Eclipse Research Articles

Weighing Uranus’ Moon Cressida with the η Ring

Abstract The η ring is one of the narrow rings of Uranus, consisting of a dense core that is 1–2 km wide and a diffuse outer sheet spanning about 40 km. Its dense core lies just exterior to the 3:2 Inner Lindblad Resonance of the small moon Cressida. We fit the η ring radius residuals and longitudes from a complete set of both ground-based and Voyager stellar and radio occultations of the Uranian rings spanning 1977–2002. We find variations in the radial position of the η ring that are likely generated by this resonance, and take the form of a 3-lobed structure rotating at an angular rate equal to the mean motion of the moon Cressida. The amplitude of these radial oscillations is 0.667 ± 0.113 km, which is consistent with the expected shape due to the perturbations from Cressida. The magnitude of these variations provides the first measurement of the mass and density of the moon Cressida ( kg and g cm−3) or, indeed, any of Uranus’ small inner moons. A better grasp of inner Uranian satellite masses will provide another clue to the composition, dynamical stability, and history of Uranus’ tightly packed system of small moons.

Influence of CT value division on dose calculation in treatment planning

Objective To divide computed tomography (CT) values into different ranges and investigate the influence of CT value division on dose calculation, and to propose a method to combine magnetic resonance imaging (MRI) with assigned CT values. Methods Ten CT images each were collected from patients with head and neck, chest, and pelvic tumors. Random sampling was performed for the CT values of main tissues or organs at the three parts, and then the mean CT value of each tissue or organ was calculated to divide the CT values into different ranges. A virtual phantom was built in the Varian Eclipse treatment planning system, and for the prescribed dose of 100 cGy, the machine output was recorded at different CT values. The influence of different CT value ranges on dose calculation was analyzed. The treatment plans of intensity-modulated radiotherapy were selected from 5 cervical cancer patients, and new CT values were assigned to the planning target volume (PTV) and organs at risk to obtain new CT images. The plans were transferred to the new CT images and compared with the results on the original CT images in terms of dosimetric parameters. Results After dividing the CT values into different ranges and verifying the results in dose calculation, the CT values corresponding to different human tissues or organs were -100 to 100 HU. The influence of CT value variation on dose calculation was within 3%. In the same treatment plan, there were small differences in dosimetric parameters between new CT images and original CT images. Dmax, Dmean, D98%, D95%, D5%, and D2% of PTV were all below 3%, and Dmax and Dmean of the bladder, rectum, small intestine, femoral head, and bone marrow were below 2%. Conclusions The influence of CT value division on dose calculation in the treatment planning for pelvic tumors is acceptable, so it can be used in combination with MRI. Key words: Tomograpy, X-ray computed; Dose calculation; Treatment planning system; Magnetic resonance image

Perception, cognition and reasoning about shadows

The way we categorize shadows interfaces with the way we perceive them (Casati, 2017). Some thought experiments such as the Yale Problem (Todes & Daniels, 1975), the Intersecting Eclipses Problem (...

The Structure of Chariklo’s Rings from Stellar Occultations

Abstract Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo’s system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the ±3.3 km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from ∼5 to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2R’s edges is available. A upper limit of ∼20 m is derived for the equivalent width of narrow (physical width km) rings up to distances of 12,000 km, counted in the ring plane.

Volcanic views, stalking storks and the ephemeral eclipse

Volcanic views, stalking storks and the ephemeral eclipse

Lunar occultations of Aldebaran and other late-type stars observed from Devasthal

We report on lunar occultations of Aldebaran (α Tau) and other ten, mostly late-type, stars observed with the Devasthal 1.3-m telescope. We derive a detailed brightness profile for Aldebaran, confirming the presence of asymmetries already recently described in a related work. We test the origin of such asymmetries by means of simulations of the effect of scintillation on the reconstructed profiles. We also derive angular diameters for two M giants, Z Cnc and SAO 161635, which we discuss in the context of previous determinations. We find first-time companions around two other stars, SAO 161665 and WZ Psc, and we detect one more previously known binary, SAO 94060. This is the first systematic effort to observe lunar occultations events at this facility, and demonstrates the capability to carry out milliarcsecond-level investigations on sources down to ≈ 9 mag. We plan to continue this routine program in the coming years, eventually utilizing also the 3.6 m DOT telescope recently erected at Devasthal for deeper sensitivity and higher accuracy.

