Добірка наукової літератури з теми "Too-few-too-bright"

Instantaneous, coincident, footprint-level satellite observations of cloud properties and radiation taken during austral summer over the Southern Ocean are used to study relationships between clouds and large-scale meteorology. Cloud properties are very sensitive to the strength of vertical motion in the midtroposphere, and low-cloud properties are sensitive to estimated inversion strength, low-level temperature advection, and sea surface temperature. These relationships are quantified. An index for the meteorological anomalies associated with midlatitude cyclones is presented, and it is used to reveal the sensitivity of clouds to the meteorology within the warm and cold sectors of cyclones. The observed relationships between clouds and meteorology are compared to those in the Community Atmosphere Model, version 5 (CAM5), using satellite simulators. Low clouds simulated by CAM5 are too few, are too bright, and contain too much ice. In the cold sector of cyclones, the low clouds are also too sensitive to variations in the meteorology. When CAM5 is coupled with an updated boundary layer parameterization known as Cloud Layers Unified by Binormals (CLUBB), bias in the ice content of low clouds is dramatically reduced. More generally, this study demonstrates that examining the instantaneous time scale is a powerful approach to understanding the physical processes that control clouds and how they are represented in climate models. Such an evaluation goes beyond the cloud climatology and exposes model bias under various meteorological conditions.

In China, Jane Austen has undergone an amazing metamorphosis from an obscure foreign writer disregarded or disapproved of for a long period to a great novelist highly acclaimed and fully acknowledged. Only recent years have seen the publication of a few scholarly articles on the reception trajectories of Austen in the Chinese academic world. This article revisits the issue, particularly the reception of Austen in early modern China from a canonical perspective. During the first major wave of literary translation, Austen was absent in the translation projects of dominant male translators, especially in Lin Shu’s choice. It was not because of their gender discrimination as generally considered, but because of their lack of canon consciousness. The literary light of Austen, too bright and too sparkling to ignore, was finally shed upon the Chinese land, but her canonical place was not instantly recognized. The wartime translators’ efforts to render Pride and Prejudice into Chinese reflect the difficulty in the making of a canonical Austen under very different historical circumstances.

AbstractFabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

Fifty years ago, in December 1937, Manfred von Ardenne submitted his first paper on the scanning electron microscope (SEM) to Zeitschrift für Physik. Moreover his eightieth birthday was on January 20th this year and it is therefore now very appropriate that we should remember the great contribution he made to the subject by that mainly theoretical paper and by the one he published a few months later on the practical realisation of the first scanning transmission electron microscope (STEM); both papers have been frequently cited in the literature. Von Ardenne designed a two-lens microscope and calculated the current in a 10nm focussed spot to be 10-12A; he also discussed how the detector should be arranged to give bright and dark field images from a transparent specimen and secondary electron images from a solid specimen. Unfortunately, at that time the only device available to him for amplifying such small currents was the thermionic valve and he quickly realised that the noise level would be much too high.

AbstractUsing information from the A-Train satellites, the properties and radiative effects of eastern Pacific Ocean boundary layer clouds are evaluated in the Community Atmosphere Model, version 5 (CAM5), from the summer of 2007 and 2008. The cloud microphysical properties are inferred using measurements from CloudSat and CALIPSO (CC) that are then used to calculate the broadband radiative flux profiles. Accounting appropriately for sampling differences between the measurements and the simulation, evidence of the “too few, too bright” low cloud bias is found in CAM5. Single-layer low clouds have a frequency of occurrence of 42% from CC, as compared with just 29% in CAM5, and the averaged cloud radiative kernel (CRK) for the model shows stronger cooling. For stratocumulus in particular, the cooling in the model CRK is larger by a factor of 2 relative to the observations, implying an overly sensitive tropical low cloud feedback. Differences in the day/night occurrence of stratocumulus help to explain some of the difference in the CRK. The cloud-type microphysics for liquid clouds is represented reasonably well by the model, with a tendency for smaller water paths and smaller effective radii. Overall, the occurrence and CRK have partially compensating errors such that the net cooling at the top of the atmosphere for eastern Pacific low clouds is −43 W m−2 in CAM5, as compared with −32 W m−2 from CC. The cooling effect in the model is accomplished by fewer low clouds with a narrower range of properties, as compared with more clouds with a broader range of properties in the observation-based dataset.

