333 research outputs found
Service médical rendu par la médecine thermale : principales réalisations de l’Afreth, difficultés méthodologiques
The distribution of accretion rates as a diagnostic of protoplanetary disc evolution
We show that the distribution of observed accretion rates is a powerful
diagnostic of protoplanetary disc physics. Accretion due to turbulent
("viscous") transport of angular momentum results in a fundamentally different
distribution of accretion rates than accretion driven by magnetised disc winds.
We find that a homogeneous sample of 300 observed accretion rates
would be sufficient to distinguish between these two mechanisms of disc
accretion at high confidence, even for pessimistic assumptions. Current samples
of T Tauri star accretion rates are not this large, and also suffer from
significant inhomogeneity, so both viscous and wind-driven models are broadly
consistent with the existing observations. If accretion is viscous, the
observed accretion rates require low rates of disc photoevaporation
(Myr). Uniform, homogeneous surveys of
stellar accretion rates can therefore provide a clear answer to the
long-standing question of how protoplanetary discs accrete.Comment: 10 pages, 8 figures. Accepted for publication in MNRA
Lil....
Ä abra ta’ poeżiji u proża li tinkludi: Biki ta’ Omm ta’ Dun Karm – Ras il-Pellegrin ta’ Manwel Agius – L-Aħħar Tislima ta’ Ä użè Galea – Lil Ibni Herman-Baruch ta’ Karmenu Vassallo – Flus ir-Regħba Ħajja Qasira ta’ P. P. Saydon – Frak ta’ R. M. B. – Id-Dolliegħa u l-Qargħa ta’ R. M. B. – Il-Barrakka ta’ Katrin ta’ P. Pawl Tabone – Ħniena! ta’ Fran. Camilleri – Lil.... ta’ M. Agius.N/
Evidence for ubiquitous carbon grain destruction in hot protostellar envelopes
Earth is deficient in carbon and nitrogen by up to orders of
magnitude compared with the Sun. Destruction of (carbon- and nitrogen-rich)
refractory organics in the high-temperature planet forming regions could
explain this deficiency. Assuming a refractory cometary composition for these
grains, their destruction enhances nitrogen-containing oxygen-poor molecules in
the hot gas (K) after the initial formation and sublimation of
these molecules from oxygen-rich ices in the warm gas (K). Using
observations of high-mass protostars with ALMA, we find that
oxygen-containing molecules (CHOH and HNCO) systematically show no
enhancement in their hot component. In contrast, nitrogen-containing,
oxygen-poor molecules (CHCN and CHCN) systematically show an
enhancement of a factor in their hot component, pointing to
additional production of these molecules in the hot gas. Assuming only thermal
excitation conditions, we interpret these results as a signature of destruction
of refractory organics, consistent with the cometary composition. This
destruction implies a higher C/O and N/O in the hot gas than the warm gas,
while, the exact values of these ratios depend on the fraction of grains that
are effectively destroyed. This fraction can be found by future chemical models
that constrain C/O and N/O from the abundances of minor carbon, nitrogen and
oxygen carriers presented here.Comment: Accepted for publication in ApJ Letter
Suldat
Ä abra ta’ poeżiji u proża li tinkludi: Sursum Corda! ta’ R. M. B. – Tal-Qali ta’ Ä użè Ellul – Tfajla ta’ Dun Karm – Meta mort Għawdex bid-dawra ta’ Ä . Cassar-Pullicino – Il-Maqdes tal-Mulej ta’ A. Buttigieg – Il-Barrakka ta’ Katrin ta’ P. Pawl Tabone – Ä lieÄ¡el ta’ Mary Meylak – Is-Suldat ta’ Ä użè Chetcuti.N/
Towards future pedestrian-vehicle interactions: Introducing theoretically-supported AR prototypes
The future urban environment may consist of mixed traffic in which pedestrians interact with automated vehicles (AVs). However, it is still unclear how AVs should communicate their intentions to pedestrians. Augmented reality (AR) technology could transform the future of interactions between pedestrians and AVs by offering targeted and individualized communication. This paper presents nine prototypes of AR concepts for pedestrian-AV interaction that are implemented and demonstrated in a real crossing environment. Each concept was based on expert perspectives and designed using theoretically-informed brainstorming sessions. Prototypes were implemented in Unity MARS and subsequently tested on an unmarked road using a standalone iPad Pro with LiDAR functionality. Despite the limitations of the technology, this paper offers an indication of how future AR systems may support future pedestrian-AV interactions
Comparing different methods to retrieve cloud top height from Meteosat satellite data
Cloud parameters such as the Cloud Top Height (CTH), Cloud Top Temperature (CTT), emissivity, particle size and optical depth have always been matter of interest for the atmospheric community. Particularly the CTH provides information leading to better understand the cloud radiative effects. Although there are many meteorological satellites providing the CTH, there are other sensors, not devoted to this purpose, that give some information from which this crucial parameter can be estimated. In this contribution we will describe three different methodologies to retrieve the CTH. The first technique is based on stereo-vision algorithms and requires two different views of the same scene and does not need of extra atmospheric information. In the second one, brightness temperatures in two IR spectral bands are converted to real cloud temperature by means of the proposed algorithms. From the CTT, the CTH is estimated using temperature vertical profiles (measured or modeled). The third technique retrieves the CTH from the output parameters of post event simulations performed by a Numerical Weather Prediction (NWP) model that in this work will be the mesoscale model WRF (Weather Research Forecast). This article presents a preliminary work, in which the heights retrieved by the three methodologies applied to the geostationary satellite Meteosat 10 are compared with the heights given by MODIS sensor installed on the polar satellite AQUA. This promising results show that valuable information about CTH can be retrieved from Meteosat which provide high frequency and large scale data useful for weather and climate research
A major asymmetric ice trap in a planet-forming disk IV. Nitric oxide gas and a lack of CN tracing sublimating ices and a C/O ratio
[Abridged] Most well-resolved disks observed with ALMA show signs of dust
traps. These dust traps set the chemical composition of the planet forming
material in these disks, as the dust grains with their icy mantles are trapped
at specific radii and could deplete the gas and dust of volatiles at smaller
radii. In this work we analyse the first detection of nitric oxide (NO) in a
protoplanetary disk. We aim to constrain the nitrogen chemistry and the
gas-phase C/O ratio in the highly asymmetric dust trap in the Oph-IRS 48 disk.
We use ALMA observations of NO, CN, CH, and related molecules and model the
effect of the dust trap on the physical and chemical structure using the
thermochemical code DALI. Furthermore, we explore how ice sublimation
contributes to the observed emission lines. NO is only observed at the location
of the dust trap but CN and CH are not detected in the Oph-IRS 48 disk.
This results in an CN/NO column density ratio of and thus a low C/O
ratio at the location of the dust trap. The main gas-phase formation pathways
to NO through OH and NH in the fiducial model predict NO emission that is an
order of magnitude lower than is observed. The gaseous NO column density can be
increased by factors ranging from 2.8 to 10 when the HO and NH gas
abundances are significantly boosted by ice sublimation. However, these models
are inconsistent with the upper limits on the HO and OH column densities
derived from observations. We propose that the NO emission in the Oph-IRS 48
disk is closely related to the nitrogen containing ices sublimating in the dust
trap. The non-detection of CN constrains the C/O ratio both inside and outside
the dust trap to be if all nitrogen initially starts as N and , consistent with the Solar value, if (part of) the nitrogen initially
starts as N or NH.Comment: Accepted for publication in Astronomy and Astrophysic
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