2022A&A...657A..69F


Query : 2022A&A...657A..69F

2022A&A...657A..69F - Astronomy and Astrophysics, volume 657A, 69-69 (2022/1-1)

Dust entrainment in photoevaporative winds: Densities and imaging.

FRANZ R., ERCOLANO B., CASASSUS S., PICOGNA G., BIRNSTIEL T., PEREZ S., RAB C. and SHARMA A.

Abstract (from CDS):


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 µm-wavelengths.
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 x 1030 erg/s, we find a dust mass-loss rate Mdust ≥ 4.1 x 10–11 M/yr for an optimistic estimate of dust densities in the wind (compared to Mgas ≃ 3.7 x 10–8 M/yr). 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.

Abstract Copyright: © ESO 2022

Journal keyword(s): X-rays: stars - stars: variables: T Tauri, Herbig Ae/Be - stars: winds, outflows - stars: pre-main sequence - protoplanetary disks

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IRAS 04158+2805 Y*O 04 18 58.1336295120 +28 12 23.355499140           M5.25 97 0
2 2MASS J04202144+2813491 Y*O 04 20 21.44280 +28 13 49.1736           M1 31 0
3 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 548 0
4 V* HV Tau C TT* 04 38 35.5125950280 +26 10 41.316576204         14.90 K6 93 0
5 THA 15-12 Or* 15 56 09.2066646912 -37 56 06.126118692   13.12 11.93 11.45   M0e 360 0
6 V* RY Lup Or* 15 59 28.3864710696 -40 21 51.249496176   12.62 9.90     G8/K1IV-V 204 0
7 V* MY Lup TT* 16 00 44.5202267160 -41 55 30.935126748   12.64 12.17 11.06   K0 92 0
8 DoAr 25 TT* 16 26 23.6911292736 -24 43 13.888543800       12.65   K5 154 0
9 Haro 1-16 Or* 16 31 33.4634997336 -24 27 37.158728076   14.02 12.80     K3e 210 0

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2023.01.27-19:15:35

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