Abstract The SPitzer InfraRed Intensive Transients Survey (SPIRITS) searched for luminous infrared (IR) transients and variables in nearly 200 nearby galaxies from 2014 to 2019, using the warm Spitzer telescope at 3.6 and 4.5 μm. Among the SPIRITS variables are IR-bright objects that are undetected in ground-based optical surveys. We classify them as (1) transients, (2) periodic variables, and (3) irregular variables. The transients include eSPecially Red Intermediate-luminosity Transient Events (SPRITEs), having maximum luminosities fainter than supernovae, red IR colors, and a wide range of outburst durations (days to years). Here we report deep optical and near-IR imaging with the Hubble Space Telescope (HST) of 21 SPIRITS variables. They were initially considered SPRITE transients, but many eventually proved instead to be periodic or irregular variables as more data were collected. HST images show most of these cool and dusty variables are associated with star-forming regions in late-type galaxies, implying an origin in massive stars. Two SPRITEs lacked optical progenitors in deep preoutburst HST images; however, one was detected during eruption at J and H, indicating a dusty object with an effective temperature of ∼1050 K. One faint SPRITE turned out to be a dusty classical nova. About half the HST targets proved to be periodic variables, with pulsation periods of 670–2160 days; they are likely dusty asymptotic-giant-branch (AGB) stars with masses of ∼5–10 M ⊙. A few of them were warm enough to be detected in deep HST frames, but most are too cool. Out of six irregular variables, two were red supergiants with optical counterparts in HST images; four were too enshrouded for HST detection.

The trend about producing and reading graphic novels has grown since the late twentieth century. These books with comic backgrounds seem to have a miraculous energy. They have been even appealing to unenthusiastic readers. They tempt people of different age groups, races and genders. They are also used for teaching ESL courses, e-learning activities, designing reality games, and teaching creative writing. If you talk to its followers, you may get the feedback that graphic novels can fulfil your demands and dreams from writing your assignments to taking you to the moon. Although many researchers have investigated the benefits of graphic novels, many faculties and librarians are still reluctant to include graphic novels in their curricula. Perhaps it is simply the attitude of many teachers and librarians that graphic novels look like a comic book, and simply are not “real” books. They have too few words, too many pictures, and lack quality to be seriously considered as literature. In the following, I, Ruzbeh Babaee, did an interview with Distinguished Professor Frederick Luis Aldama on realities of graphic novels.Aldama is a distinguished scholar and Professor of English at The Ohio State University, United States. In the departments of English and Spanish & Portuguese he is involved in teaching courses on US Latino and Latin American cultural phenomena, literature, film, music, video games, and comic books. He has founded and directed the White House Hispanic Bright Spot awarded LASER/Latino and Latin American Space for Enrichment Research. Professor Aldama won the Ohio Education Summit Award for Founding & Directing LASER in 2016. In April 2017, Aldama was awarded OSU’s Alumni Award for Distinguished Teaching and inducted into the Academy of Teaching. He is the author, co-author, and editor of 30 books, including his first book of fiction/graphic fiction, Long Stories Cut Short: Fictions from the Borderlands.

