scholarly journals The Debiased Kuiper Belt: Our Solar System as a Debris Disk

2013 ◽  
Vol 8 (S299) ◽  
pp. 232-236 ◽  
Author(s):  
Samantha M. Lawler ◽  
Keyword(s):  
Solar System ◽  
Large Fraction ◽  
Kuiper Belt ◽  
Ecliptic Plane ◽  
Asteroid Belt ◽  
Debris Disks ◽  
Disk Model ◽  
Excellent Starting Point ◽  
Starting Point ◽  
Debris Disk

AbstractThe dust measured in debris disks traces the position of planetesimal belts. In our Solar System, we are also able to measure the largest planetesimals directly and can extrapolate down to make an estimate of the dust. The zodiacal dust from the asteroid belt is better constrained than the only rudimentary measurements of Kuiper belt dust. Dust models will thus be based on the current orbital distribution of the larger bodies which provide the collisional source. The orbital distribution of many Kuiper belt objects is strongly affected by dynamical interactions with Neptune, and the structure cannot be understood without taking this into account. We present the debiased Kuiper belt as measured by the Canada-France Ecliptic Plane Survey (CFEPS). This model includes the absolute populations for objects with diameters >100 km, measured orbital distributions, and size distributions of the components of the Kuiper belt: the classical belt (hot, stirred, and kernel components), the scattering disk, the detached objects, and the resonant objects (1:1, 5:4, 4:3, 3:2 including Kozai subcomponent, 5:3, 7:4, 2:1, 7:3, 5:2, 3:1, and 5:1). Because a large fraction of known debris disks are consistent with dust at Kuiper belt distances from the host stars, the CFEPS Kuiper belt model provides an excellent starting point for a debris disk model, as the dynamical interactions with planets interior to the disk are well-understood and can be precisely modelled using orbital integrations.

Natural transportation routes in the Solar System

2019 ◽  
Vol 15 (S350) ◽  
pp. 471-473
Author(s):  
Nataša Todorović
Keyword(s):  
Solar System ◽  
Large Fraction ◽  
Outer Part ◽  
Asteroid Belt ◽  
Water Molecules ◽  
Early Solar System ◽  
Type Water ◽  
Transportation Routes

AbstractThe aim of this work is to explain the possible mechanism in the early Solar System, by which water-rich asteroids may have been delivered to Earth. Carbonaceous (C-type) asteroids, with a large fraction of water molecules, dominate in the outer part of the asteroid belt and the possibility of their migration toward Earth is still not well explained. In this work, we observe very efficient dynamical routes along which C-type water-bearing asteroids are delivered to Earth.

scholarly journals On the solar system—debris disk connection

2007 ◽  
Vol 3 (S249) ◽  
pp. 347-354 ◽  
Author(s):  
Amaya Moro-Martín
Keyword(s):  
Solar System ◽  
Debris Disks ◽  
Debris Disk

AbstractThis paper emphasizes the connection between solar and extra-solar debris disks: how models and observations of the Solar System are helping us understand the debris disk phenomenon, and vice versa, how debris disks are helping us place our Solar System into context.

scholarly journals The Locations of Secular Resonances and the Evolution of Small Solar System Bodies

1992 ◽  
Vol 152 ◽  
pp. 123-132
Author(s):  
Ch Froeschle ◽  
P. Farinella ◽  
C. Froeschle ◽  
Z. Knežević ◽  
A. Milani
Keyword(s):  
Perturbation Theory ◽  
Solar System ◽  
Small Body ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Asteroid Belt ◽  
Secular Resonances ◽  
Outer Planets ◽  
Proper Elements ◽  
Solar System Bodies

Generalizing the secular perturbation theory of Milani and Knežević (1990), we have determined in the a — e — I proper elements space the locations of the secular resonances between the precession rates of the longitudes of perihelion and node of a small body and the corresponding eigenfrequencies of the secular perturbations of the four outer planets. We discuss some implications of the results for the dynamical evolution of small solar system bodies. In particular, our findings include: (i) the fact that the g = g6 resonance in the inner asteroid belt lies closer than previously assumed to the Flora region, providing a plausible dynamical route to inject asteroid fragments into planet-crossing orbits; (ii) the possible presence of some low-inclination “stable islands” between the orbits of the outer planets; (iii) the fact that none of the secular resonances considered in this work exists for semimajor axes > 50 AU, so that these resonances do not provide a mechanism for transporting inwards possible Kuiper–belt comets.

