127 research outputs found
Collisional modelling of the debris disc around HIP 17439
We present an analysis of the debris disc around the nearby K2 V star HIP
17439. In the context of the Herschel DUNES key programme the disc was observed
and spatially resolved in the far-IR with the Herschel PACS and SPIRE
instruments. In a first model, Ertel et al. (2014) assumed the size and radial
distribution of the circumstellar dust to be independent power laws. There, by
exploring a very broad range of possible model parameters several scenarios
capable of explaining the observations were suggested. In this paper, we
perform a follow-up in-depth collisional modelling of these scenarios trying to
further distinguish between them. In our models we consider collisions, direct
radiation pressure, and drag forces, i.e. the actual physical processes
operating in debris discs. We find that all scenarios discussed in Ertel et al.
are physically sensible and can reproduce the observed SED along with the PACS
surface brightness profiles reasonably well. In one model, the dust is produced
beyond 120au in a narrow planetesimal belt and is transported inwards by
Poynting-Robertson and stellar wind drag. A good agreement with the observed
radial profiles would require stellar winds by about an order of magnitude
stronger than the solar value, which is not supported, although not ruled out,
by observations. Another model consists of two spatially separated planetesimal
belts, a warm inner and a cold outer one. This scenario would probably imply
the presence of planets clearing the gap between the two components. Finally,
we show qualitatively that the observations can be explained by assuming the
dust is produced in a single, but broad planetesimal disc with a surface
density of solids rising outwards, as expected for an extended disc that
experiences a natural inside-out collisional depletion. Prospects of
discriminating between the competing scenarios by future observations are
discussed.Comment: Astronomy and Astrophysics (accepted for publication). 11 pages, 8
figure
Collisional modelling of the AU Microscopii debris disc
The spatially resolved AU Mic debris disc is among the most famous and
best-studied debris discs. We aim at a comprehensive understanding of the dust
production and the dynamics of the disc objects with in depth collisional
modelling including stellar radiative and corpuscular forces. Our models are
compared to a suite of observational data for thermal and scattered light
emission, ranging from the ALMA radial surface brightness profile at 1.3mm to
polarisation measurements in the visible. Most of the data can be reproduced
with a planetesimal belt having an outer edge at around 40au and subsequent
inward transport of dust by stellar winds. A low dynamical excitation of the
planetesimals with eccentricities up to 0.03 is preferred. The radial width of
the planetesimal belt cannot be constrained tightly. Belts that are 5au and
17au wide, as well as a broad 44au-wide belt are consistent with observations.
All models show surface density profiles increasing with distance from the star
as inferred from observations. The best model is achieved by assuming a stellar
mass loss rate that exceeds the solar one by a factor of 50. While the SED and
the shape of the ALMA profile are well reproduced, the models deviate from the
scattered light data more strongly. The observations show a bluer disc colour
and a lower degree of polarisation for projected distances <40au than predicted
by the models. The problem may be mitigated by irregularly-shaped dust grains
which have scattering properties different from the Mie spheres used. From
tests with a handful of selected dust materials, we derive a preference for
mixtures of silicate, carbon, and ice of moderate porosity. We address the
origin of the unresolved central excess emission detected by ALMA and show that
it cannot stem from an additional inner belt alone. Instead, it should derive,
at least partly, from the chromosphere of the central star.Comment: Astronomy and Astrophysics (accepted for publication), 18 pages, 11
figure
The cold origin of the warm dust around epsilon Eridani
Context: The K2V star eps Eri hosts one known inner planet, an outer Kuiper
belt analog, and an inner disk of warm dust. Spitzer/IRS measurements indicate
that the warm dust is present at distances as close as a few AU from the star.
Its origin is puzzling, since an "asteroid belt" that could produce this dust
would be unstable because of the known inner planet. Aims: Here we test the
hypothesis that the observed warm dust is generated by collisions in the outer
belt and is transported inward by Poynting-Robertson (P-R) drag and strong
stellar winds. Methods: We simulated a steady-state distribution of dust
particles outside 10AU with a collisional code and in the inner region (r<10AU)
with single-particle numerical integrations. By assuming homogeneous spherical
dust grains composed of water ice and silicate, we calculated the thermal
emission of the dust and compared it with observations. We investigated two
different orbital configurations for the inner planet inferred from RV
measurements, one with a highly eccentric orbit of e=0.7 and another one with a
moderate one of e=0.25. We also produced a simulation without a planet.
