A&A 370, 447-455 (2001)
DOI: 10.1051/0004-6361:20010199
J. C. Augereau1 - R. P. Nelson2 - A. M. Lagrange1 - J. C. B. Papaloizou2 - D. Mouillet1
1 - Laboratoire
d'Astrophysique de l'Observatoire de Grenoble, Université J.
Fourier, CNRS, BP 53,
38041 Grenoble Cedex 9, France
2 -
Astronomy Unit, School of Mathematical Sciences, Queen Mary
& Westfield College, Mile End Road, London E1 4NS, UK
Received 27 October 2000 / Accepted 19 January 2001
Abstract
We report a new and complete model of the Pictoris disk,
which succeeds in accounting for both the surface brightness
distribution, warp characteristics, the outer ``butterfly'' asymmetry
as observed by HST/STIS in scattered light, as well as the infrared
emission.
Our model includes the presence of a disk of planetesimals extending
out to 120-150AU, perturbed gravitationally by a giant planet on an
inclined orbit, following the approach of Mouillet et al. (1997b). At any time,
the planetesimal disk is assumed to be the source of a distribution of
grains produced through collisional evolution, with the same initial
orbital parameter distribution. The steady state spatial grain
distribution is found incorporating the effects of radiation pressure
which can cause the distribution of the smallest particles to become
very distended.
With realistic assumptions about the grains' chemical properties, the
modeling confirms the previously evident need for an additional
population of hot grains close to the star, to account for the
12
m fluxes at short distances from the star. It also indicates
that this population cannot explain the outer 12
m flux
distribution when the effects of gravity and radiation pressure
determine the distribution. Very small grains, produced by
collisions among aggregates, are tentatively proposed to account for
this 12
m outer emission.
Key words: stars: circumstellar matter - stars:
Pictoris
The Pictoris gaseous and dusty disk has been extensively studied for 15
years. The dust disk, seen nearly edge-on, extends to at least a
distance of 100AU from the central star, with a sharp decrease in
the surface brightness distribution of scattered light beyond about
120AU. The dynamics of the small grains producing the scattered
light is determined by radiation pressure, collisions with other
grains and/or evaporation and to a lesser extent, Poynting-Robertson
drag. The images at 12
m show that the maximum of the dust
surface density distribution is located between 80AU and 100AU
(Pantin et al. 1997, assuming the Hipparcos distance of 19.28pc from Crifo et al. 1997 for
Pictoris). The total dust mass, as measured from
sub-millimeter data, ranges between a few and a few tens of lunar
masses (Zuckerman & Becklin 1993; Holland et al. 1998; Dent et al. 2000).
The 10m silicate spectrum (Knacke et al. 1993) appears to mimic that
of Halley's comet but not that of comet Hale-Bopp (Lagage et al. 1999). The
10
m features are best fitted by the emission of small
(submicronic) crystalline silicates (Knacke et al. 1993; Li & Greenberg 1998). It was
suggested that these grains could result from comet evaporation, a
scenario that had already been proposed to explain the very peculiar
spectroscopic activity (Lagrange et al. 1987; Ferlet et al. 1987). Furthermore,
Lecavelier des Etangs et al. (1996)
proposed that the appearance of the entire disk, as seen in scattered
light, could be explained by grains released from evaporating comets
at distances of 15-30AU and subsequently pushed out by radiation
pressure.
The Northeast and Southwest extensions of the dust disk have been found to be asymmetric in scattered light as well as in thermal emission. At visual wavelength, Kalas & Jewitt (1995) noticed five radial or vertical asymmetries beyond 150AU. In the Northeast extension for example, the vertical brightness distribution in scattered light is asymmetric with respect to the disk mid-plane out to hundreds of AU and this situation is reversed in the Southwest extension (``butterfly'' asymmetry). Kalas et al. (2000) and Larwood et al. (2001) recently proposed that this asymmetry is produced by a close encounter with a M0V star in the last 105 years.
In the inner part of the disk (at about 60-70AU) the 12m
images reveal a factor of 3 side to side brightness asymmetry
(Pantin et al. 1997) which is much smaller at optical and near-infrared
wavelengths (Mouillet et al. 1997a, at most a factor of 1.5). Orbiting
evaporating bodies on eccentric orbits with the same longitude of
periastron can produce such axial asymmetries
(Lecavelier des Etangs et al. 1996; Lecavelier des Etangs 1998).
