Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
arxiv(2024)
摘要
[Ne II] 12.81 μm emission is a well-used tracer of
protoplanetary disk winds due to its blueshifted line profile. MIRI-MRS
recently observed T Cha, detecting this line along with lines of [Ne III], [Ar
II] and [Ar III], with the [Ne II] and [Ne III] lines found to be extended
while the [Ar II] was not. In this complementary work, we use these lines to
address long-debated questions about protoplanetary disk winds regarding their
mass-loss rate, the origin of their ionization, and the role of
magnetically-driven winds as opposed to photoevaporation. To this end, we
perform photoionization radiative transfer on simple hydrodynamic wind models
to map the line emission. We compare the integrated model luminosities to those
observed with MIRI-MRS to identify which models most closely reproduce the data
and produce synthetic images from these to understand what information is
captured by measurements of the line extents. Along with the low degree of
ionization implied by the line ratios, the relative compactness of [Ar II]
compared to [Ne II] is particularly constraining. This requires Ne II
production by hard X-rays and Ar II production by soft X-rays (and/or EUV) in
an extended (≳ 10 au) wind that is shielded from soft X-rays -
necessitating a dense wind with material launched on scales down to 1 au. Such
conditions could be produced by photoevaporation, whereas an extended MHD wind
producing equal shielding would likely underpredict the line fluxes. However, a
tenuous inner MHD wind may still contribute to shielding the extended wind.
This picture is consistent with constraints from spectrally-resolved line
profiles.
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