Results: Our models can reproduce the shape and magnitude of the observed SED
from mid-IR to sub-mm wavelengths, as well as the Spitzer/MIPS radial
brightness profiles. The best-fit dust composition includes both ice and
silicates. The results are similar for the two possible planetary orbits and
without a planet. Conclusions: The observed warm dust in the system can indeed
stem from the outer belt and be transported inward by P-R and stellar wind
drag. The inner planet has little effect on the distribution of dust, so that
the planetary orbit could not be constrained. Reasonable agreement between the
model and observations can only be achieved by relaxing the assumption of
purely silicate dust and assuming a mixture of silicate and ice in comparable
amounts.Comment: 9 pages, 9 figures, abstract abridge
Scalar Representation and Conjugation of Set-Valued Functions
To a function with values in the power set of a pre-ordered, separated
locally convex space a family of scalarizations is given which completely
characterizes the original function. A concept of a Legendre-Fenchel conjugate
for set-valued functions is introduced and identified with the conjugates of
the scalarizations. Using this conjugate, weak and strong duality results are
proven.Comment: arXiv admin note: substantial text overlap with arXiv:1012.435
<i>Herschel</i> observations of the debris disc around HIP 92043
Context. Typical debris discs are composed of particles ranging from several micron sized dust grains to km sized asteroidal bodies, and their infrared emission peaks at wavelengths 60-100 μm. Recent Herschel DUNES observations have identified several debris discs around nearby Sun-like stars (F, G and K spectral type) with significant excess emission only at 160 μm.
Aims. We observed HIP 92043 (110 Her, HD 173667) at far-infrared and sub-millimetre wavelengths with Herschel PACS and SPIRE. Identification of the presence of excess emission from HIP 92043 and the origin and physical properties of any excess was undertaken through analysis of its spectral energy distribution (SED) and the PACS images.
Methods. The PACS and SPIRE images were produced using the HIPE photProject map maker routine. Fluxes were measured using aperture photometry. A stellar photosphere model was scaled to optical and near infrared photometry and subtracted from the far-infared and sub-mm fluxes to determine the presence of excess emission. Source radial profiles were fitted using a 2D Gaussian and compared to a PSF model based on Herschel observations of α Boo to check for extended emission.
Results. Clear excess emission from HIP 92043 was observed at 70 and 100 μm. Marginal excess was observed at 160 and 250 μm. Analysis of the images reveals that the source is extended at 160 μm. A fit to the source SED is inconsistent with a photosphere and single temperature black body.
Conclusions. The excess emission from HIP 92043 is consistent with the presence of an unresolved circumstellar debris disc at 70 and 100 μm, with low probability of background contamination. The extended 160 μm emission may be interpreted as an additional cold component to the debris disc or as the result of background contamination along the line of sight. The nature of the 160 μm excess cannot be determined absolutely from the available data, but we favour a debris disc interpretation, drawing parallels with previously identified cold disc sources in the DUNES sample
Forming the first planetary systems: debris around Galactic thick disc stars
The thick disc contains stars formed within the first Gyr of Galactic
history, and little is known about their planetary systems. The Spitzer MIPS
instrument was used to search 11 of the closest of these old low-metal stars
for circumstellar debris, as a signpost that bodies at least as large as
planetesimals were formed. A total of 22 thick disc stars has now been
observed, after including archival data, but dust is not found in any of the
systems. The data rule out a high incidence of debris among star systems from
early in the Galaxy's formation. However, some stars of this very old
population do host giant planets, at possibly more than the general incidence
among low-metal Sun-like stars. As the Solar System contains gas giants but
little cometary dust, the thick disc could host analogue systems that formed
many Gyr before the Sun.Comment: accepted by MNRAS Letters; 5 pages, 4 figure
Lagrange Duality in Set Optimization
Based on the complete-lattice approach, a new Lagrangian duality theory for
set-valued optimization problems is presented. In contrast to previous
approaches, set-valued versions for the known scalar formulas involving infimum
and supremum are obtained. In particular, a strong duality theorem, which
includes the existence of the dual solution, is given under very weak
assumptions: The ordering cone may have an empty interior or may not be
pointed. "Saddle sets" replace the usual notion of saddle points for the
