Volume 590, June 2016
|Number of page(s)||12|
|Published online||29 April 2016|
Spiral-driven accretion in protoplanetary discs
II. Self-similar solutions
Laboratoire AIM, Paris-Saclay, CEA/IRFU/SAp – CNRS – Université Paris
2 LERMA (UMR CNRS 8112), École Normale Supérieure, 75231 Paris Cedex, France
3 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
4 CNRS, IPAG, 38000 Grenoble, France
Accepted: 4 February 2016
Context. Accretion discs are ubiquitous in the Universe, and it is crucial to understand how angular momentum and mass are radially transported in these objects.
Aims. Here, we study the role played by non-linear spiral patterns within hydrodynamical and non-self-gravitating accretion discs assuming that external disturbances such as infall onto the disc may trigger them.
Methods. To do so, we computed self-similar solutions that describe discs in which a spiral wave propagates. These solutions present shocks and critical sonic points that were analyzed.
Results. We calculated the wave structure for all allowed temperatures and for several spiral shocks. In particular, we inferred the angle of the spiral pattern, the stress it exerts on the disc, and the associated flux of mass and angular momentum as a function of temperature. We quantified the rate of angular momentum transport by means of the dimensionless α parameter. For the thickest disc we considered (corresponding to h/r values of about one-third), we found values of α as high as 0.1 that scaled with the temperature T such that α ∝ T3 / 2 ∝ (h/r)3. The spiral angle scales with the temperature as arctan(r/h).
Conclusions. These solutions suggests that perturbations occurring at disc outer boundaries, such as perturbations due to infall motions, can propagate deep inside the disc and therefore should not be ignored, even when considering small radii.
Key words: protoplanetary disks / instabilities / hydrodynamics / accretion, accretion disks
© ESO, 2016
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