50 research outputs found
On the Solar System-Debris Disk Connecction
This 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.Comment: 8 pages, Exoplanets: Detection, Formation and Dynamics Proceedings
IAU Symposium No. 249 200
A Study of the Dynamics of Dust from the Kuiper Belt: Spatial Distribution and Spectral Energy Distribution
The dust produced in the Kuiper Belt (KB) spreads throughout the Solar System
forming a dust disk. We numerically model the orbital evolution of KB dust and
estimate its equilibrium spatial distribution and its brightness and spectral
energy distributions (SED), assuming greybody absorption and emission by the
dust grains. We show that the planets modify the KB disk SED, so potentially we
can infer the presence of planets in spatially unresolved debris disks by
studying the shape of their SEDs. We point out that there are inherent
uncertainties in the prediction of structure in the dust disk, owing to the
chaotic dynamics of dust orbital evolution imposed by resonant gravitational
perturbations of the planets.Comment: 19 pages, 14 figures in jpg, accepted to A
Locating Planetesimal Belts in the Multiple-planet Systems HD 128311, HD 202206, HD 82943, and HR 8799
In addition to the Sun, six other stars are known to harbor multiple planets and debris disks: HD 69830, HD 38529, HD 128311, HD 202206, HD 82943, and HR 8799. In this paper, we set constraints on the location of the dust-producing planetesimals around the latter four systems. We use a radiative transfer model to analyze the spectral energy distributions of the dust disks (including two new Spitzer IRS spectra presented in this paper), and a dynamical model to assess the long-term stability of the planetesimals' orbits. As members of a small group of stars that show evidence of harboring a multiple planets and planetesimals, their study can help us learn about the diversity of planetary systems
A Molecular Counterpart to the Herbig-Haro 1-2 Flow
We present high angular resolution (12"-24") and high sensitivity 12CO and
13CO J=2-1 and J=1-0 observations of the HH 1-2 outflow. The observations show
the molecular counterpart, moving with a velocity of approx. 30 km/s, of the
optical bipolar system driven by the VLA 1 embedded source. Along the optical
jet there are certain regions where the molecular gas reaches deprojected
velocities of 100-200 km/s, and that we interpret as the molecular jet. The
bipolar CO outflow has a length of approx. 260" with a curved morphology
towards the North where it extends beyond the HH 1 object (approx. 120") .
Two new molecular outflows have been detected, one arising from IRAS
05339-0647 which excites the HH 147 optical flow and another powered by VLA 2
which drives the HH 144 optical outflow. The molecular outflow driven by the
VLA 3 source is also clearly detected and spatially resolved from the VLA 1
main outflow.Comment: 14 pages, 4 figures, accepted ApJLet
The debris disk - terrestrial planet connection
The eccentric orbits of the known extrasolar giant planets provide evidence
that most planet-forming environments undergo violent dynamical instabilities.
Here, we numerically simulate the impact of giant planet instabilities on
planetary systems as a whole. We find that populations of inner rocky and outer
icy bodies are both shaped by the giant planet dynamics and are naturally
correlated. Strong instabilities -- those with very eccentric surviving giant
planets -- completely clear out their inner and outer regions. In contrast,
systems with stable or low-mass giant planets form terrestrial planets in their
inner regions and outer icy bodies produce dust that is observable as debris
disks at mid-infrared wavelengths. Fifteen to twenty percent of old stars are
observed to have bright debris disks (at wavelengths of ~70 microns) and we
predict that these signpost dynamically calm environments that should contain
terrestrial planets.Comment: Contribution to proceedings of IAU 276: Astrophysics of Planetary
System