Nursery for Planets

2017 ◽  
Author(s):  
John Chambers ◽  
Jacqueline Mitton
Keyword(s):  
Solar System ◽  
Immanuel Kant ◽  
Kuiper Belt ◽  
Planetary Systems ◽  
Protoplanetary Disks ◽  
Young Stars ◽  
Asteroid Belt ◽  
Two Dimensional

This chapter illustrates how the solar system has a decidedly two-dimensional aspect to it. The orbits of the eight major planets all lie in almost the same plane, deviating by no more than seven degrees. Bodies in the asteroid belt and the Kuiper belt stray a little further afield, but these belts are arranged like flattened donuts, aligned with the same plane as the planets. Immanuel Kant and Pierre-Simon de Laplace noted the planar nature of the solar system and used this as the basis for their nebular theories in which the solar system grew out of a flattened disk of matter. Young stars like those in the constellation Orion are often surrounded by disk-shaped clouds of gas and dust. Astronomers quickly dubbed these “protoplanetary” disks, assuming that they will someday form planetary systems.

scholarly journals Finding Asteroid belt Analogues with WISE

2013 ◽  
Vol 8 (S299) ◽  
pp. 352-353
Author(s):  
Rahul I. Patel ◽  
Stanimir Metchev
Keyword(s):  
Main Sequence ◽  
Galactic Plane ◽  
Terrestrial Planet ◽  
Asteroid Belt ◽  
Debris Disks ◽  
Main Sequence Stars ◽  
Sky Survey ◽  
Data Release ◽  
Debris Disk ◽  
Cross Matching

AbstractWe present the detection of stars with infrared (IR) excesses attributed to circumstellar debris disks from the WISE All-Sky Survey at the WISE 12 and 22 μm bandpasses (W3 and W4, respectively). Excess flux at these wavelengths is significant because it traces material in the regions of terrestrial planet formation. We searched for debris disks by cross-matching Hipparcos main sequence stars with the All-Sky Data Release from WISE and seeking excess flux at W3 and W4. Our sample is confined to a volume of 75 pc around the sun, and outside the galactic plane (|b|>5°). Debris disk-bearing stars were identified as 95%-confidence outliers in 2MASS/WISE color distributions, after checking for erroneous photometry and contamination from unrelated nearby objects.

scholarly journals The Possible Belts for Extrasolar Planetary Systems

2004 ◽  
Vol 191 ◽  
pp. 217-221
Author(s):  
Ing-Guey Jiang ◽  
M. Duncan ◽  
D.N.C. Lin
Keyword(s):  
Solar System ◽  
Extrasolar Planets ◽  
Kuiper Belt ◽  
Planetary Systems ◽  
Asteroid Belt ◽  
High Eccentricity ◽  
Kuiper Belt Object ◽  
The Stability

AbstractMore than 100 extrasolar planets have been discovered since the 1990s. Unlike those of the solar system, these planets’ orbital eccentricities cover a huge range from 0 to 0.7. Incidentally, the first Kuiper belt object was discovered in 1992. Thus an interesting and important question will be whether extrasolar planetary systems could have structures like the Kuiper belt or asteroid belt. We investigate the stability of these planetary systems with different orbital eccentricities by similar procedures to Rabl & Dvorak (1988) and Holman & Wiegert (1999). We claim that most extrasolar planetary systems can have their own belts at the outer regions. However, we find that orbits with high eccentricity are very powerful in depletion of these populations.

scholarly journals Enrichment of the HR 8799 planets by minor bodies and dust

2020 ◽  
Author(s):  
Kateryna Frantseva ◽  
Michael Mueller ◽  
Petr Pokorný ◽  
Floris F. S. van der Tak ◽  
Inge Loes ten Kate
Keyword(s):  
Solar System ◽  
Total Mass ◽  
Kuiper Belt ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Refractory Materials ◽  
Exoplanetary Systems ◽  
Main Asteroid Belt ◽  
The Impact ◽  
Shed Light

<p>Are minor bodies and dust delivering volatile and/or refractory materials in exoplanetary systems?<span class="Apple-converted-space"> </span></p> <p>Around ~20% of the nearest stars are found to host analogues of the main asteroid belt and the Kuiper belt. Our aim is to study the possibility of material delivery through minor bodies and dust to the planetary surfaces. To shed light on these delivery processes we extrapolate our Solar System scenarios to the exoplanetary system HR 8799. The system is known to host four giant planets and two belts of minor bodies.</p> <p>We performed a set of N-body simulations to study the impact rates of minor bodies and dust on the HR 8799 planets. We find that the planets suffer impacts by objects from the inner and outer belt. We convert these to volatile and refractory delivery rates using our best estimates of the total mass contained in the belts and their volatile/refractory content. Over their lifetime, the four giant planets receive between 10<sup>-4</sup> and 10<sup>-3 </sup>M<sub>Earth</sub> of material from both belts. This delivery leads to volatile and refractory enrichment of the planets that may be observable. Since the four giants HR 8799 e, d, c, b are located beyond the snow line (and presumably formed there), we expect them to be born volatile-rich. Therefore any future detection of refractories might imply delivery through impacts.</p>

scholarly journals Dynamical Evolution of the Early Solar System

2018 ◽  
Vol 56 (1) ◽  
pp. 137-174 ◽  
Author(s):  
David Nesvorný
Keyword(s):  
Solar System ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Dynamical Instability ◽  
Orbital Energy ◽  
Interstellar Space ◽  
Early Solar System ◽  
Planetary Migration

