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Validity of PDR models for thermalized near-IR H₂ in the disk wind

Ascertain whether photodissociation region models at the derived disk-wind densities (hydrogen nuclei density ≥10^5 cm⁻³ with H₂ abundance ≤10⁻³) can reproduce the thermalization of the near‑infrared H₂ levels for reasonable far‑UV radiation field strengths (G₀) and on the observed spatial scales in DG Tau B.

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Background

The authors propose that the hot H₂ emission may trace a dense photodissociated layer (PDR-like) along inner magnetized disk-wind streamlines. Given the inferred densities and abundances, they highlight the need to verify that realistic PDR models can produce the observed level thermalization at the spatial scales and radiation fields present in DG Tau B.

References

However, it remains to be checked that PDR models at the derived disk wind densities (n$_H$ $7$ 10${5}$ cm${-3}$ for H$_2$ abundance $7$ 10${-3}$ see 2 4.3 above) can reproduce the thermalization of the H$_2$ levels for reasonable G$_0$ values and on the spatial scales observed here.

— JWST study of the DG Tau B disk wind candidate: I -- Overview and Nested H$_2$/CO outflows (2403.19400 - Delabrosse et al., 28 Mar 2024) in Section 5.2 (MHD Disk wind scenario)