The Growth Mechanisms of Macroscopic Bodies in Protoplanetary Disks

By J. Blum, G. Wurm. 2008

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View Paper: https://www.semanticscholar.org/paper/7be7e2dd5344dd2f6a37522afbb90a76de5a233e

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In Astronomy and Astrophysics

Citations in the corpus

Dust Evolution and the Formation of Planetesimals (2016, background): “Still, many studies have shed light on this enormous parameter space and identified possible outcomes and how they depend on or scale with particle properties and collisional parameters (see Blum & Wurm 2008; Testi et al. 2014; Johansen et al. 2014, for recent reviews).”
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK (2012, background): “…turbulent relative motion of particles causes collisions that either grow or fragment these grains, seems incompatible for standard values of the turbulence parameter (αt = 0.01, Shakura & Sunyaev 1973), fragmentation threshold velocity (ut = 10 m/s, Blum & Wurm 2008), and 100:1 gasto-dust ratio.”
The outcome of protoplanetary dust growth: pebbles, boulders or planetesimals? (2009, methodology): “In the past years, numerous laboratory and space experiments on the collisional evolution of protoplanetary dust have been performed (Blum & Wurm 2008).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, methodology): “For icy grains, we take vf = 10 m s −1 (Gundlach & Blum 2015), while for ‘dry’ grains we use the fragmentation threshold for silicates, vf = 1 m s −1 (Blum & Wurm 2008).”
The Inner Regions of Protoplanetary Disks (2010, background): “For instance, dust particles that collide at these high temperatures may stick and melt together due to processes such as sintering and/or eutectic melting (see e.g. Blum & Wurm, 2008).”
THE STICKINESS OF MICROMETER-SIZED WATER-ICE PARTICLES (2014, background): “In contrast to silicates, for which empirical evidence for the low-velocity collision behavior exists (Blum & Wurm 2008; Güttler et al. 2010), the collision properties of carbonaceous materials and ices (and, in particular, of the most abundant water ice) are mainly unknown.”
Fluffy dust forms icy planetesimals by static compression (2013, background): “…has been an unsolved problem in the complete planet formation theory; the intermediate-sized bodies are believed to be poorly sticky (Zsom et al. 2010), easily disrupted by collisions (Blum & Wurm 2008), or liable to fall quickly onto the central star (Adachi et al. 1976; Weidenschilling 1977).”
Breaking through: The effects of a velocity distribution on barriers to dust growth (2012, background): “As laboratory experiments (Blum & Wurm 2008; Güttler et al. 2010) and numerical simulations (Zsom et al. 2010; Birnstiel et al. 2010) have improved our understanding of the collision process and the dust evolution, it has become evident that incremental growth to form planetesimals cannot continue…”
Astrophysics with Extraterrestrial Materials (2016, background): “These more energetic collisions stop being accretional and instead result in bouncing (no mass transfer) or are erosional (all resulting dust aggregates are smaller than the original colliding pair), thus frustrating growth (see review by Blum & Wurm 2008).”
Astrochemistry and compositions of planetary systems (2020, background): “Once grains grow they settle towards the midplane and drift inwards (Blum and Wurm 2008), which can result in substantial redistribution of volatiles both vertically and radially (Cuzzi and Zahnle 2004; Ciesla and Cuzzi 2006; Meijerink et al.”
Trapping dust particles in the outer regions of protoplanetary disks (2011, background): “Laboratory experiments and theoretical work suggest that typical values for fragmentation velocities are of the order of few m s−1 for silicate dust (see e. g. Blum & Wurm 2008).”
Free collisions in a microgravity many-particle experiment. I. Dust aggregate sticking at low velocities (2011, background): “Many laboratory experiments have shown that millimeter-sized particles do not stick to each other if they collide at a velocity which is expected to occur under the conditions in a PPD (see review by Blum and Wurm (2008) and recent experiments by Beitz et al. (2011)). Indeed, the sticking velocities”
Ice Condensation as a Planet Formation Mechanism (2013, background): “Sticking, or coagulation, as a growth mechanism has been extensively studied, both experimentally (Blum & Wurm, 2008; Zsom et al., 2010) and numerically (Brauer et al., 2008; Windmark et al., 2012).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, background): “At these large collision energies, the particles tend to fragment rather thanstick (Blum & Wurm 2008), which effectively prevents further growth (Dullemond & Dominik 2005; Brauer et al. 2008; Birnstiel et al. 2010).”
Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities (2011, background): “Perhaps these planetesimal bursts were “abandoned” by the 8 This does require sufficient amounts of pebbles and rocks to begin with, the formation of which is not yet well-understood (Blum & Wurm 2008).”
Protoplanetary Disks and Their Evolution (2011, background): “Collisional grain growth (Blum & Wurm 2008) is expected to have a strong radial dependence due to the decreasing density and rotational velocity with increasing radius.”
Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution (2009, background): “Over the last decade, a number of elegant experimental studies by Blum and coworkers (see Blum & Wurm 2008) have provided direct support for these concepts and in many ways expanded our understanding of the coagulation process.”
Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “The collision processes described here have been extensively investigated in the laboratory and can be considered robust (Blum & Wurm 2008; Güttler et al. 2010).”