Origin and impact of protostellar outflows

Determine the physical origin of protostellar outflows (including collimated jets and wider molecular outflows) and quantify their impact on protoplanetary disk evolution and planet formation processes.

Background

The paper investigates DG Tau B, a Class I protostar with a structured disk and rotating CO outflow, as a prime system to study outflow origins and their consequences for disk evolution. The authors emphasize that understanding whether outflows arise from mechanisms such as magnetohydrodynamic disk winds or swept-up envelope material, and how they regulate mass and angular momentum in disks, remains pivotal for models of disk evolution and planet formation.

References

The origin of outflows and their impact on proto-planetary disk evolution and planet formation processes are still crucial open questions.

— JWST study of the DG Tau B disk wind candidate: I -- Overview and Nested H$_2$/CO outflows  (2403.19400 - Delabrosse et al., 2024) in Abstract, first paragraph

Nevertheless, we does not exclude the possibility that they are molecular outflows associated with the central target.

— Disk survey in the Serpens star-forming region: Environmental effects in nearby star-forming regions  (2609.03759 - Tong et al., 3 Sep 2026) in Section 3.3, Outflows

This geometry alone, however, does not distinguish magnetocentrifugal launching from acceleration by gradients in the toroidal magnetic pressure.

— Magnetically Driven Obliquity in Circumplanetary Disks and Twisted Bipolar-jet Formation  (2609.10035 - Chametla et al., 9 Sep 2026) in Section 5.2, “Twisted bipolar jet ejection mechanisms”