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 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.

scholarly journals The Debris Disk Explorer: a balloon-borne coronagraph for observing debris disks

2013 ◽  
Author(s):  
Lewis C. Roberts ◽  
Geoffrey Bryden ◽  
Wesley Traub ◽  
Stephen Unwin ◽  
John Trauger ◽  
...  
Keyword(s):  
Debris Disks ◽  
Debris Disk

scholarly journals Planet forming disks, debris disks and the Solar System

2019 ◽  
Vol 15 (S350) ◽  
pp. 207-215
Author(s):  
Inga Kamp
Keyword(s):  
Chemical Composition ◽  
Solar System ◽  
Planetary Systems ◽  
Theoretical Work ◽  
Structure Evolution ◽  
Debris Disks ◽  
Physical Processes ◽  
Disk Structure ◽  
Open Questions ◽  
Evolution Modeling

AbstractVLT instruments and ALMA with their high spatial resolution have revolutionized in the past five years our view and understanding of how disks turn into planetary systems. This talk will briefly outline our current understanding of the physical processes occurring and chemical composition evolving as these disks turn into debris disks and eventually planetary systems like our own solar system. I will especially focus on the synergy between disk structure/evolution modeling and astrochemical laboratory/theoretical work to highlight the most recent advances, and open questions such as (1) how much of the chemical composition in disks is inherited from molecular clouds, (2) the relevance of snowlines for planet formation, and (3) what is the origin of the gas in debris disks and what can we learn from it. For each of the three, I will outline briefly how the combination of theory/lab astrochemistry, astrophysical models and observations are required to advance our understanding.

scholarly journals Upper limits on the water vapour content of the β Pictoris debris disk

2019 ◽  
Vol 628 ◽  
pp. A127 ◽  
Author(s):  
M. Cavallius ◽  
G. Cataldi ◽  
A. Brandeker ◽  
G. Olofsson ◽  
B. Larsson ◽  
...  
Keyword(s):  
Solar System ◽  
Far Infrared ◽  
Kinetic Temperature ◽  
Line Flux ◽  
Water Vapour Content ◽  
Water Ice ◽  
Upper Limit ◽  
Upper Limits ◽  
Debris Disk ◽  
Lower Limits

Context. The debris disk surrounding β Pictoris has been observed with ALMA to contain a belt of CO gas with a distinct peak at ~85 au. This CO clump is thought to be the result of a region of enhanced density of solids that collide and release CO through vaporisation. The parent bodies are thought to be comparable to solar system comets, in which CO is trapped inside a water ice matrix. Aims. Since H2O should be released along with CO, we aim to put an upper limit on the H2O gas mass in the disk of β Pictoris. Methods. We used archival data from the Heterodyne Instrument for the Far-Infrared (HIFI) aboard the Herschel Space Observatory to study the ortho-H2O 110–101 emission line. The line is undetected. Using a python implementation of the radiative transfer code RADEX, we converted upper limits on the line flux to H2O gas masses. The resulting lower limits on the CO/H2O mass ratio are compared to the composition of solar system comets. Results. Depending on the assumed gas spatial distribution, we find a 95% upper limit on the ortho-H2O line flux of 7.5 × 10−20 W m−2 or 1.2 × 10−19 W m−2. These translate into an upper limit on the H2O mass of 7.4 × 1016–1.1 × 1018 kg depending on both the electron density and gas kinetic temperature. The range of derived gas-phase CO/H2O ratios is marginally consistent with low-ratio solar system comets.

scholarly journals SEARCHING FOR GAS GIANT PLANETS ON SOLAR SYSTEM SCALES: VLT NACO/APP OBSERVATIONS OF THE DEBRIS DISK HOST STARS HD172555 AND HD115892

2011 ◽  
Vol 736 (2) ◽  
pp. L32 ◽  
Author(s):  
Sascha P. Quanz ◽  
Matthew A. Kenworthy ◽  
Michael R. Meyer ◽  
Julien H. V. Girard ◽  
Markus Kasper
Keyword(s):  
Solar System ◽  
Giant Planets ◽  
Debris Disk ◽  
Gas Giant ◽  
Host Stars

scholarly journals Characterizing planetesimal belts through the study of debris dust

2010 ◽  
Vol 6 (S276) ◽  
pp. 54-59
Author(s):  
Amaya Moro-Martín
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Planetary Systems ◽  
Dust Particles ◽  
Debris Disks ◽  
Main Sequence Stars ◽  
Wide Range ◽  
Robust Process

AbstractMain sequence stars are commonly surrounded by disks of dust. From lifetime arguments, it is inferred that the dust particles are not primordial but originate from the collision of planetesimals, similar to the asteroids, comets and KBOs in our Solar system. The presence of these debris disks around stars with a wide range of masses, luminosities, and metallicities, with and without binary companions, is evidence that planetesimal formation is a robust process that can take place under a wide range of conditions. Debris disks can help us learn about the formation, evolution and diversity of planetary systems.

scholarly journals SOLAR SYSTEM ANALOGS AROUNDIRAS-DISCOVERED DEBRIS DISKS

2009 ◽  
Vol 701 (2) ◽  
pp. 1367-1372 ◽  
Author(s):  
Christine H. Chen ◽  
Patrick Sheehan ◽  
Dan M. Watson ◽  
P. Manoj ◽  
Joan R. Najita
Keyword(s):  
Solar System ◽  
Debris Disks

scholarly journals Inclination Excitation of Solar System Debris Disk Due to Stellar Flybys

2020 ◽  
Vol 901 (2) ◽  
pp. 92
Author(s):  
Nathaniel W. H. Moore ◽  
Gongjie Li ◽  
Fred C. Adams
Keyword(s):  
Solar System ◽  
Debris Disk

scholarly journals ACS Coronagraphic Observations of Optically Thin Debris Disks

2004 ◽  
Vol 221 ◽  
pp. 449-457
Author(s):  
Mark Clampin ◽  
John Krist ◽  
David R. Ardila ◽  
David A. Golimowski ◽  
Holland C. Ford ◽  
...  
Keyword(s):  
Angular Resolution ◽  
Debris Disks ◽  
Reference Star ◽  
Point Spread Functions ◽  
Point Spread ◽  
Imaging Mode ◽  
Debris Disk ◽  
Advanced Camera For Surveys

The Advanced Camera for Surveys (ACS) offers a coronagraphic imaging mode with angular resolution of 0.026″pixel−1. In combination with with the appropriate subtraction of reference star point spread functions (PSF) the coronagraph is capable of achieving contrast ratios of ∼1000. We present some of the first ACS observations of the optically thin debris disk HD141569A and discuss new results from these observations.

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