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 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 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.

scholarly journals Comprehensive Census and Complete Characterization of Nearby Debris Disk Stars

2015 ◽  
Vol 10 (S314) ◽  
pp. 179-182
Author(s):  
Tara H. Cotten ◽  
Inseok Song
Keyword(s):  
Large Scale ◽  
Complete Characterization ◽  
High Resolution Spectroscopy ◽  
Debris Disks ◽  
Infrared Excess ◽  
History Of ◽  
Debris Disk ◽  
Host Stars ◽  
Comprehensive Study

AbstractDebris disks are intimately linked to planetary system evolution since the rocky material surrounding the host stars is believed to be due to secondary generation from the collisions of planetesimals. With the conclusion and lack of future large scale infrared excess survey missions, it is time to summarize the history of using excess emission in the infrared as a tracer of debris and exploit all available data as well as provide a comprehensive study of the parameters of these important objects. We have compiled a catalog of infrared excess stars from peer-reviewed articles and performed an extensive search for new debris disks by cross-correlating the Tycho-2 and AllWISE catalogs. This study will conclude following the thorough examination of each debris disk star's parameters obtained through high-resolution spectroscopy at various facilities which is currently ongoing. We will maintain a webpage (www.debrisdisks.org) devoted to these infrared excess sources and provide various resources related to our catalog creation, SED fitting, and data reduction.

scholarly journals Constraining the detectability of water ice in debris disks

2019 ◽  
Vol 629 ◽  
pp. A141
Author(s):  
M. Kim ◽  
S. Wolf ◽  
A. Potapov ◽  
H. Mutschke ◽  
C. Jäger
Keyword(s):  
Scattered Light ◽  
Spectral Energy ◽  
Debris Disks ◽  
Water Ice ◽  
Spatially Resolved ◽  
Infrared Telescope ◽  
Effective Medium Theories ◽  
Debris Disk ◽  
Highly Porous ◽  
Entire Planet

Context. Water ice is important for the evolution and preservation of life. Identifying the distribution of water ice in debris disks is therefore of great interest in the field of astrobiology. Furthermore, icy dust grains are expected to play important roles throughout the entire planet formation process. However, currently available observations only allow deriving weak conclusions about the existence of water ice in debris disks. Aims. We investigate whether it is feasible to detect water ice in typical debris disk systems. We take the following ice destruction mechanisms into account: sublimation of ice, dust production through planetesimal collisions, and photosputtering by UV-bright central stars. We consider icy dust mixture particles with various shapes consisting of amorphous ice, crystalline ice, astrosilicate, and vacuum inclusions (i.e., porous ice grains). Methods. We calculated optical properties of inhomogeneous icy dust mixtures using effective medium theories, that is, Maxwell-Garnett rules. Subsequently, we generated synthetic debris disk observables, such as spectral energy distributions and spatially resolved thermal reemission and scattered light intensity and polarization maps with our code DMS. Results. We find that the prominent ~3 and 44 μm water ice features can be potentially detected in future observations of debris disks with the James Webb Space Telescope (JWST) and the Space Infrared telescope for Cosmology and Astrophysics (SPICA). We show that the sublimation of ice, collisions between planetesimals, and photosputtering caused by UV sources clearly affect the observational appearance of debris disk systems. In addition, highly porous ice (or ice-rich aggregates) tends to produce highly polarized radiation at around 3 μm. Finally, the location of the ice survival line is determined by various dust properties such as a fractional ratio of ice versus dust, physical states of ice (amorphous or crystalline), and the porosity of icy grains.

scholarly journals A Model of Stochastic Collisions as the Cause of Clumps in Debris Disks

2004 ◽  
Vol 202 ◽  
pp. 399-401
Author(s):  
M. C. Wyatt ◽  
W. R. F. Dent ◽  
J. S. Greaves ◽  
W. S. Holland
Keyword(s):  
Simple Model ◽  
Debris Disks ◽  
Heuristic Model ◽  
Detailed Model ◽  
Debris Disk ◽  
Collisional Evolution

We present a heuristic model for the collisional evolution of material in a debris disk. This is used to consider the probability that the 2-3% brightness clump observed in the sub-mm Fomalhaut disk is caused by stochastic collisions between large planetesimals. While this simple model finds that the probability that the clump is caused by collisions is low (about 1 in 80,000), a more detailed model is required to ascertain its true likelihood.

scholarly journals Debris Disks and Multiplicity within the 75pc Volume-limited A-Star (VAST) Survey

