simulations of a disk wind outflow from a protostar forming from an initially 60M_⊙core embedded in a high-pressure environment typical of massive star-forming regions. We simulate the growth of the protostar fromm_*= 1M_⊙to 26M_⊙over a period of ∼100,000 yr. The outflow quickly excavates a cavity with a half opening angle of ∼10° through the core. This angle remains relatively constant until the star reaches 4M_⊙. It then grows steadily in time, reaching a value of ∼50° by the end of the simulation. We estimate a lower limit to the star formation efficiency (SFE) of 0.43. However, accounting for continued accretion from a massive disk and residual infall envelope, we estimate that the final SFE may be as high as ∼0.7. We examine observable properties of the outflow, especially the evolution of the cavity's opening angle, total mass, and momentum flux, and the velocity distributions of the outflowing gas, and compare with the massive protostars G35.20-0.74N and G339.88-1.26 observed by the Atacama Large Millimeter/submillimeter Array (ALMA), yielding constraints on their intrinsic properties. 

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4. The Disk Substructures at High Angular Resolution Project (DSHARP). X. Multiple Rings, a Misaligned Inner Disk, and a Bright Arc in the Disk around the T Tauri star HD 143006

   https://doi.org/10.3847/2041-8213/aaf745  

   Pérez, Laura M.; Benisty, Myriam; Andrews, Sean M.; Isella, Andrea; Dullemond, Cornelis P.; Huang, Jane; Kurtovic, Nicolás T.; Guzmán, Viviana V.; Zhu, Zhaohuan; Birnstiel, Tilman; et al (December 2018, The Astrophysical Journal)
5. Chemodynamical Analysis of Metal-rich High-eccentricity Stars in the Milky Way's Disk

   https://doi.org/10.3847/1538-4357/acb6f5  

   Lee, Ayeon; Lee, Young Sun; Kim, Young Kwang; Beers, Timothy C.; An, Deokkeun (March 2023, The Astrophysical Journal)

   Abstract We present a chemodynamical analysis of 11,562 metal-rich, high-eccentricity halo-like main-sequence stars, which have been referred to as the Splash or Splashed Disk, selected from the Sloan Digital Sky Survey and Large Sky Area Multi-Object Fiber Spectroscopic Telescope. When divided into two groups, a low-[ α /Fe] population (LAP) and a high-[ α /Fe] population (HAP), based on kinematics and chemistry, we find that they exhibit very distinct properties, indicative of different origins. From a detailed analysis of their orbital inclinations, we suggest that the HAP arises from a large fraction (∼90%) of heated disk stars and a small fraction (∼10%) of in situ stars from a starburst population, likely induced by interaction of the Milky Way with the Gaia-Sausage/Enceladus (GSE) or another early merger. The LAP comprises about half accreted stars from the GSE and half formed by the GSE-induced starburst. Our findings further imply that the Splash stars in our sample originated from at least three different mechanisms: accretion, disk heating, and a merger-induced starburst. 

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