Planetary formation: the role of physical uncertainties in planetesimal fragmentation and disruption

SAN SEBASTIAN, IRINA L.; GUILERA, O. ; PARISI, M. G.

Hallig Hooghe

Encuentro; TU IGeP Hallig Hooge retreat in ''Planetesimal Formation''; 2017

TU (Technische Universitat Braunschweig) IGeP

Modern planetary formation models  (Inaba et al. 2003, Kobayasahi et al. 2010,2011, Morbidelli et al. 2009, Chambers 2014, and Guilera et al. 2014)  include the interaction among planetesimals. The collision between two planetesimals may result in agglomeration, compaction, fragmentation, erosion and/or disruption, where QD* is defined as the specific impact energy  per unit target mass which is the energy required to disperse 50% of the target mass and Q is the collisional energy per unit target mass. All the planetary formation models mentioned above adopt QD*  correspondig to basalts at a collision velocity Vrel of 3 km/seg (Benz & Aspaugh, 1999)for all materials and impact velocities. We are working interpolating QD*  for  Vrel  25 m/s, 3 km/s and 5 km/s for basalts and Vrel  0.5 km/s and 3 km/s for ice from Benz & Asphaug (1999) and Benz (2000)  using a mixture of both materials.