Lagrangian, and this concept is proven to be sufficient to show the equivalence
between the existence of primal/dual solutions and strong duality on the one
hand and the existence of a saddle set for the Lagrangian on the other hand
A peculiar class of debris disks from Herschel/DUNES - A steep fall off in the far infrared
Aims. We present photometric data of debris disks around HIP 103389 (HD
199260), HIP 107350 (HN Peg, HD206860), and HIP 114948 (HD 219482), obtained in
the context of our Herschel Open Time Key Program DUNES (DUst around NEarby
Stars). Methods. We used Herschel/PACS to detect the thermal emission of the
three debris disks with a 3 sigma sensitivity of a few mJy at 100 um and 160
um. In addition, we obtained Herschel/PACS photometric data at 70 um for HIP
103389. Two different approaches are applied to reduce the Herschel data to
investigate the impact of data reduction on the photometry. We fit analytical
models to the available spectral energy distribution (SED) data. Results. The
SEDs of the three disks potentially exhibit an unusually steep decrease at
wavelengths > 70 um. We investigate the significance of the peculiar shape of
these SEDs and the impact on models of the disks provided it is real. Our
modeling reveals that such a steep decrease of the SEDs in the long wavelength
regime is inconsistent with a power-law exponent of the grain size distribution
-3.5 expected from a standard equilibrium collisional cascade. In contrast, a
very distinct range of grain sizes is implied to dominate the thermal emission
of such disks. However, we demonstrate that the understanding of the data of
faint sources obtained with Herschel is still incomplete and that the
significance of our results depends on the version of the data reduction
pipeline used. Conclusions. A new mechanism to produce the dust in the
presented debris disks, deviations from the conditions required for a standard
equilibrium collisional cascade (grain size exponent of -3.5), and/or
significantly different dust properties would be necessary to explain the
potentially steep SED shape of the three debris disks presented. (abridged)Comment: 14 pages, 4 figures, accepted by A&
Debris discs in binaries: a numerical study
Debris disc analysis and modelling provide crucial information about the
structure and the processes at play in extrasolar planetary systems. In binary
systems, this issue is more complex because the disc should in addition respond
to the companion star's perturbations. We explore the dynamical evolution of a
collisionally active debris disc for different initial parent body populations,
diverse binary configurations and optical depths. We focus on the radial extent
and size distribution of the disc at a stationary state. We numerically follow
the evolution of massless small grains, initially produced from a
circumprimary disc of parent bodies following a size distribution in ds . Grains are submitted to both stars' gravity as well as
radiation pressure. In addition, particles are assigned an empirically derived
collisional lifetime. For all the binary configurations the disc extends far
beyond the critical semimajor axis for orbital stability. This is due
to the steady production of small grains, placed on eccentric orbits reaching
beyond by radiation pressure. The amount of matter beyond acrit
depends on the balance between collisional production and dynamical removal
rates: it increases for more massive discs as well as for eccentric binaries.
Another important effect is that, in the dynamically stable region, the disc is
depleted from its smallest grains. Both results could lead to observable
signatures. We have shown that a companion star can never fully truncate a
collisionally active disc. For eccentric companions, grains in the unstable
regions can significantly contribute to the thermal emission in the mid-IR.
Discs with sharp outer edges, especially bright ones such as HR4796A, are
probably shaped by other mechanisms.Comment: accepted for publication in A&
Debris discs around nearby Solar analogues
An unbiased search for debris discs around nearby Sun-like stars is reported.
Thirteen G-dwarfs at 12-15 parsecs distance were searched at 850 \umum
wavelength, and a disc is confirmed around HD 30495. The estimated dust mass is
0.008 M with a net limit \la 0.0025 M for the average
disc of the other stars. The results suggest there is not a large missed
population of substantial cold discs around Sun-like stars -- HD 30495 is a
bright rather than unusually cool disc, and may belong to a few hundred Myr-old
population of greater dust luminosity. The far-infared and millimetre survey
data for Sun-like stars are well fitted by either steady state or stirred
models, provided that typical comet belts are comparable in size to that in the
Solar System.Comment: published in MNRA
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