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abstract: 'We revisit, via a very simplified set of equations, a linear streaming instability (technically an overstability), which is present in, and potentially important for, dusty protoplanetary disks [@YoudinGoodman2005]. The goal is a better understanding of the physical origin of such instabilities, which are notoriously subtle. Rotational dynamics seem to be essential to this type of instability, which cannot be captured by one-dimensional Cartesian models. Dust ‘pileups’ in moving pressure maxima are an important triggering mechanism of the instability, and drag feedback of dust upon the gas allows these maxima to be strengthened. Coriolis forces and the background drift counteract the effects of the pressure force.'
author:
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    Emmanuel Jacquet,$^1$ Steven Balbus,$^2$ Henrik Latter$^3$\
    $^1$LMCM, Muséum National d’Histoire Naturelle, 57 rue Cuvier, 75005 Paris, France\
    $^2$LRA, Ecole Normale Supérieure, 45 rue d’Ulm, 75005 Paris, France\
    $^3$AFD Group, DAMTP, University of Cambridge, CMS Wilberforce Rd, Cambridge UK CB3 0WA
bibliography:
- 'bibliography.bib'
title: 'On linear dust-gas streaming instabilities in protoplanetary discs'
---

Introduction
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The formation of planets via dust accretion starting with micron-sized grains and ending with $10^4-10^5$-km-sized bodies in a protoplanetary disc is a multiphase process (see e.g. the review by @ChiangYoudin2010, henceforth CY10). Grains smaller than 