Adaptive optics (Mouillet et al. 1997b) and HST observations (Burrows et al. 1995; Heap et al. 2000) revealed the inner warping of its dust disk at about 70AU and in the same direction as the ``butterfly'' asymmetry. Mouillet et al. (1997b) modeled this warp as being due to grains which followed the distribution of a parent body planetesimal disk which was perturbed by the gravitational influence of a Jupiter-like planet on an orbit inclined at 3 degrees to the disk mid-plane.
The important effect of perturbation by the giant planet is to cause the parent body disk to precess differentially. The more rapid precession in the inner regions causes the parent body disk to become coplanar with the planetary orbit. At large distances the inclination of the parent body disk retains its initial value. The warp is located in the transition region where the local orbital precession timescale is comparable to the age of the system. The location of the warp accordingly propagates outwards with time.
Mouillet et al. (1997b) found an approximate relationship between the position
of the warp, the mass ratio of planet to star, its orbital (assumed
circular) radius and the age of the system in the form:
Note that when, as assumed here, the warp location is significantly larger than the orbital radius, that location depends only on the product of the age of the system, the square of the orbital radius and the planetary mass ratio. We comment that, because it does not incorporate a non axisymmetric perturbation, the model proposed by Lecavelier des Etangs et al. (1996) cannot account for the inner warp, but the influence of radiation pressure, clearly revealed by their study, is certainly of great importance.
Complete modeling of the disk has not been performed so far. In this
paper we formulate a model of the disk which reproduces both the
scattered light images, in particular the warped disk and the
``butterfly'' asymmetry, and also the infrared (IR) images and fluxes.
In Sect. 2, we outline the basis of this model and Sect. 3 presents the scattered light images which can be compared
with the recent HST/STIS data (Heap et al. 2000). In Sect. 4,
we synthesize the IR 12m image and compare with the
observations. In Sect. 5 we summarize and discuss the proposed model in a more general context.
The short lifetime of the grains, in comparison to the age of the system, as a result of the action of collisions and radiation pressure leads to the hypothesis of the existence of a parent body disk consisting of planetesimals with sizes larger than 1m which acts as a source for the grains as collision products (see for example the discussion in Mouillet et al. 1997b, and references therein).
As in Mouillet et al. (1997b) we suppose that the physical collision time in
the parent body disk is sufficiently long compared to the age of the
system that it can be approximated as a collisionless disk lying
between 1.5D and 15D. The disk aspect ratio H/r is taken to be
0.1. Through our modeling procedure we are able to construct arbitrary
surface density profiles. This is done by constructing parent body
disks consisting of weighted contributions from 100 elementary rings
composed of 104 particles and with a ratio of inner and outer radii
equal to
.
This is possible because the
particles are collisionless.
For working parameters we adopt
being also the model
unit of distance, planet to star mass ratio
M/M* = 10-3,planetary orbital eccentricity of zero with an inclination of 3
with respect to the initial mid-plane of the parent body disk.
However, as above, we note that the important parameter is MD2rather than M and D separately. Mouillet et al. (1997b) also show that the
propagation of the warp is unaffected for eccentricities of the
planetary orbit up to 0.5. However, large eccentricities may lead to
side to side (radial) asymmetries of the parent body disc which in
turn may lead to some asymmetries in the generation of small dust
particles. The study of asymmetries produced in this way is beyond the
scope of this paper.
The configuration of the warped parent body disk, obtained using the
above procedures, with the surface density we adopted is illustrated
in Fig. 1.
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Figure 1:
Vertical position of the mean PB disk mass assuming
the surface density distribution of Fig. 2. The
vertical and radial scales are not the same in this figure. The
warped disk extends out to 140-150AU with a maximum close to
75AU from the star and a vertical extension of ![]() |
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We assume that each planetesimal (parent body or hereafter PB) is the
progenitor of small particles (produced for instance by collisions)
that are significantly affected by the radiation pressure of the
central star. We assume no initial relative velocity between the PB
and the smallest particles produced. A consequence of this assumption
and the near circular motion of the PB is that the periastron of a
dust particle equals that of the PB. The effect of radiation pressure
is quantified by the ratio of the force due to radiation pressure to
that due to the gravity of the central star,
The case
corresponds to a
bound dust particle with the same motion as its PB. When
,
particles have zero energy and so are just
unbound. We consider 11 values of
equally spaced
between and including 0.45 and 0.001. For each value of
,
a dust distribution is generated from the PB by phase
mixing 106 particles for 20 orbital periods measured
at the outer radius of the disk. The time-scales
required for phase mixing are always short compared to the time-scale
for propagating the warp. Also the optical depth of the disk is large
enough that the timescale for destruction of the dust by collisions is
shorter than any drag timescale due to the Poynting-Robertson effect
(see also Mouillet et al. 1997b). The Poynting-Robertson effect then is
neglected here.