Several properties of the Solar System, including the wide radial spacing of the giant planets, can be explained if planets radially migrated by exchanging orbital energy and momentum with outer disk planetesimals. Neptune's planetesimal-driven migration, in particular, has a strong advocate in the dynamical structure of the Kuiper belt. A dynamical instability is thought to have occurred during the early stages with Jupiter having close encounters with a Neptune-class planet. As a result of the encounters, Jupiter acquired its current orbital eccentricity and jumped inward by a fraction of an astronomical unit, as required for the survival of the terrestrial planets and from asteroid belt constraints. Planetary encounters also contributed to capture of Jupiter Trojans and irregular satellites of the giant planets. Here we discuss the dynamical evolution of the early Solar System with an eye to determining how models of planetary migration/instability can be constrained from its present architecture. Specifically, we review arguments suggesting that the Solar System may have originally contained a third ice giant on a resonant orbit between Saturn and Uranus. This hypothesized planet was presumably ejected into interstellar space during the instability. The Kuiper belt kernel and other dynamical structures in the trans-Neptunian region may provide evidence for the ejected planet. We favor the early version of the instability where Neptune migrated into the outer planetesimal disk within a few tens of millions of years after the dispersal of the protosolar nebula. If so, the planetary migration/instability was not the cause of the Late Heavy Bombardment. Mercury's orbit may have been excited during the instability.

scholarly journals Organic matter and water from asteroid Itokawa

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Q. H. S. Chan ◽  
A. Stephant ◽  
I. A. Franchi ◽  
X. Zhao ◽  
R. Brunetto ◽  
...  
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Parent Body ◽  
Asteroid Belt ◽  
True Nature ◽  
Water Ice ◽  
Nanocrystalline Graphite ◽  
Terrestrial Water ◽  
Solar System Bodies ◽  
Small Dust

AbstractUnderstanding the true nature of extra-terrestrial water and organic matter that were present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which was the first mission that brought pristine asteroidal materials to Earth’s astromaterial collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD =  + 4868 ± 2288‰; δ15N =  + 344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and offers support for material mixing in the asteroid belt that occurred in scales from small dust infall to catastrophic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modified by D-enriched exogenous organics and water derived from a carbonaceous parent body.

scholarly journals Improved synthesis of SV2A targeting radiotracer [11C]UCB-J

2019 ◽  
Vol 4 (1) ◽  
Author(s):  
Johanna Rokka ◽  
Eva Schlein ◽  
Jonas Eriksson
Keyword(s):  
Methyl Iodide ◽  
Water Solution ◽  
Synthesis Method ◽  
Radiochemical Yield ◽  
Preparative Hplc ◽  
Step Method ◽  
Synaptic Density ◽  
Excellent Starting Point ◽  
Starting Point

Abstract Introduction [11C]UCB-J is a tracer developed for PET (positron emission tomography) that has high affinity towards synaptic vesicle glycoprotein 2A (SV2A), a protein believed to participate in the regulation of neurotransmitter release in neurons and endocrine cells. The localisation of SV2A in the synaptic terminals makes it a viable target for in vivo imaging of synaptic density in the brain. Several SV2A targeting compounds have been evaluated as PET tracers, including [11C]UCB-J, with the aim to facilitate studies of synaptic density in neurological diseases. The original two-step synthesis method failed in our hands to produce sufficient amounts of [11C]UCB-J, but served as an excellent starting point for further optimizations towards a high yielding and simplified one-step method. [11C]Methyl iodide was trapped in a clear THF-water solution containing the trifluoroborate substituted precursor, potassium carbonate and palladium complex. The resulting reaction mixture was heated at 70 °C for 4 min to produce [11C]UCB-J. Results After semi-preparative HPLC purification and reformulation in 10% ethanol/phosphate buffered saline, the product was obtained in 39 ± 5% radiochemical yield based on [11C]methyl iodide, corresponding to 1.8 ± 0.5 GBq at EOS. The radiochemical purity was > 99% and the molar activity was 390 ± 180 GBq/μmol at EOS. The product solution contained < 2 ppb palladium. Conclusions A robust and high yielding production method has been developed for [11C]UCB-J, suitable for both preclinical and clinical PET applications.

Sign in / Sign up

Export Citation Format

Share Document