The Nebular Shock Wave Model for Chondrule Formation: Shock Processing in a Particle–Gas Suspension

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Asteroids Were Born Big (2009, background): “The particles eventually stick together through electrostatic forces, forming larger fractal aggregates (Dominik and Tielens, 1997; Kempf et al., 1999; Wurm and Blum, 1998, 2000; Colwell and Taylor, 1999; Blum et al., 2000).”
Chondrules and the Protoplanetary Disk (2011, background): “Several groups have shown that millimetersized silicate grains in the nebula could have been heated during passage of a shock wave and cooled at the rates inferred from laboratory experiments (Iida et al. 2001, Desch & Connolly 2002, Ciesla & Hood 2002, Desch et al. 2005).”
Chondrule formation during planetesimal accretion (2011, background): “…popular idea that low density mechanical aggregates of solar-composition dust, or pre-chondrules of some sort, were melted when the nebula was heated by powerful shocks (e.g. Boss and Durisen 2005; Ciesla and Hood, 2002; Desch and Connolly, 2002; Morris and Desch, 2010) whose cause is much debated.”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, background): “Many were melted after they were formed, possibly by nebular shock waves (Ciesla & Hood 2002, Desch & Connolly 2002, Hood & Horanyi 1993, Richter et al. 2006) or by passage near the Sun and launch to the meteorite-forming region by the X-wind (Shu et al. 1996).”