Dust entrainment in photoevaporative winds: densities and imaging
Author
dc.contributor.author
Franz, R.
Author
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Ercolano, B.
Author
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Casassus Montero, Simón Pablo
Author
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Picogna, G.
Author
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Birnstiel, T.
Author
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Pérez, S.
Author
dc.contributor.author
Rab, Ch
Author
dc.contributor.author
Sharma, A.
Admission date
dc.date.accessioned
2022-11-24T13:06:45Z
Available date
dc.date.available
2022-11-24T13:06:45Z
Publication date
dc.date.issued
2022
Cita de ítem
dc.identifier.citation
A&A 657, A69 (2022)
es_ES
Identifier
dc.identifier.other
10.1051/0004-6361/202140812
Identifier
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https://repositorio.uchile.cl/handle/2250/189349
Abstract
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Context. X-ray- and extreme-ultraviolet- (together: XEUV-) driven photoevaporative winds acting on protoplanetary disks around
young T-Tauri stars may crucially impact disk evolution, affecting both gas and dust distributions.
Aims. We constrain the dust densities in a typical XEUV-driven outflow, and determine whether these winds can be observed at µmwavelengths.
Methods. We used dust trajectories modelled atop a 2D hydrodynamical gas model of a protoplanetary disk irradiated by a central
T-Tauri star. With these and two different prescriptions for the dust distribution in the underlying disk, we constructed wind density
maps for individual grain sizes. We used the dust density distributions obtained to synthesise observations in scattered and polarised
light.
Results. For an XEUV-driven outflow around a M∗ = 0.7 M T-Tauri star with LX = 2 × 1030 erg s−1
, we find a dust mass-loss rate
M˙
dust . 4.1 × 10−11 M yr−1
for an optimistic estimate of dust densities in the wind (compared to M˙
gas ≈ 3.7 × 10−8 M yr−1
). The
synthesised scattered-light images suggest a distinct chimney structure emerging at intensities I/Imax < 10−4.5
(10−3.5
) at λobs = 1.6
(0.4) µm, while the features in the polarised-light images are even fainter. Observations synthesised from our model do not exhibit
clear features for SPHERE IRDIS, but show a faint wind signature for JWST NIRCam under optimal conditions.
Conclusions. Unambiguous detections of photoevaporative XEUV winds launched from primordial disks are at least challenging with
current instrumentation; this provides a possible explanation as to why disk winds are not routinely detected in scattered or polarised
light. Our calculations show that disk scale heights retrieved from scattered-light observations should be only marginally affected by
the presence of an XEUV wind.
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Lenguage
dc.language.iso
en
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Publisher
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EDP Sciences
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Type of license
dc.rights
Attribution-NonCommercial-NoDerivs 3.0 United States