Enceladus Plume Structure and Time Variability: Comparison of Cassini Observations.

During three low-altitude (99, 66, 66 km) flybys through the Enceladus plume in 2010 and 2011, Cassini's ion neutral mass spectrometer (INMS) made its first high spatial resolution measurements of the plume's gas density and distribution, detecting in situ the individual gas jets within the broad plume. Since those flybys, more detailed Imaging Science Subsystem (ISS) imaging observations of the plume's icy component have been reported, which constrain the locations and orientations of the numerous gas/grain jets. In the present study, we used these ISS imaging results, together with ultraviolet imaging spectrograph stellar and solar occultation measurements and modeling of the three-dimensional structure of the vapor cloud, to constrain the magnitudes, velocities, and time variability of the plume gas sources from the INMS data. Our results confirm a mixture of both low and high Mach gas emission from Enceladus' surface tiger stripes, with gas accelerated as fast as Mach 10 before escaping the surface. The vapor source fluxes and jet intensities/densities vary dramatically and stochastically, up to a factor 10, both spatially along the tiger stripes and over time between flyby observations. This complex spatial variability and dynamics may result from time-variable tidal stress fields interacting with subsurface fissure geometry and tortuosity beyond detectability, including changing gas pathways to the surface, and fluid flow and boiling in response evolving lithostatic stress conditions. The total plume gas source has 30% uncertainty depending on the contributions assumed for adiabatic and nonadiabatic gas expansion/acceleration to the high Mach emission. The overall vapor plume source rate exhibits stochastic time variability up to a factor ∼5 between observations, reflecting that found in the individual gas sources/jets. Key Words: Cassini at Saturn—Geysers—Enceladus—Gas dynamics—Icy satellites. Astrobiology 17, 926–940.

Alcohol Misuse Is on the Rise in the U.S.

The current preoccupation with opioid misuse could eclipse another, more widespread, epidemic: alcohol misuse. In two nationally representative surveys

Particle sizes in Saturn's rings from UVIS stellar occultations 1. Variations with ring region

The Cassini spacecraft's Ultraviolet Imaging Spectrograph (UVIS) includes a high speed photometer (HSP) that has observed stellar occultations by Saturn's rings with a radial resolution of ∼10 m. In the absence of intervening ring material, the time series of measurements by the HSP is described by Poisson statistics in which the variance equals the mean. The finite sizes of the ring particles occulting the star lead to a variance that is larger than the mean due to correlations in the blocking of photons due to finite particle size and due to random variations in the number of individual particles in each measurement area. This effect was first exploited by Showalter and Nicholson (1990) with the stellar occultation observed by Voyager 2. At a given optical depth, a larger excess variance corresponds to larger particles or clumps that results in greater variation of the signal from measurement to measurement. Here we present analysis of the excess variance in occultations observed by Cassini UVIS. We observe differences in the best-fitting particle size in different ring regions. The C ring plateaus show a distinctly smaller effective particle size, R, than the background C ring, while the background C ring itself shows a positive correlation between R and optical depth. The innermost 700 km of the B ring has a distribution of excess variance with optical depth that is consistent with the C ring ramp and C ring but not with the remainder of the B1 region. The Cassini Division, while similar to the C ring in spectral and structural properties, has different trends in effective particle size with optical depth. There are discrete jumps in R on either side of the Cassini Division ramp, while the C ring ramp shows a smooth transition in R from the C ring to the B ring. The A ring is dominated by self-gravity wakes whose shadow size depends on the occultation geometry. The spectral “halo” regions around the strongest density waves in the A ring correspond to decreases in R. There is also a pronounced dip in R at the Mimas 5:3 bending wave corresponding to an increase in optical depth there, suggesting that at these waves small particles are liberated from clumps or self-gravity wakes leading to a reduction in effective particle size and an increase in optical depth.

Measuring the Radius and Mass of Planet Nine

Batygin & Brown () suggested the existence of a new planet in our solar system that is supposed to be responsible for the perturbation of eccentric orbits of small outer bodies. The main challenge now is to detect and characterize this putative body. Here, we investigate the principles of the determination of its physical parameters, mainly its mass and radius. For that purpose, we concentrate on two methods: stellar occultations and gravitational microlensing effects (amplification, deflection, and time delay). We estimate the main characteristics of a possible occultation or gravitational effects: flux variation of a background star, duration, and probability of occurrence. We also investigate the additional benefits of direct imaging and of an occultation.

