scholarly journals The onset of flysch sedimentation in the Kaoko Belt (NW Namibia) – Implications for the pre-collisional evolution of the Kaoko–Dom Feliciano–Gariep orogen

2017 ◽  
Vol 298 ◽  
pp. 220-234 ◽  
Author(s):  
Jiří Konopásek ◽  
Karl-Heinz Hoffmann ◽  
Jiří Sláma ◽  
Jan Košler
2010 ◽  
Vol 18 (4) ◽  
pp. 688-707 ◽  
Author(s):  
V. Janoušek ◽  
J. Konopásek ◽  
S. Ulrich ◽  
V. Erban ◽  
L. Tajčmanová ◽  
...  

1999 ◽  
Vol 31 (4) ◽  
pp. 239-248 ◽  
Author(s):  
H. Ghildiyal ◽  
E. Jansen ◽  
A. Kirfel

The volume texture of a naturally deformed quartzite from the Kaoko belt, North-West Namibia, has been analysed by both universal stage microscopy and neutron diffraction. Universal stage microscopy is restricted to the determination of the base pinacoid preferred orientation in quartzite. For a more complete description of the texture, the orientations of additional crystal planes, such as first and second order prisms as well as positive and negative rhombs, must be known. Neutron methods allow the evaluation of pole figures of all Bragg reflecting planes, of which those of the first order prisms being considered to be the most active slip planes, are of particular interest. Drawbacks of neutron diffraction, i.e. the faking of an eventually absent inversion centre and lack of resolution, can be overcome by pole figure inversion and subsequent calculation of desired pole figures. Both, universal stage microscopy and neutron diffraction yield well comparable results, of course only with respect to the pole figure of the c-axis.


2006 ◽  
Vol 70 (18) ◽  
pp. A182
Author(s):  
D.A. Foster ◽  
S.J. Coyner ◽  
P.A. Mueller ◽  
G.D. Kamenov ◽  
D.R. Gray ◽  
...  
Keyword(s):  

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

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

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

Author(s):  
Jaume Vergés ◽  
Manel Fernàndez ◽  
Albert Martìnez

2009 ◽  
Vol 5 (S263) ◽  
pp. 98-101 ◽  
Author(s):  
Gonzalo C. de Elía ◽  
Romina P. Di Sisto ◽  
Adrián Brunini

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.


2020 ◽  
Vol 492 (4) ◽  
pp. 5709-5720
Author(s):  
Loic Nassif-Lachapelle ◽  
Daniel Tamayo

ABSTRACT Direct imaging surveys have found that long-period super-Jupiters are rare. By contrast, recent modelling of the widespread gaps in protoplanetary discs revealed by Atacama Large Millimetre Array suggests an abundant population of smaller Neptune to Jupiter-mass planets at large separations. The thermal emission from such lower-mass planets is negligible at optical and near-infrared wavelengths, leaving only their weak signals in reflected light. Planets do not scatter enough light at these large orbital distances, but there is a natural way to enhance their reflecting area. Each of the four giant planets in our Solar system hosts swarms of dozens of irregular satellites, gravitationally captured planetesimals that fill their host planets’ spheres of gravitational influence. What we see of them today are the leftovers of an intense collisional evolution. At early times, they would have generated bright circumplanetary debris discs. We investigate the properties and detectability of such irregular satellite discs (ISDs) following models for their collisional evolution from Kennedy & Wyatt (2011). We find that the scattered light signals from such ISDs would peak in the 10–100 au semimajor axis range implied by ALMA, and can render planets detectable over a wide range of parameters with upcoming high-contrast instrumentation. We argue that future instruments with wide fields of view could simultaneously characterize the atmospheres of known close-in planets, and reveal the population of long-period Neptune–Jupiter mass exoplanets inaccessible to other detection methods. This provides a complementary and compelling science case that would elucidate the early lives of planetary systems.


Sign in / Sign up

Export Citation Format

Share Document