89 research outputs found
Shape and spin distributions of asteroid populations from brightness variation estimates and large databases
Context. Many databases on asteroid brightnesses (e.g. ALCDEF, WISE) are
potential sources for extensive asteroid shape and spin modelling. Individual
lightcurve inversion models require several apparitions and hundreds of data
points per target. However, we can analyse the coarse shape and spin
distributions over populations of at least thousands of targets even if there
are only a few points and one apparition per asteroid. This is done by
examining the distribution of the brightness variations observed within the
chosen population.
Aims. Brightness variation has been proposed as a population-scale rather
than individual-target observable in two studies so far. We aim to examine this
approach rigorously to establish its theoretical validity, degree of
ill-posedness, and practical applicability.
Methods. We model the observed brightness variation of a target population by
considering its cumulative distribution function (CDF) caused by the joint
distribution function of two fundamental shape and spin indicators. These are
the shape elongation and the spin latitude of a simple ellipsoidal model. The
main advantage of the model is that we can derive analytical basis functions
that yield the observed CDF as a function of the shape and spin distribution.
The inverse problem can be treated linearly. Even though the inaccuracy of the
model is considerable, databases of thousands of targets should yield some
information on the distribution.
Results. We establish the theoretical soundness and the typical accuracy
limits of the approach both analytically and numerically. Using simulations, we
derive a practical estimate of the model distribution in the (shape,
spin)-plane. We show that databases such as Wide-field Infrared Survey Explorer
(WISE) yield coarse but robust estimates of this distribution, and as an
example compare various asteroid families with each other.Comment: 16 pages, 21 figures, manuscript accepted in Astronomy &
Astrophysics, to be published in section 10. Planets and planetary system
Physical and dynamical properties of the main belt triple asteroid (87) Sylvia
We present the analysis of high angular resolution observations of the triple
Asteroid (87) Sylvia collected with three 8-10 m class telescopes (Keck, VLT,
Gemini North) and the Hubble Space Telescope. The moons' mutual orbits were
derived individually using a purely Keplerian model. We computed the position
of Romulus, the outer moon of the system, at the epoch of a recent stellar
occultation which was successfully observed at less than 15 km from our
predicted position, within the uncertainty of our model. The occultation data
revealed that the Moon, with a surface-area equivalent diameter
Ds=23.10.7km, is strongly elongated (axes ratio of
2.70.32.70.3), significantly more than single asteroids of similar
size in the main-belt. We concluded that its shape is probably affected by the
tides from the primary. A new shape model of the primary was calculated
combining adaptive-optics observations with this occultation and 40 archived
light-curves recorded since 1978. The difference between the
J2=0.024-0.009+0.016 derived from the 3-D shape model assuming an homogeneous
distribution of mass for the volume equivalent diameter Dv=27310km primary
and the null J2 implied by the Keplerian orbits suggests a non-homogeneous mass
distribution in the asteroid's interior
An anisotropic distribution of spin vectors in asteroid families
Current amount of ~500 asteroid models derived from the disk-integrated
photometry by the lightcurve inversion method allows us to study not only the
spin-vector properties of the whole population of MBAs, but also of several
individual collisional families. We create a data set of 152 asteroids that
were identified by the HCM method as members of ten collisional families, among
them are 31 newly derived unique models and 24 new models with well-constrained
pole-ecliptic latitudes of the spin axes. The remaining models are adopted from
the DAMIT database or the literature. We revise the preliminary family
membership identification by the HCM method according to several additional
criteria - taxonomic type, color, albedo, maximum Yarkovsky semi-major axis
drift and the consistency with the size-frequency distribution of each family,
and consequently we remove interlopers. We then present the spin-vector
distributions for eight asteroidal families. We use a combined orbital- and
spin-evolution model to explain the observed spin-vector properties of objects
among collisional families. In general, we observe for studied families similar
trends in the (a_p, \beta) space: (i) larger asteroids are situated in the
proximity of the center of the family; (ii) asteroids with \beta>0{\deg} are
usually found to the right from the family center; (iii) on the other hand,
asteroids with \beta<0{\deg} to the left from the center; (iv) majority of
asteroids have large pole-ecliptic latitudes (|\beta|\gtrsim 30{\deg}); and
finally (v) some families have a statistically significant excess of asteroids
with \beta>0{\deg} or \beta<0{\deg}. Our numerical simulation of the long-term
evolution of a collisional family is capable of reproducing well the observed
spin-vector properties. Using this simulation, we also independently constrain
the age of families Flora (1.0\pm0.5 Gyr) and Koronis (2.5-4 Gyr).Comment: Accepted for publication in A&A (September 16, 2013
The binary near-Earth asteroid (175706) 1996 FG3 - An observational constraint on its orbital evolution
Using our photometric observations taken between 1996 and 2013 and other
published data, we derived properties of the binary near-Earth asteroid
(175706) 1996 FG3 including new measurements constraining evolution of the
mutual orbit with potential consequences for the entire binary asteroid
population. We also refined previously determined values of parameters of both
components, making 1996 FG3 one of the most well understood binary asteroid
systems. We determined the orbital vector with a substantially greater accuracy
than before and we also placed constraints on a stability of the orbit.