Howling at the Moon with Eclipse Enthusiasts

From the reporters who stared at goats to poets who tweeted haiku, eclipse watchers across the nation flaunted their weird.

Umbreon or Antumbra? Can you tell the difference between eclipse terms and Pokémon lingo?

Umbreon or Antumbra? Can you tell the difference between eclipse terms and Pokémon lingo?

Supramolecular architectures in the salt trimethoprimium ferrocene-1-carboxylate and the cocrystal 4-amino-5-chloro-2,6-dimethylpyrimidine-ferrocene-1-carboxylic acid (1/1).

In the salt trimethoprimium ferrocenecarboxylate [systematic name: 2,4-diamino-5-(3,4,5-trimethoxybenzyl)pyrimidin-1-ium ferrocene-1-carboxylate], (C14H19N4O3)[Fe(C5H5)(C6H4O2)], (I), of the antibacterial compound trimethoprim, the carboxylate group interacts with the protonated aminopyrimidine group of trimethoprim via two N-H...O hydrogen bonds, generating a robust R22(8) ring motif (heterosynthon). However, in the cocrystal 4-amino-5-chloro-2,6-dimethylpyrimidine-ferrocene-1-carboxylic acid (1/1), [Fe(C5H5)(C6H5O2)]·C6H8ClN3, (II), the carboxyl-aminopyrimidine interaction [R22(8) motif] is absent. The carboxyl group interacts with the pyrimidine ring via a single O-H...N hydrogen bond. The pyrimidine rings, however, form base pairs via a pair of N-H...N hydrogen bonds, generating an R22(8) supramolecular homosynthon. In salt (I), the unsubstituted cyclopentadienyl ring is disordered over two positions, with a refined site-occupation ratio of 0.573 (10):0.427 (10). In this study, the two five-membered cyclopentadienyl (Cp) rings of ferrocene are in a staggered conformation, as is evident from the C...Cg...Cg...C pseudo-torsion angles, which are in the range 36.13-37.53° for (I) and 22.58-23.46° for (II). Regarding the Cp ring of the minor component in salt (I), the geometry of the ferrocene ring is in an eclipsed conformation, as is evident from the C...Cg...Cg...C pseudo-torsion angles, which are in the range 79.26-80.94°. Both crystal structures are further stabilized by weak π-π interactions.

Eclipse science: Discoveries in the Moon’s shadow

Eclipse science: Discoveries in the Moon’s shadow

3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D~100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (~34% of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptive-optics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (343 deg,+47 deg), and volume-equivalent diameter (193 +/- 6km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 +/- 0.64 g.cm-3 , in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ~40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt.

Organized Autotelescopes for Serendipitous Event Survey (OASES): Design and performance

Abstract Organized Autotelescopes for Serendipitous Event Survey (OASES) is an optical observation project that aims to detect and investigate stellar occultation events by kilometer-sized trans-Neptunian objects (TNOs). In this project, multiple low-cost observation systems for wide-field and high-speed photometry were developed in order to detect rare and short-timescale stellar occultation events. The observation system consists of commercial off-the-shelf 0.28 m aperture f/1.58 optics providing a 2${^{\circ}_{.}}$3 × 1${^{\circ}_{.}}$8 field of view. A commercial CMOS camera is coupled to the optics to obtain full-frame imaging with a frame rate greater than 10 Hz. As of 2016 September, this project exploits two observation systems, which are installed on Miyako Island, Okinawa, Japan. Recent improvements in CMOS technology in terms of high-speed imaging and low readout noise mean that the observation systems are capable of monitoring ∼2000 stars in the Galactic plane simultaneously with magnitudes down to V ∼ 13.0, providing ∼20% photometric precision in light curves with a sampling cadence of 15.4 Hz. This number of monitored stars is larger than for any other existing instruments for coordinated occultation surveys. In addition, a precise time synchronization method needed for simultaneous occultation detection is developed using faint meteors. The two OASES observation systems are executing coordinated monitoring observations of a dense stellar field in order to detect occultations by kilometer-sized TNOs for the first time.

