2,844 research outputs found
Spirals in protoplanetary disks from photon travel time
Spiral structures are a common feature in scattered-light images of
protoplanetary disks, and of great interest as possible tracers of the presence
of planets. However, other mechanisms have been put foward to explain them,
including self-gravity, disk-envelope interactions, and dead zone boundaries.
These mechanisms explain many spirals very well, but are unable to easily
account for very loosely wound spirals and single spiral arms. We study the
effect of light travel time on the shape of a shadow cast by a clump orbiting
close (within au) of the central star, where there can be
significant orbital motion during the light travel time from the clump to the
outer disk and then to the sky plane. This delay in light rays reaching the sky
plane gives rise to a variety of spiral- and arc-shaped shadows, which we
describe with a general fitting formula for a flared, inclined disk.Comment: Accepted for publication in A&A Letters. Videos available at
dl.dropboxusercontent.com/u/3526708/spiralmovies.zi
How Do Induced Affective States Bias Emotional Contagion to Faces? A Three-Dimensional Model
Affective states can propagate in a group of people and influence their ability to judge others’ affective states. In the present paper, we present a simple mathematical model to describe this process in a three-dimensional affective space. We obtained data from 67 participants randomly assigned to two experimental groups. Participants watched either an upsetting or uplifting video previously calibrated for this goal. Immediately, participants reported their baseline subjective affect in three dimensions: (1) positivity, (2) negativity, and (3) arousal. In a second phase, participants rated the affect they subjectively judged from 10 target angry faces and ten target happy faces in the same three-dimensional scales. These judgments were used as an index of participant’s affective state after observing the faces. Participants’ affective responses were subsequently mapped onto a simple three-dimensional model of emotional contagion, in which the shortest distance between the baseline self-reported affect and the target judgment was calculated. The results display a double dissociation: negatively induced participants show more emotional contagion to angry than happy faces, while positively induced participants show more emotional contagion to happy than angry faces. In sum, emotional contagion exerted by the videos selectively affected judgments of the affective state of others’ faces. We discuss the directionality of emotional contagion to faces, considering whether negative emotions are more easily propagated than positive ones. Additionally, we comment on the lack of significant correlations between our model and standardized tests of empathy and emotional contagion.DFG, 414044773, Open Access Publizieren 2019 - 2020 / Technische Universität Berli
Lattice-Based proof of a shuffle
In this paper we present the first fully post-quantum proof of a shuffle for RLWE encryption schemes. Shuffles are commonly used to construct mixing networks (mix-nets), a key element to ensure anonymity in many applications such as electronic voting systems. They should preserve anonymity even against an attack using quantum computers in order to guarantee long-term privacy. The proof presented in this paper is built over RLWE commitments which are perfectly binding and computationally hiding under the RLWE assumption, thus achieving security in a post-quantum scenario. Furthermore we provide a new definition for a secure mixing node (mix-node) and prove that our construction satisfies this definition.Peer ReviewedPostprint (author's final draft
Recensión: Noguera, P. A., Pierce, J. C. y Ahram, R. (Eds.). (2016). Race, equity, and education: sixty years from Brown. Nueva York: Springer. 297 páginas. ISBN 978-3-319-23771-8
Observational diagnostics of elongated planet-induced vortices with realistic planet formation timescales
Gap-opening planets can generate dust-trapping vortices that may explain some
of the latest discoveries of high-contrast crescent-shaped dust asymmetries in
transition discs. While planet-induced vortices were previously thought to have
concentrated shapes, recent computational work has shown that these features
naturally become much more elongated in the gas when simulations account for
the relatively long timescale over which planets accrete their mass. In this
work, we conduct two-fluid hydrodynamical simulations of vortices induced by
slowly-growing Jupiter-mass planets in discs with very low viscosity (). We simulate the dust dynamics for four particle sizes
spanning 0.3 mm to 1 cm in order to produce synthetic ALMA images. In our
simulations, we find that an elongated vortex still traps dust, but not
directly at its center. With a flatter pressure bump and disruptions from the
planet's overlapping spiral density waves, the dust instead circulates around
the vortex. This motion (1) typically carries the peak off-center, (2) spreads
the dust out over a wider azimuthal extent , (3) skews the
azimuthal profile towards the front of the vortex, and (4) can also create
double peaks in newly-formed vortices. In particular, we expect that the most
defining observational signature, a peak offset of more than ,
should be detectable of the time in observations with a beam diameter
of at most the planet's separation from its star.Comment: Accepted to MNRAS. 13 pages, 8 figures. Movies available at:
