<i>Hubble Space Telescope</i>Advanced Camera for Surveys Coronagraphic Imaging of the AU Microscopii Debris Disk

Krist, John; Ardila, D. R.; Golimowski, D. A.; Clampin, Mark; Ford, H. C.; Illingworth, G. D.; Hartig, G.; Bartko, F.; Benítez, N.; Blakeslee, John P.; Bouwens, Rychard; Bradley, Larry; Broadhurst, Tom; Brown, Robert A.; Burrows, C. J.; Cheng, E. S.; Cross, N. J. G.; Demarco, R.; Feldman, P. D.; Franx, Marijn; Goto, Tomotsugu; Grönwall, C.; Holden, B.; Homeier, N.; Infante, L.; Kimble, Randy A.; Lesser, Michael P.; Martel, A. R.; Mei, S.; Menanteau, F.; Meurer, G. R.; Miley, G. K.; Motta, V.; Postman, Marc; Rosati, P.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Z.; White, R. L.; Zheng, Wei

doi:10.1086/426755

Cited by 119 publications

(134 citation statements)

References 14 publications

Supporting

Mentioning

112

Contrasting

Order By: Relevance

“…The other relatively well resolved disc is around the β Pic coevol star Au Mic. To some extent, it resembles a scaled-down β Pic, with a roughly flat disc in the inner r < 30 AU region and a H/r ∼ 0.05 beyond that (Krist et al 2005), but no obvious vertical asymmetries or warps. For the two other resolved edge-on systems, HD 15115 and HD 139664, the vertical structure is more poorly constrained because of lower resolution and signal-to-noise ratios.…”

Section: Vertical Structure Of Debris Discsmentioning

confidence: 95%

“…6. Vertical FWHM (=2H) for the AU Mic disc, as derived from observations (Krist et al 2005) and obtained for a test numerical disc initially confined to a narrow annulus at ∼40 AU with e dyn = i dyn = 0. The observed FWHM has been averaged over the two ansae (see Fig.…”

Section: The "Natural" Thickness Of Debris Discsmentioning

confidence: 99%

“…The observed FWHM has been averaged over the two ansae (see Fig. 7 of Krist et al 2005). The synthetic profile has been degraded to the resolution of the scattered light images, i.e., 2 AU.…”

Section: The "Natural" Thickness Of Debris Discsmentioning

confidence: 99%

See 2 more Smart Citations

Vertical structure of debris discs

Thébault

2009

A&A

View full text Add to dashboard Cite

Context. The vertical thickness of debris discs is often used as a measure of these systems' dynamical excitation, and as clues to the presence of hidden massive perturbers such as planetary embryos. However, this argument might be flawed because the observed dust should be naturally placed on inclined orbits by the combined effect of radiation pressure and mutual collisions. Aims. We critically reinvestigate this issue and numerically estimate the "natural" vertical thickness of a collisionally evolving disc, in the absence of any additional perturbing body. Methods. We use a deterministic collisional code, to follow the dynamical evolution of a population of indestructible test grains suffering mutual inelastic impacts. Grain differential sizes as well as the effect of radiation pressure are taken into account. Results. We find that, under the coupled effect of radiation pressure and collisions, grains naturally acquire inclinations of a few degrees. The disc is stratified with respect to grain sizes, the smallest grains having the largest vertical dispersion and the largest being clustered closer to the midplane. Conclusions. Debris discs should have a minimum "natural" observed aspect ratio h min ∼ 0.04 ± 0.02 from visible to mid-IR wavelengths, where the flux is dominated by the smallest bound grains. These values are comparable to the estimated thicknesses of several vertically resolved debris discs, as illustrated by the specific example of AU Mic. For all systems with h ∼ h min , the presence (or absence) of embedded perturbing bodies cannot be inferred from the vertical dispersion of the disc.

show abstract

Section: Vertical Structure Of Debris Discsmentioning

confidence: 95%

Section: The "Natural" Thickness Of Debris Discsmentioning

confidence: 99%

See 1 more Smart Citation

Vertical structure of debris discs

Thébault

2009

A&A

View full text Add to dashboard Cite

show abstract

“…Currently, among the nearby M-stars, the only spatially resolved debris disk is around the very young M1 star AU Mic Liu et al 2004;Krist et al 2005;Wilner et al 2012) which has been modeled by Augereau & Beust (2006) and Strubbe & Chiang (2006). In addition, there are a few candidate disks with excesses above photospheric level (e.g.…”

Section: ) and Containmentioning

confidence: 99%

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Lestrade

Matthews

Sibthorpe

et al. 2012

A&A

View full text Add to dashboard Cite

Debris disks have been found primarily around intermediate and solar mass stars (spectral types A-K) but rarely around low mass M-type stars. We have spatially resolved a debris disk around the remarkable M3-type star GJ 581 hosting multiple planets using deep PACS images at 70, 100 and 160 μm as part of the DEBRIS Program on the Herschel Space Observatory. This is the second spatially resolved debris disk found around an M-type star, after the one surrounding the young star AU Mic (12 Myr). However, GJ 581 is much older (2-8 Gyr), and is X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images and found that the best fit model is for a disk extending radially from 25 ± 12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper belt but it surrounds a low mass star (0.3 M ) and its fractional dust luminosity L dust /L * of ∼10 −4 is much higher. The inclination limits of the disk found in our analysis make the masses of the planets small enough to ensure the long-term stability of the system according to some dynamical simulations. The disk is collisionally dominated down to submicron-sized grains and the dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. We suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars. Finally, the known planets, of low masses and orbiting within 0.3 AU from the star, cannot dynamically perturb the disk over the age of the star, suggesting that an additional planet exists at larger distance that is stirring the disk to replenish the dust.

show abstract

“…In the following, a geometrically thick disk with a Gaussian vertical dust distribution and a scale height H(r) = 0.47 r 50 AU + 0.34 AU is used (for AU Mic cf. Metchev et al 2005;Krist et al 2005). The density ρ of the disk is given by…”

Section: Geometrically Thick Disksmentioning

confidence: 99%

Detecting circumstellar disks around gravitational microlenses

Hundertmark

Hessman

2009

A&A

View full text Add to dashboard Cite

Aims. We investigate the chance of detecting proto-planetary or debris disks in stars that induce microlensing event (lenses), and consider the modification of the light curve shapes due to occultation and extinction by the disks, as well as the gravitational deflection caused by the additional mass. Methods. The magnification of gravitational microlensing events is calculated using the ray shooting method. The occultation is taken into account by neglecting or weighting the images on the lens plane according to a transmission map of the corresponding disk for a point source point lens (PSPL) model. The estimated frequency of events is obtained by considering the possible inclinations and optical depths of the disk. Results. We conclude that gravitational microlensing can be used, in principle, as a tool for detecting debris disks beyond 1 kpc, but estimate that each year around 1 debris disk is expected for lens stars of F, G, or K spectral type and about 10 debris disks might have shown signatures in existing datasets.

show abstract

Hubble Space TelescopeAdvanced Camera for Surveys Coronagraphic Imaging of the AU Microscopii Debris Disk

Abstract: We present Hubble Space Telescope Advanced Camera for Surveys multicolor coronagraphic images of the recently discovered edge-on debris disk around the nearby (∼ 10 pc) M dwarf AU Microscopii. The disk is seen between r =0. ′′ 75 -

Cited by 119 publications

References 14 publications

Vertical structure of debris discs

Vertical structure of debris discs

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Detecting circumstellar disks around gravitational microlenses

Contact Info

Product

Resources

About