2013 ◽  
Vol 8 (S299) ◽  
pp. 334-335
Author(s):  
R. J. De Rosa ◽  
B. Smith ◽  
J. Bulger ◽  
J. Patience ◽  
C. Marois ◽  
...  
Keyword(s):  
Future Study ◽  
Large Scale ◽  
Binary Systems ◽  
Debris Disks ◽  
Companion Star ◽  
Large Sample ◽  
Planetary Mass ◽  
Debris Disk

AbstractWe present the preliminary findings of an investigation of the multiplicity of debris disk stars identified within our Volume-limited A-star (VAST) multiplicity survey. Previous studies have produced conflicting results regarding the multiplicity fraction of debris disk-hosting stars compared with non-excess stars. By combining our large-scale volume-limited AO survey of A-type stars with the all-sky WISE catalogue, we have investigated the frequency of binary companions to a large sample of A-type stars with and without measured 22μm excess. The results of this study will allow for a greater understanding of the interaction between a companion star and a circumstellar debris disk, informing future study into the formation and stability of planetary-mass companions within binary systems.

scholarly journals Warm Debris Disks with WISE and HST

2015 ◽  
Vol 10 (S314) ◽  
pp. 175-178 ◽  
Author(s):  
Deborah Padgett ◽  
Karl Stapelfeldt
Keyword(s):  
Scattered Light ◽  
Terrestrial Planets ◽  
Wide Field ◽  
Debris Disks ◽  
Circumstellar Material ◽  
Excess Emission ◽  
Sky Survey ◽  
Debris Disk ◽  
Infrared Survey

AbstractUsing 22 μm data from the Wide Field Infrared Survey Explorer (WISE), we have completed a sensitive all-sky survey for debris disks in Hipparcos and Tycho catalog stars within 120 pc. This warm excess emission traces material in the circumstellar region likely to host terrestrial planets. Several hundred previously unknown debris disk candidates were identified. We are currently performing follow-up observations to characterize the stars, companions, and circumstellar material in these systems with a variety of facilities including Keck, Herschel, and HST. Thirteen WISE debris disks have been observed to date using HST/STIS coronagraphy. Five of these disks have been detected in scattered light. One is a large and highly asymmetric edge-on disk which appears to be both warped and bifurcated.

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 Fraction for M-dwarfs in Nearby Young Moving Groups

2015 ◽  
Vol 10 (S314) ◽  
pp. 159-162 ◽  
Author(s):  
Alex Binks
Keyword(s):  
Stellar Wind ◽  
Rapid Decline ◽  
Debris Disks ◽  
M Dwarfs ◽  
Disk Structure ◽  
Debris Disk ◽  
The Absolute ◽  
Moving Groups ◽  
M Dwarf

AbstractI present the first substantial work to measure the fraction of debris disks for M-dwarfs in nearby moving groups (MGs). Utilising the AllWISE IR catalog, 17 out of 151 MG members are found with an IR photometric excess indicative of disk structure. The M-dwarf debris disk fraction is ≲6 per cent in MGs younger than 40 Myr, and none are found in the groups older than 40 Myr. Simulations show, however, that debris disks around M-dwarfs are not present above a WISEW1-W4 colour of ~2.5, making calculating the absolute disk fractions difficult. The debris disk dissipation timescale appears to be faster than for higher-mass stars, and mechanisms such as enhanced stellar wind drag and/or photoevaporation could account for the more rapid decline of disks observed amongst M-dwarfs.

scholarly journals HD141569A: Disk Dissipation Caught in Action

2015 ◽  
Vol 10 (S314) ◽  
pp. 201-202 ◽  
Author(s):  
J. Péricaud ◽  
E. Di Folco ◽  
A. Dutrey ◽  
J.-C. Augereau ◽  
V. Piétu ◽  
...  
Keyword(s):  
Scattered Light ◽  
Dust Emission ◽  
Debris Disks ◽  
Debris Disk ◽  
Multiple Rings

AbstractDebris disks are usually thought to be gas-poor, the gas being dissipated by accretion or evaporation during the protoplanetary phase. HD141569A is a 5 Myr old star harboring a famous debris disk, with multiple rings and spiral features. I present here the first PdBI maps of the 12CO(2−1), 13CO(2−1) gas and dust emission at 1.3 mm in this disk. The analysis reveals there is still a large amount of (primordial) gas extending out to 250 AU, i.e. inside the rings observed in scattered light. HD141569A is thus a hybrid disk with a huge debris component, where dust has evolved and is produced by collisions, with a large remnant reservoir of gas.

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