https://lavinia.as.arizona.edu/~mhammer/vortex_signatures.htm
An Inner Disk in the Large Gap of the Transition Disk SR 24S
We report new Atacama Large Millimeter/sub-millimeter Array (ALMA) Band 3
observations at 2.75 mm of the TD around SR 24S with an angular resolution of
0.11'' 0.09'' and a peak signal-to-noise ratio of . We
detect an inner disk and a mostly symmetric ring-like structure that peaks at
0.32'', that is 37 au at a distance of 114.4 pc. The full
width at half maximum of this ring is 28 au. We analyze the observed
structures by fitting the dust continuum visibilities using different models
for the intensity profile, and compare with previous ALMA observations of the
same disk at 0.45 mm and 1.30 mm. We qualitatively compare the results of these
fits with theoretical predictions of different scenarios for the formation of a
cavity or large gap. The comparison of the dust continuum structure between
different ALMA bands indicates that photoevaporation and dead zone can be
excluded as leading mechanisms for the cavity formation in SR 24S disk, leaving
the planet scenario (single or multiple planets) as the most plausible
mechanism. We compared the 2.75 mm emission with published (sub-)centimeter
data and find that the inner disk is likely tracing dust thermal emission. This
implies that any companion in the system should allow dust to move inwards
throughout the gap and replenish the inner disk. In the case of one single
planet, this puts strong constraints on the mass of the potential planet inside
the cavity and the disk viscosity of about 5 and
, respectively.Comment: Accepted to Ap
Rotationally resolved spectroscopy of (20000) Varuna in the near-infrared
Models of the escape and retention of volatiles by minor icy objects exclude
any presence of volatile ices on the surface of TNOs smaller than ~1000km in
diameter at the typical temperature in this region of the solar system, whereas
the same models show that water ice is stable on the surface of objects over a
wide range of diameters. Collisions and cometary activity have been used to
explain the process of surface refreshing of TNOs and Centaurs. These processes
can produce surface heterogeneity that can be studied by collecting information
at different rotational phases. The aims of this work are to study the surface
composition of (20000)Varuna, a TNO with a diameter ~650km and to search for
indications of rotational variability. We observed Varuna during two
consecutive nights in January 2011 with NICS@TNG obtaining a set of spectra
covering the whole rotation period of Varuna. After studying the spectra
corresponding to different rotational phases, we did not find any indication of
surface variability. In all the spectra, we detect an absorption at 2{\mu}m,
suggesting the presence of water ice on the surface. We do not detect any other
volatiles on the surface, although the S/N is not high enough to discard their
presence. Based on scattering models, we present two possible compositions
compatible with our set of data and discuss their implications in the frame of
the collisional history of the Kuiper Belt. We find that the most probable
composition for the surface of Varuna is a mixture of amorphous silicates,
complex organics, and water ice. This composition is compatible with all the
materials being primordial. However, our data can also be fitted by models
containing up to a 10% of methane ice. For an object with the characteristics
of Varuna, this volatile could not be primordial, so an event, such as an
energetic impact, would be needed to explain its presence on the surface.Comment: 6 pages, 5 figures, to be published in A&
Research Brief: Pre and post-intervention comparative analysis - School level data and multi-informant survey knowledge, attitudes and practices (KAP) on disability and inclusive education
Research Brief: Post-intervention multi-informant survey on knowledge, attitudes and practices (KAP) on disability and inclusive education
Disrupted asteroid P/2016 G1. II. Follow-up observations from the Hubble Space Telescope
After the early observations of the disrupted asteroid P/2016 G1 with the
10.4m Gran Telescopio Canarias (GTC), and the modeling of the dust ejecta, we
have performed a follow-up observational campaign of this object using the
Hubble Space Telescope (HST) during two epochs (June 28 and July 11, 2016). The
analysis of these HST images with the same model inputs obtained from the GTC
images revealed a good consistency with the predicted evolution from the GTC
images, so that the model is applicable to the whole observational period from
late April to early July 2016. This result confirms that the resulting dust
ejecta was caused by a relatively short-duration event with onset about 350
days before perihelion, and spanning about 30 days (HWHM). For a size
distribution of particles with a geometric albedo of 0.15, having radii limits
of 1 m and 1 cm, and following a power-law with index --3.0, the total
dust mass ejected is 210 kg. As was the case with the GTC
observations, no condensations in the images that could be attributed to a
nucleus or fragments released after the disruption event were found. However,
the higher limiting magnitude reachable with the HST images in comparison with
those from GTC allowed us to impose a more stringent upper limit to the
observed fragments of 30 m.Comment: 10 pages, 2 figures Accepted by Astronomical Journal, Nov. 2, 201
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