scholarly journals Collisional Evolution of the Inner Zodiacal Cloud

2021 ◽  
Vol 2 (5) ◽  
pp. 185 ◽  
Author(s):  
J. R. Szalay ◽  
P. Pokorný ◽  
D. M. Malaspina ◽  
A. Pusack ◽  
S. D. Bale ◽  
...  
Keyword(s):  
Zodiacal Cloud ◽  
Collisional Evolution

The Collisional Evolution of the Asteroid Belt and Its Contribution to the Zodiacal Cloud

Icarus ◽  
1997 ◽  
Vol 130 (1) ◽  
pp. 140-164 ◽  
Author(s):  
Daniel D. Durda ◽  
Stanley F. Dermott
Keyword(s):  
Asteroid Belt ◽  
Zodiacal Cloud ◽  
Collisional Evolution

Asteroid collisions as origin of debris disks: Asteroid shape reconstruction from BNAO Rozhen photometry

2019 ◽  
Vol 15 (S350) ◽  
pp. 451-453
Author(s):  
G. Apostolovska ◽  
E. Vchkova Bebekovska ◽  
A. Kostov ◽  
Z. Donchev
Keyword(s):  
Laboratory Experiments ◽  
Extrasolar Planets ◽  
Shape Reconstruction ◽  
Inversion Method ◽  
Debris Disks ◽  
Shape Parameters ◽  
Zodiacal Cloud ◽  
Photometric Observations ◽  
Different Shapes ◽  
Asteroid Surface

AbstractAs a result of collisions during their lifetimes, asteroids have a large variety of different shapes. It is believed that high velocity collisions or rotational spin-up of asteroids continuously replenish the Sun’s zodiacal cloud and debris disks around extrasolar planets (Jewitt (2010)). Knowledge of the spin and shape parameters of the asteroids is very important for understanding collision asteroid processes. Lately photometric observations of asteroids showed that variations in brightness are not accompanied by variations in colour index which indicate that the shape of the lightcurve is caused by varying illuminations of the asteroid surface rather than albedo variations over the surface. This conclusion became possible when photometric investigations were combined with laboratory experiments (Dunlap (1971)). In this article using the convex lightcurve inversion method we obtained the sense of rotation, pole solutions and preliminary shape of 901 Brunsia.

Asteroid collisional evolution

Icarus ◽  
1990 ◽  
Vol 87 (2) ◽  
pp. 391-402 ◽  
Author(s):  
A. Cellino ◽  
V. Zappalà ◽  
D.R. Davis ◽  
P. Farinella ◽  
P. Paolicchi
Keyword(s):  
Collisional Evolution

Collisional Evolution of Small-Body Populations

Asteroids III ◽  
2002 ◽  
pp. 545-558
Author(s):  
Donald R. Davis ◽  
Daniel D. Durda ◽  
Francesco Marzari ◽  
Adriano Campo Bagatin ◽  
Ricardo Gil-Hutton
Keyword(s):  
Small Body ◽  
Collisional Evolution

The Pyrenean orogen: pre-, syn-, and post-collisional evolution

2002 ◽  
Vol 08 ◽  
Author(s):  
Jaume Vergés ◽  
Manel Fernàndez ◽  
Albert Martìnez
Keyword(s):  
Collisional Evolution

2.1.8 Sources of Interplanetary Dust: Asteroids

1976 ◽  
Vol 31 ◽  
pp. 187-205 ◽  
Author(s):  
J. S. Dohnanyi
Keyword(s):  
Interplanetary Dust ◽  
Asteroid Belt ◽  
The Sun ◽  
Number Density ◽  
Zodiacal Cloud ◽  
Relative Contribution ◽  
Potential Source ◽  
Asteroidal Belt ◽  
Pioneer 10

AbstractThe asteroid belt is examined as a potential source of interplanetary dust. Using results from the Pioneer-10 experiments the relative contribution of asteroidal and cometary particles to the Zodiacal cloud is estimated using methods developed in earlier studies of meteoroidal collisions (collisional model). It is found that the contribution of asteroidal particles to dust in the asteroidal belt is small compared with the number density of cometary type particles. Similar conclusions apply to the Zodiacal cloud between the sun and the asteroid belt. When definitive criteria for differentiating between comets and asteroids become available, a reexamination of some of our conclusions may become necessary.The distribution of asteroidal rotations is analyzed; it is found that the gross features of the distribution can be reproduced using the collisional model.

scholarly journals Impactor Flux on the Pluto-Charon System

2009 ◽  
Vol 5 (S263) ◽  
pp. 98-101 ◽  
Author(s):  
Gonzalo C. de Elía ◽  
Romina P. Di Sisto ◽  
Adrián Brunini
Keyword(s):  
Size Distribution ◽  
Kuiper Belt ◽  
Primary Source ◽  
Mean Motion ◽  
Stability And Instability ◽  
The Stability ◽  
Mean Motion Resonance ◽  
Collisional Evolution

AbstractIn this work, we study the impactor flux on Pluto and Charon due to the collisional evolution of Plutinos.To do this, we develop a statistical code that includes catastrophic collisions and cratering events, and takes into account the stability and instability zones of the 3:2 mean motion resonance with Neptune. Our results suggest that if 1 Pluto-sized object is in this resonance, the flux of D = 2 km Plutinos on Pluto is ~4–24 percent of the flux of D = 2 km Kuiper Belt projectiles on Pluto. However, with 5 Pluto-sized objects in the resonance, the contribution of the Plutino population to the impactor flux on Pluto may be comparable to that of the Kuiper Belt. As for Charon, if 1 Pluto-sized object is in the 3:2 resonance, the flux of D = 2 km Plutinos is ~10–63 percent of the flux of D = 2 km impactors coming from the Kuiper Belt. However, with 5 Pluto-sized objects, the Plutino population may be a primary source of the impactor flux on Charon. We conclude that it is necessary to specify the Plutino size distribution and the number of Pluto-sized objects in the 3:2 Neptune resonance in order to determine if the Plutino population is a primary source of impactors on the Pluto-Charon system.

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