Model of a Kuiper Belt Small Grain Population and Resulting Far-Infrared Emission

Backman, D. E.; Dasgupta, Amil; Stencel, R. E.

doi:10.1086/309660

Cited by 106 publications

(123 citation statements)

References 20 publications

Supporting

Mentioning

117

Contrasting

Order By: Relevance

“…Table 3 is only available in electronic form at http://www.aanda.org continuously replenished by collisions of larger bodies (see e.g. Backman et al 1995). Deeper and more targeted observations by the Infrared Space Observatory (ISO), Spitzer, and AKARI have revised and extended this list of debris disk candidates to encompass over 200 stars Rhee et al 2007; UK ATC Debris Disk Database 2009).…”

Section: Introductionmentioning

confidence: 99%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid-and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. Aims. The β Pictoris moving group is a nearby stellar association of young (∼12 Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. Methods. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870 μm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. Results. From our sample, β Pic, HD 181327, and HD 172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. Conclusions. We find a mean fractional dust luminosityf dust = 1.1 × 10 −3 at t ≈ 12 Myr, which together with recent data at 100 Myr suggests an f dust ∝ t −α decline of the emitting dust, with α > 0.8.

show abstract

Section: Introductionmentioning

confidence: 99%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…However, we cannot rule out the existence of EKO particles since EKO can produce many ejecta particles in the EKO region (e.g. Backman et al, 1995;Stern, 1996) and about 20% of micron-sized particles can avoid gravitational scattering by outer planets in their orbital evolution (Liou et al, 1996) To be consistent with the Galileo/Ulysses results, the real contribution of EKO dust will be smaller than that in Fig. 5.…”

Section: Contribution Of Each Dust Groupmentioning

confidence: 75%

“…5, an additional group of dust particles from Edgeworth-Kuiper belt objects has been applied as a possible dust source outside 5 AU. The number density distribution of EKO particles has been estimated by using a similar calculation to that described in the previous section, assuming the radial distribution of EKOs from Backman et al (1995) and the factor of interstellar flux C = 1.0 outside 5 AU. Also, the number density of EKO particles in 10 −12 g ≤ m ≤ 10 −9 g is set to be comparable with that of the IMF model.…”

Section: Contribution Of Each Dust Groupmentioning

confidence: 99%

See 1 more Smart Citation

Collisional evolution and the resulting mass distribution of interplanetary dust

Ishimoto

2014

Earth Planet Sp

View full text Add to dashboard Cite

On the basis of numerical approaches for the collisional and orbital evolution of dust particles, the number density distribution of interplanetary dust with the mass range of m ≥ 10 −12 g is investigated. The slope of the mass distribution of dust particles strongly depends on the radial dependence of dust production by their parent bodies, and the collisional interaction between particles. Specifically, the m −7/3 dependence of the number density distribution at 1 AU for m ≥ 10 −6 g can be explained through the balance between the collisional loss of particles and the dust supply, whereas the m −4/3 dependence for 10 −12 g ≤ m ≤ 10 −6 g particles is derived from simple PoyntingRobertson orbital decay. A possible model of the dust populations of asteroidal, cometary, and Edgeworth-Kuiper belt origin that is consistent with the observed dust flux at a solar distance of 1 AU is presented.

show abstract

“…We set n = 1 as in the formal factor in Mie scattering in the following; see, e.g., Spitzer (1978), Greenberg (1978), and Backman et al (1995). This gives the temperature of objects at the Edgeworth-Kuiper Belt distance as in Figure 1, showing that for emission in WMAP frequencies this suppression causes some effects only for a < 50 μm, the emission from which is unimportant for the parameters that concern us; hence, the results hardly depend on the suppression factor assumed for a wide variety of its choice.…”

Section: Size Distribution and Thermal Radiation From Grainsmentioning

confidence: 99%

MICROWAVE EMISSION FROM THE EDGEWORTH-KUIPER BELT AND THE ASTEROID BELT CONSTRAINED FROM THEWILKINSON MICROWAVE ANISOTROPY PROBE

Ichikawa¹,

Fukugita²

2011

ApJ

View full text Add to dashboard Cite

Objects in the Edgeworth-Kuiper Belt and the main asteroid belt should emit microwaves that may give rise to extra anisotropy signals in the multipole of the cosmic microwave background (CMB) experiment. Constraints are derived from the absence of positive detection of such anisotropies for 50, meaning the total mass of Edgeworth-Kuiper Belt objects is smaller than 0.2 M ⊕ . This limit is consistent with the mass extrapolated from the observable population with the size of a 15 km, assuming that the small-object population follows the power law in size dN/da ∼ a −q with the canonical index expected for collisional equilibrium, q 3.5, with which 23% of the mass is ascribed to objects smaller than are observationally accessible down to grains. A similar argument applied to the main asteroid belt indicates that the grain population should not increase more quickly than q 3.6 toward smaller radii, if the grain population follows the power law that continues to observed asteroids with larger radii. Both cases are at or only slightly above the limit that can be physically significant, implying the importance of further tightening the CMB anisotropy limit, which may be attained with observation at higher radio frequencies.

show abstract

Model of a Kuiper Belt Small Grain Population and Resulting Far-Infrared Emission

Cited by 106 publications

References 20 publications

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Collisional evolution and the resulting mass distribution of interplanetary dust

MICROWAVE EMISSION FROM THE EDGEWORTH-KUIPER BELT AND THE ASTEROID BELT CONSTRAINED FROM THEWILKINSON MICROWAVE ANISOTROPY PROBE

Contact Info

Product

Resources

About