To construct the final image of the disk in scattered light or in
thermal emission arising from any PB surface density distribution in
practice, a radial weight function is applied to the contribution from
each dust particle depending on the elementary ring between 1.5D and
15D from which it originated (the distance to this ring also
corresponds to the periastron distance of the dust particle). Several
distributions can therefore be investigated using this
technique in a reasonable amount of time.
The image of the disk also depends on the physical properties of the
grains. Here we have adopted the comet dust model proposed by
Li & Greenberg (1998, and references therein) to reproduce the Pictoris spectral
energy distribution (SED). In this model, the dust consists of porous
aggregates made from a silicate core coated with organic refractories
(see also Pantin et al. 1997). A more detailed account of the grain model
used here is given in Augereau et al. (1999). Initially, we fix the porosity
of the grains to be 0.95 and assume that most are amorphous
(Li & Greenberg 1998; Lagage et al. 1999).
Water ice may be present on the surfaces of the elementary submicronic
particles that compose an aggregate (Greenberg & Hage 1990, and references therein). The amount of ice is quantified by a volume
percentage in addition to that of vacuum (due to the porosity). A
grain is assumed icy if it is produced further than the ice
sublimation distance. That distance depends on the grain size and
amount of ice (typically between 20AU for grains larger than
100
m and 100AU for grains smaller than
1
m).
Due to the effect of radiation pressure, non-icy grains can be present
at very large distances as well as icy grains, possibly mixing two
dust chemical compositions at a given distance from the star.
For the range of
values we consider, there is a
one-to-one relationship between the value of
and the
grain size a which can be expressed in the form
(Artymowicz 1988, for instance), where Kdepends on the optical properties of the grain which are computed
using the Mie theory
(Bohren & Huffman 1983). Some examples of K values for
different amounts of ice and porosities can be derived from the values
of
given in Table 1. A grain size
distribution with
is assumed to take into
account the relative number n(a) of grains with radius greater than
a produced in the disk by collision processes. For each
value (or grain size), the appropriate relative number
density and thus the contribution to a scattered light or thermal
emission image is computed. The 11 independent images then are
correctly superimposed with appropriate weight factors so as to
produce a final image of the disk for any required PB surface density
distribution or wavelength of interest.
In order to complete the above procedure, the disk orientation with respect to the observer has to be specified. This introduces two additional parameters: the line of nodes of the perturbing planet and the disk inclination with respect to a plane normal to the line of sight.
The first stage in the modeling procedure is to find a surface density
distribution for the PB disk that leads to consistent results with
both scattered light observations and thermal emission data.
![]() |
Figure 2:
Surface density of the PB disk (bold-dashed line) that gives
a good fit to the observed surface brightness distribution in
scattered light. The resulting dust surface density integrated over
the grain size (or
![]() ![]() |
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Applying the observational constraints described above, we tried several PB body surface density distributions. We were able to find a solution (Fig. 2) that gives a fit to the scattered light images (Fig. 3).
In this solution, the distribution of PB is confined inside
150AU. Due to the radiation pressure acting on the grains, the
outer part of the disk is filled with small particles. This can be seen
in Fig. 2, where we have plotted the resulting surface
density distributions for grains of different sizes. The final surface
density of the grains averaged over the grain size distribution peaks
at about 110-120AU from the star, close to the assumed outer edge
of the parent disk (Fig. 2).
