VELOCITY-DEPENDENT CATASTROPHIC DISRUPTION CRITERIA FOR PLANETESIMALS

By S. Stewart, Z. Leinhardt. 2009

177 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/382d533eb4085ca874870cb6805ce6ae5715553f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Nesvorný
2. Z. Leinhardt
3. S. Stewart
4. A. Morbidelli
5. A. Youdin
6. William Bottke
7. W. Benz
8. D. Lin

In Geophysics

1. M. Brown
2. Z. Leinhardt
3. S. Stewart
4. Derek C. Richardson
5. D. Nesvorný
6. A. Youdin
7. W. Benz
8. William Bottke

Citations in the corpus

• TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS (2010, background): “If these planetesimals have sizes larger than a few km (as in the Kuiper Belt, e.g., Pan & Sari 2005), their velocity dispersion would exceed that for disruptive collisions (Stewart & Leinhardt 2009).”
• Full numerical simulations of catastrophic small body collisions (2008, background): “D. Note that the slope is also about −0.5 for very low velocity (m s−1) collisions ( Stewart and Leinhardt, 2008 ).”
• FORMATION OF KUIPER BELT BINARIES BY GRAVITATIONAL COLLAPSE (2010, methodology): “The fragmentation can be included in the next generation models using scaling laws developed for low-speed collisions between icy bodies (e.g., Leinhardt & Stewart 2009; Stewart & Leinhardt 2009), even though it can be challenging to deal with the full complexity of the collisional cascade.”
• Dynamics of rotationally fissioned asteroids: Source of observed small asteroid systems (2011, background): “The middle plot shows the total velocity of the impactor relative to the target and compares this value to the catastrophic disruption velocity of Stewart and Leinhardt (2009).”
• The Compositions of Kuiper Belt Objects (2011, methodology): “Using scalings from numerical simulations of Stewart & Leinhardt (2009), we find that to remove enough ice mass to create an object with the ∼2.6 g cm−3 of Eris from an object that initially had the ∼2.0 g cm−3 of Pluto requires hitting Triton with a ∼ 500 km KBO traveling 40 km s−1!”
• COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, methodology): “3, and qs = 1 based on the work in Stewart & Leinhardt (2009). tion energy for small bodies (RC1 < 1000 km) and a high disruption energy for planet-sized bodies.”
• Fragment properties at the catastrophic disruption threshold: The effect of the parent body’s internal structure (2009, background): “Using these new variables, they found some differences with respect to the results plotted with the traditional ones (see Stewart and Leinhardt 2009 for details).”
• COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, background): “Instead of target radius, the variable RC1 was introduced by Stewart & Leinhardt (2009) in order to generalize the dependence of Q∗RD on size for different density bodies and for different projectile-to-target mass ratios.”
• Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, background): “For α ∼ 10, such particles collide at relative velocities Vrel ∼ VL ∼ 10 3 cm/sec - which are probably disruptive (Stewart and Leinhardt 2009).”
• Debris disc stirring by secular perturbations from giant planets (2009, unknown): “We are interested in the transition from net accretion to net erosion, and so use the conditionQR > Q∗RD, where Q∗RD = 0.095 J kg −1 „ RC1 100 m «−0.33 “ vrel 1m s−1 ”0.8 +0.025 J kg−1 „ RC1 100 m «1.2 “ vrel 1 ms−1 ”0.8 (21) for weak aggregates (Stewart & Leinhardt 2009).”