Records of Sighting of Halley's Comet in the 1531 Apparition and an Eclipse in Guru Nanak's References

Two celestial occurrences find place in the incidents related to the great poet - saint Guru Nanak (1469-1539 CE), founder of Sikhism, or in his teachings. The first one referred to as lamma tara (long star) figures in a hymn in the Sri Guru Granth Sahib and the other is a solar eclipse that occurred while Guru Nanak was visiting Kurukshetra. I conclude that the long star must be Halley's Comet in its apparition in 1531. This is significant considering that the record of sighting of a comet in an Indian scripture has so far not been identified. Further, among the many eclipses occurring during the relevant period of 1498-1521, that of 13 January 1507 is the most probable one. The eclipse is historical in the sense that it is the first observational record to be depicted in an Indian mural.

Incorporation of dihydroartemisinin into memantine through a propriate spacer to make hybrid with enhanced effects to protect PC12 cells from corticosterone-caused impairments

Ten memantine(Mema)-dihydroartemisinin(DHA) ligands were designed and synthesized. Three types of isomers including α, β, and a defined γ isomer were found in each intermediates(1a—1e). Type γ isomer was firstly reported here and confirmed as a less stable eclipsed conformation. The bonding of Mema with DHA through different carbon chains generally makes the new entities more cytotoxic than either Mema or artemisinin(Arte). The β Mema/DHA ligands are a little bit more cytotoxic than α ligands. By applying corticosterone(Cort)-impaired PC12 cells models, it was found that Mema and those ligands with more than 3 carbon chains showed weak or no neuro-protective activities against the insults. However, two ligands, 2a(β) and 2b(β) showed better effects than either Arte or their combination(Mema/Arte in 1:1 molar ratio) at a dose of 5 µmol/L. Furthermore, ligands 2a(β), 2b(β) and 2c(β) were confirmed as mild N-methyl-D-aspartate(NMDA) antagonists, and their corresponding α isomers are weak NMDA antagonists. All the data indicate that the bonding of Mema/DHA in compacted β conformation mode results in enhanced effects against Cort-induced insults in PC12 cells and might reverse memantine as an anti-depression NMDA antagonist.

Improved pointing information for SCIAMACHY from in-flight measurements of the viewing directions towards sun and moon

Abstract. The SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY (SCIAMACHY) on Envisat (2002–2012) performed nadir, limb, solar/lunar occultation and various monitoring measurements. The pointing information of the instrument is determined by the attitude information of the Envisat platform with its star trackers together with the encoder readouts of both the azimuth and the elevation scanner of SCIAMACHY. In this work, we present additional sources of attitude information from the SCIAMACHY measurements itself. The basic principle is the same as used by the star tracker: we measure the viewing direction towards celestial objects, i.e. sun and moon, to detect possible mispointings. In sun over limb port observations, we utilise the vertical scans over the solar disk. In horizontal direction, SCIAMACHY's sun follower device (SFD) is used to adjust the viewing direction. Moon over limb port measurements use for both the vertical and the horizontal direction the adjustment by the SFD. The viewing direction is steered towards the intensity centroid of the illuminated part of the lunar disk. We use reference images from the USGS Robotic Lunar Observatory (ROLO) to take into account the inhomogeneous surface and the variations by lunar libration and phase to parameterise the location of the intensity centroid from the observation geometry. Solar observations through SCIAMACHY's so-called sub-solar port (with a viewing direction closely to zenith) also use the SFD in the vertical direction. In the horizontal direction the geometry of the port defines the viewing direction. Using these three type of measurements, we fit improved mispointing parameters by minimising the pointing offsets in elevation and azimuth. The geolocation of all retrieved products will benefit from this; the tangent heights are especially improved. The altitudes assigned to SCIAMACHY's solar occultation measurements are changed in the range of −130 to −330 m, the lunar occultation measurements are changed in the range of 0 to +130 m and the limb measurements are changed in the range of −50 to +60 m (depending on season, altitude and azimuth angle). The horizontal location of the tangent point is changed by about 5 km for all measurements. These updates are implemented in version 9 of the SCIAMACHY Level 1b products and Level 2 version 7 (based on L1b version 9).

V2197 Cyg - A Semi-Detached Eclipsing Binary?

V2197 Cyg - A Semi-Detached Eclipsing Binary?