IRAS |
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|
Flux at 12![]() |
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0.040 | 0.056 | 0.037 | 0.047 | 0.017 | 0.017 |
Flux at 25![]() |
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3.5 | 2.1 | 3.4 | 1.9 | 2.4 | 1.6 |
Flux at 60![]() |
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12.5 | 16.3 | 12.4 | 16.3 | 11.9 | 13.6 |
Flux at 100![]() |
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10.4 | 10.2 | 10.3 | 10.2 | 9.8 | 9.7 |
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|
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6 | 12 | 7 | 15 | 16 | 26 |
At distances greater than about 30AU, the main shape of the mid-plane
surface brightness distribution in scattered light from Heap et al. (2000)
is well matched depending somewhat on the precise anisotropic
scattering properties (Fig. 3).
![]() |
Figure 3:
Surface brightness distributions in mag![]() |
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A radial power law index between -5 and -5.5 is measured at distances larger than 120AU when the dust disk is seen almost edge-on as predicted by Lecavelier des Etangs et al. (1996) and indeed observed with the HST/STIS instrument.
Importantly, due to the effect of radiation pressure, the distribution
of the grain sizes is a function of the distance from the star as
shown in Figs. 2 and 4.
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Figure 4:
Upper panel: grain size distribution at different
distances from the star. In each case the distribution is
normalized such that the integral over a has been normalized to
1. Lower panel: N index assuming that the grain size
distribution
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Due to the effect of the assumed perturbing planet, the precession of
the orbital planes of PB within 70-80AU results in a distribution
with average inclination coincident with the planetary orbit. Beyond
70-80AU and up to the assumed outer edge of the PB disk (close to 140-150AU), the PB orbits have undergone only partial precession.
Therefore, the mean inclination of their orbital planes to that of the
initial disk ranges between 3
and about 0.5
.
Mouillet et al. (1997b) showed that the warp, or the short scale asymmetry of the vertical position of the maximum surface brightness, can be reproduced assuming all particles followed the distribution of the parent body disk. Adding the effects of radiation pressure acting on grains with a given size distribution to the model of Mouillet et al. (1997b) causes a modest shift of the warp position, and so does not affect the conclusions on the propagation and observability of the warp as seen in Fig. 5, which can be directly compared to the HST/STIS images (Heap et al. 2000).
We now investigate whether our model can account for the ``butterfly''
asymmetry. Basically, radiation pressure greatly extends the surface
density distribution of the smallest particles, i.e. those which
have the larger
values, beyond that of the PB disk
(Fig. 2).
Accordingly, the asymmetry in the vertical
location of the surface brightness maximum originating in the PB disk
can be transmitted outwards as illustrated in Fig. 6.
The
result is a flared-like disk, with the so-called butterfly asymmetry.
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Figure 5: The warped disk normalized for each vertical cut to its maximum surface brightness. To compare with Fig. 10 from Heap et al. (2000) and to emphasize the vertical asymmetry, contours at 99%, 50% and 10% of the maximum surface brightness have been superimposed |
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For illustrative purpose, we focus on the particular case for which the line of nodes of the planetary orbit and the line of sight are aligned (the observability of the warp as a function of the location of the line of nodes is discussed in Mouillet et al. 1997b). The simulated disk in scattered light then convincingly exhibits a large scale asymmetry as observed in STIS data up to 200AU (Fig. 5).
It is worth noticing that this asymmetry is present much further out
than 200AU (Fig. 7), in agreement with the large scale
images of Kalas & Jewitt (1995) for instance.
Figure 8 quantifies the
radial dependence of the asymmetry by the ratio of half widths at half
maximum above and below the observed mid-plane. The ratio evidences
the position of the warp at 70-80AU and shows that the disk remains
asymmetric up to at least 500AU as observed. In other words, the
asymmetric distribution of PB responsible for the observed warp at
70-80AU, and assumed to result from the perturbation of an inclined
planet, leads naturally to a large scale asymmetry very similar to the
``butterfly'' asymmetry. Therefore, the observability of the
``butterfly'' asymmetry depends as well on the inclination of the
planet to the PB disk mid-plane (3
in this model), and on the
line of nodes of the planet to the line of sight.
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Figure 6:
The location of the maximum surface brightness
for a vertical cut as a function of distance, for disks composed of
grains with a single size as indicated, seen in scattered light. The
line for
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The dynamical approach we have followed allows us to reproduce in a consistent way most observations in scattered light, namely: the surface brightness distribution, the small scale (warp) and large scale (``butterfly'') asymmetries, assuming a planetary perturber and taking into account the effects of radiation pressure acting on the grains. But as expected, the model does not explain the NE-SW asymmetries.