Specifically, the ecliptic longitude and latitude of the orbital pole are
266{\deg} and -83{\deg}, respectively, with the mean radius of the uncertainty
area of 4{\deg}, and the orbital period is 16.1508 +/- 0.0002 h (all quoted
uncertainties correspond to 3sigma). We looked for a quadratic drift of the
mean anomaly of the satellite and obtained a value of 0.04 +/- 0.20 deg/yr^2,
i.e., consistent with zero. The drift is substantially lower than predicted by
the pure binary YORP (BYORP) theory of McMahon and Scheeres (McMahon, J.,
Scheeres, D. [2010]. Icarus 209, 494-509) and it is consistent with the theory
of an equilibrium between BYORP and tidal torques for synchronous binary
asteroids as proposed by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D.
[2011]. ApJ Letters, 736, L19). Based on the assumption of equilibrium, we
derived a ratio of the quality factor and tidal Love number of Q/k = 2.4 x 10^5
uncertain by a factor of five. We also derived a product of the rigidity and
quality factor of mu Q = 1.3 x 10^7 Pa using the theory that assumes an elastic
response of the asteroid material to the tidal forces. This very low value
indicates that the primary of 1996 FG3 is a 'rubble pile', and it also calls
for a re-thinking of the tidal energy dissipation in close asteroid binary
systems.Comment: Many changes based on referees comment
Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva
From a set of adaptive optics (AO) observations collected with the W.M. Keck telescope between August and September 2009, we derived the orbital parameters of the most recently discovered satellites of the large C-type asteroid (93) Minerva. The satellites of Minerva, which are approximately 3 and 4 km in diameter, orbit very close to the primary (∼5 and ∼8 × R_p and ∼1% and ∼2% × R_(Hill)) in a circular manner, sharing common characteristics with most of the triple asteroid systems in the main-belt. Combining these AO observations with lightcurve data collected since 1980 and two stellar occultations in 2010 and 2011, we removed the ambiguity of the pole solution of Minerva’s primary and showed that it has an almost regular shape with an equivalent diameter D_(eq) = 154 ± 6 km in agreement with IRAS observations. The surprisingly high bulk density of 1.75 ± 0.30 g/cm3 for this C-type asteroid, suggests that this taxonomic class is composed of asteroids with different compositions, For instance, Minerva could be made of the same material as dry CR, CO, and CV meteorites. We discuss possible scenarios on the origin of the system and conclude that future observations may shine light on the nature and composition of this fifth known triple main-belt asteroid
2021 occultations and transits of Linus orbiting (22) Kalliope: I. Polygonal and `cliptracing' algorithm
The satellite Linus orbiting the main-belt asteroid (22) Kalliope exhibited
occultation and transit events in late 2021. A photometric campaign was
organized and observations were taken by the TRAPPIST-South, SPECULOOS-Artemis,
OWL-Net, and BOAO telescopes, with the goal to constrain models of this system.
Our dynamical model is complex, with multipoles (up to the order ),
internal tides, and external tides. The model was constrained by astrometry
(spanning 2001--2021), occultations, adaptive-optics imaging, calibrated
photometry, as well as relative photometry. Our photometric model was
substantially improved. A new precise () light curve
algorithm was implemented, based on polygon intersections, which are computed
exactly -- by including partial eclipses and partial visibility of polygons.
Moreover, we implemented a `cliptracing' algorithm, based again on polygon
intersections, in which partial contributions to individual pixels are computed
exactly. Both synthetic light curves and synthetic images are then very smooth.
Based on our combined solution, we confirmed the size of Linus, . However, this solution exhibits some tension between the light
curves and the PISCO speckle-interferometry dataset. In most solutions, Linus
is darker than Kalliope, with the albedos vs. . This
is confirmed on deconvolved images. A~detailed revision of astrometric data
allowed us to revise also the value of Kalliope. Most
importantly, a~homogeneous body is excluded. For a differentiated body, two
solutions exist: low-oblateness (), with a~spherical iron
core, and alternatively, high-oblateness () with an
elongated iron core. These correspond to the low- and high-energy collisions,
respectively, studied by means of SPH simulations in our previous work.Comment: Astronomy and Astrophysics, accepte
- …