Volume 635, March 2020
|Number of page(s)||16|
|Section||Planets and planetary systems|
|Published online||06 March 2020|
Dust entrainment in photoevaporative winds: The impact of X-rays
Faculty of Physics, University Observatory, Ludwig-Maximilians-Universität München,
2 Excellence Cluster Origin and Structure of the Universe, Boltzmannstr. 2, 85748 Garching, Germany
Accepted: 8 January 2020
Context. X-ray- and extreme ultraviolet (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 investigate the dust entrainment in XEUV-driven photoevaporative winds and compare our results to existing magnetohydrodynamic and EUV-only models.
Methods. We used a 2D hydrodynamical gas model of a protoplanetary disk irradiated by both X-ray and EUV spectra from a central T Tauri star to trace the motion of passive Lagrangian dust grains of various sizes. The trajectories were modelled starting at the disk surface in order to investigate dust entrainment in the wind.
Results. For an X-ray luminosity of LX = 2 × 1030 erg s−1 emitted by a M* = 0.7 M⊙ star, corresponding to a wind mass-loss rate of Ṁw ≃ 2.6 × 10−8 M⊙ yr−1, we find dust entrainment for sizes a0 ≲ 11 μm (9 μm) from the inner 25 AU (120 AU). This is an enhancement over dust entrainment in less vigorous EUV-driven winds with Ṁw ≃ 10−10 M⊙ yr−1. Our numerical model also shows deviations of dust grain trajectories from the gas streamlines even for μm-sized particles. In addition, we find a correlation between the size of the entrained grains and the maximum height they reach in the outflow.
Conclusions. X-ray-driven photoevaporative winds are expected to be dust-rich if small grains are present in the disk atmosphere.
Key words: protoplanetary disks / X-rays: stars / accretion, accretion disks / circumstellar matter / stars: pre-main sequence / stars: winds, outflows
© ESO 2020
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