A fully consistent disk model should reproduce both the scattered
light images and thermal data. Our aim is to estimate the thermal IR
(12, 25, 60 and 100m) fluxes produced by the distribution found
in Sect. 3. Table 1 summarizes the computed
fluxes assuming the dust model proposed by Li & Greenberg (1998) for different
porosities and amounts of ice.
The 100m and 60
m emissions (the latter slightly
depending on the amount of ice) are correctly matched by the dust ring
made of grains at the blow-out size limit that reproduces the
scattered light profile.
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Figure 7: Modeled disk at large distances from the star. A large scale asymmetry with respect to the mid-plane is found, similar to the observed ``butterfly'' asymmetry |
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Figure 8: Ratio of half widths at half maximum above and below the observed mid-plane for a vertical cut as a function of distance and for the extension of the disk seen in Fig. 7 |
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On the other hand, the simulated 12m and 25
m fluxes are
smaller than observed. This shows that an additional population of
hotter grains is required, in total agreement with previous works
showing that most of the 12
m emission comes from a region close
to the star (see for example Knacke et al. 1993), which is also confirmed
by the resolved images from Pantin et al. (1997). This close population also
certainly contributes to the integrated 25
m flux.
Most of the 12m flux originates within
20AU from the
star as seen before. However, as shown by Pantin et al. (1997), a small part
of the 12
m flux comes from regions up to
100AU. Our aim
is here to see whether our model accounts for this ``outer''
12
m emission.
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Figure 9:
Linear brightness distribution in thermal emission at
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Core-mantle grains smaller than
K have
ratios larger than 0.5. A close inspection of
Fig. 2 indicates that particles with
ratios larger than typically 0.4 have quite similar surface densities
and tend to mimic that of the
grains which are
almost just unbound. In the following, we will use this property to
simulate a dust disk with very small particles.
We propose hereafter possible scenarios a priori able to explain
the presence of very small grains at large distances, and we check
whether or not they may quantitatively reproduce the 12m flux
at large distances under reasonable assumptions.
A first possibility is that the submicronic grains produced close to
the star, for instance by comet evaporation, responsible for most of
the integrated 12m flux and required to explain the 10
m
silicate spectroscopic features, also supply the disk beyond
30AU with enough small dust particles through radiation
pressure. This would give an attractive solution to the lack of
12
m emission at distances larger than
30AU in our
model.
We therefore assumed a population of very small grains close to the
star and let them evolve under radiation pressure. It appears that,
whatever the assumptions on the surface density distribution of the
inner population, the radial shape of the 12m flux distribution
does not match the one found by Pantin et al. (1997) beyond
30AU.
This is mainly due to the radial decrease of the grain temperature
with distance from the star which tends to result in most of the
emission at 12
m
coming from close to the star leading either to
very to small contributions further than
30AU or to radial
profiles for the emission not consistent with the resolved observations.
A population of submicronic grains certainly exists close to the star
but our modeling indicates that additional grains produced further
than 30AU should be present to account for the radial shape of
the 12
m emission.
We will now consider the dust disk that reproduces the scattered light
data and extrapolate the initial a-3.5 grain size distribution to
grains with
ratios larger than 0.5. We consider
non-icy grains for simplicity and P=0.95 which gives good fits to
the large wavelength fluxes.
In other terms, we simply extend the grain size distribution that
successfully fitted the scattered light images in Sect. 3
to a minimum grain size of about 0.1m instead of a few tens of
micrometers. This actually allows us to fit the 12
m emission
further than
20AU. The 60
m
and 100
m integrated fluxes
are unchanged as well as the scattered light profile inside 120AU
because the amount of large grains is not affected by the reduction in
minimum grain size. However, beyond 120AU, the scattered light
surface brightness profile changes: it follows now a r-3.5 radial
power law (instead of r-5). r-3.5 is not consistent with
STIS data, but is in better agreement with previous data
(e.g. Golimowski et al. 1993; Kalas & Jewitt 1995; Mouillet et al. 1997b).
It is therefore premature to conclude whether or not this extrapolation is correct on the sole basis of the surface brightness distribution at large distances. Moreover, the rate of production of such small grains must be continuous and more efficient than indicated by a simple extrapolation from the larger grains, since being unbound, their life-time in the disk is very short, in fact 1 to 103 times shorter than grains with sizes just above the blow out limit. The mass loss rate from the system due to the blow out of these grains is also correspondingly larger.
