The UV Perspective of Low-Mass Star Formation

Abstract

The formation of low-mass stars in molecular clouds involves accretion disks and jets, which are of broad astrophysical interest. Accreting stars represent the closest examples of these phenomena. Star and planet formation are also intimately connected, setting the starting point for planetary systems like our own. The ultraviolet (UV) spectral range is particularly suited to study star formation, because virtually all relevant processes radiate at temperatures associated with UV emission processes or have strong observational signatures in the UV. In this review, we describe how UV observations provide unique diagnostics for the accretion process, the physical properties of the protoplanetary disk, and jets and outflows.

arXiv comment26 pages, 12 figures. Published in Galaxies special issue: "Star Formation in the UV", ed. Jorick Vink

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Cited by in corpus (9)

• The Mass Accretion Rate and Stellar Properties in Class I Protostars
• The ODYSSEUS Survey. Motivation and First Results: Accretion, Ejection, and Disk Irradiation of CVSO 109
• Multicolor Variability of Young Stars in the Lagoon Nebula: Driving Causes and Intrinsic Timescales
• On the Mass Accretion Rates of Herbig Ae/Be Stars. Magnetospheric Accretion or Boundary Layer?
• Lyman-alpha Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems
• Monitoring accretion rate variability in the Orion Nebula Cluster with the Wendelstein Wide Field Imager
• PENELLOPE VII: Revisiting empirical relations to measure accretion luminosity
• Pre main sequence: Accretion & Outflows
• Understanding Accretion Variability Through TESS Observations of Taurus