The physics of aggregates, present in circumstellar environments, is complex and
not well understood. Catastrophic disruption of an aggregate can occur
if the impact velocity is high enough (typically a few tenths of
kms-1, Dominik & Tielens 1997, for instance), producing nearly compact
submicronic grains.
In the vicinity of Pictoris, such grains smaller than
10
m
may have
ratios smaller than 0.5 depending on their
precise chemical composition, i.e. if they are not too
refractory (e.g. Artymowicz 1988). This leads ultimately to a
discontinuity in the grain size distribution which could appear
depleted in grains of sizes ranging between
10
m and 2 K.
We tested this scenario by assuming an additional population of
m compact silicate grains with a surface density
distribution that corresponds to that of the
particles. The 12
m resolved emission is very well matched in
terms of shape and flux
20-30AU with a mass of
m grains of the same order of magnitude as the mass
contained in the particles of size 2 K. The far-IR emission and the
scattered light images, in particular the r-5 radial shape of the
surface brightness distribution further than 120AU, are not affected
by the presence of such very small grains since they are very poor
scatterers. The presence of such very small grains, and if so, their
chemical composition as well as their size distribution, remain
open issues.
As in Mouillet et al. (1997b), we assumed a disk of planetesimals orbiting
around Pictoris and subject to the gravitational perturbation of a planet
on an inclined orbit.
Assuming that collisions among these planetesimals produce grains with
a size distribution proportional to a-3.5 between the blow out
limit and millimeter sizes, and assuming that these grains are subject
to radiation pressure in addition to gravitational forces, and using
plausible chemical composition and optical properties for the grains,
we are able to reproduce the scattered light images (intensity, radial
distribution, warp, ``butterfly'' asymmetry) as well as the far IR
integrated fluxes. The PB are located between 20 and 150AU with a
peak at 100-120AU. Due to radiation pressure, the grain
radial distribution strongly depends on their size and the resulting
dust disk extends very far from the star. The ``butterfly'' asymmetry
is nothing more than the mirror of the warp of PB disk at larger
distances due to radiation pressure.
The 12m images require an additional population of small grains
close to the star as was evident several years ago and attributed to
comet evaporation. We have shown that radiation pressure acting on
these grains does not produce a distribution that can account for the
observed radial shape of the 12
m emission as found by Pantin et al. (1997) at distances larger than
20-30AU. A population
of grains smaller than (or comparable to) the blow-out limit in
addition to the population necessary to reproduce the scattered light
images may account for this >30AU 12
m emission. It is
found that the extrapolation of the a-3.5 distribution down to
such small sizes is somewhat problematic. A tentative alternative
could be that there is a discrete population of grains with size less
than
m in addition to the main population of grains.
This is plausible as we assume that the main population of grains is
made of porous aggregates ultimately breaking down and producing <10
m grains that could be responsible for the emission
further than 30AU at 12
m, without affecting the scattered
light images and the 60-100
m integrated fluxes. As another
alternative, it is also possible to argue that the a-3.5 law is
unlikely close to the blow-out limit: grains close to the blow-out
size may be over-abundant simply because of the lack of smaller grains
able to efficiently destroy them. In this latter scenario, a larger
number of small grains is explained as a result of collisions, without
involving additional processes.
Finally, our consistent modeling of the Pictoris disk, combining the
various available observations has the following limitations: 1) the
solution found is probably not unique as various parameters (optical
properties, size distribution, spatial distribution, grain production
mechanisms) are intricately involved; 2) the application of the
a-3.5 size distribution all the way between blow-out size and
parent bodies is questionable; 3) the side-to-side asymmetry in the
12
m and 20
m images has not yet been explained.
Obviously, this asymmetry originates close to the star and might be
due to the evaporating comets as was proposed by Lecavelier des Etangs et al. (1996).
Further investigations will be able to benefit from new direct
constraints on the spatial distribution of grains, as observed at
various wavelengths (scattered light and thermal emission high angular
resolution images), for the inner disk (50 AU), and optical
properties of the grains.
Acknowledgements
We wish to thank Philippe Thébault, Alain Lecavelier, Hervé Beust for fruitful discussions. J. C. Augereau and A. M. Lagrange acknowledge visitor support at QMWC through PPARC grant: PPARC GR/J88357.