In this paper, I discuss the observational quantities that are useful for judging the successes and failures of current massive star evolutionary theory. The galaxies of the Local Group can serve as important laboratories for providing these diagnostics, as their metallicities vary by a factor of ten. We find that the evolutionary tracks do a good job of matching the distribution of stars in the H-R diagram during the main-sequence phase. However, none of the models produce RSGs that are as cool and as bright as what is observed. The relative number of WC and WN stars is a strong function of metallicity, and the Padova and Geneva ‘normal mass-loss’ models do a reasonably good job of matching the observations at low metallicities, but predict too few WCs at higher metallicity. The ‘enhanced’ mass-loss models of the Geneva group do not match the observations at all. New data is providing excellent statistics on the number of RSGs in these nearby galaxies, and the number ratio of RSGs to WRs is also an extremely sensitive function of metallicity. None of the models reproduce the trend of the RSG/WR ratio with metallicity.

AbstractThis contribution summarises the first characterisation of the 12 μm warm dust (“exo-Zodi”) luminosity function around Sun-like stars, focussing on the dustiest systems that can be identified by the WISE mission (Kennedy & Wyatt 2013). We use the sample of main-sequence stars observed by Hipparcos within 150pc as an unbiased sample, and report the detection of six new warm dust candidates. The ages of five of these new sources are unknown, meaning that they may be sites of terrestrial planet formation or rare analogues of other old warm dust systems. We show that the dustiest old (> Gyr) systems such as BD+20 307 are 1 in 10,000 occurrences. Bright warm dust is much more common around young (<120 Myr) systems, with a ~1% occurrence rate. We show that a two component in situ model where all stars have initially massive warm disks and in which warm debris is also generated at some random time along the stars' main-sequence lifetime, perhaps due to a collision, can explain the observations. However, if all stars only have initially massive warm disks these would not be visible at Gyr ages, and random collisions on the main-sequence are too infrequent to explain the high disk occurrence rate for young stars. That is, neither component can explain the observations on their own. Despite these conclusions, we cannot rule out an alternative dynamical model in which comets are scattered in from outer regions because the distribution of systems with the appropriate dynamics is unknown. Our in situ model predicts that the fraction of stars with exo-Zodi bright enough to cause problems for future exo-Earth imaging attempts is at least roughly 10%, and is higher for populations of stars younger than a few Gyr. This prediction of roughly 10% also applies to old stars because bright systems like BD+20 307 imply a population of fainter systems that were once bright, but are now decaying through fainter levels. Our prediction should be strongly tested by the Large Binocular Telescope Interferometer, which will provide valuable constraints and input for more detailed evolution models. A detection fraction lower than our prediction could indicate that the hot dust in systems like BD+20 307 has a cometary origin due to the quirks of the planetary dynamics. Population models of comet delivery need to be developed to help distinguish between different possible origins of warm dust.

Dans cette thèse on tente de réduire le biais “Too Few, Too Bright” partagé par la plupart des GCMs qui tendent à sous-estimer la couverture des nuages bas et à sur-estimer leur épaisseur optique. On travaille ainsi sur deux aspects de la représentation des nuages bas dans LMDz6. Sous-maille : On introduit une paramétrisation pour distinguer les fractions nuageuses volumiques CFvol et surfaciques CFsurf au sein des mailles du GCM, tout en recalibrant le calcul de l’eau condensée qc en prenant en compte l’épaisseur des mailles jusqu’alors négligée. Cette étape permet : -de diminuer l’épaisseur optique des nuages bas par la prise en compte de l’épaisseur des mailles dans le calcul de qc -d’augmenter la fraction nuageuse vue par le schéma de rayonnement qui reçoit CFsurf au lieu de CFvol Inter-maille : On propose une nouvelle paramétrisation de la longueur de décorrélation du schéma de recouvrement exponentiel-aléatoire, permettant d'évaluer la manière dont se recouvrent les nuages indépendamment dans chaque colonne atmosphérique, tout en prenant en compte le cisaillement de vent et en s’adaptant à des choix de modélisation comme la résolution verticale du GCM. On évalue les impacts radiatifs de ces paramétrisations avec le simulateur COSP2 dans lequel nous implémentons le cloud-generator du code radiatif ECRad. Sur nos diagnostiques, on observe : -une diminution des zones peu couvertes et très réfléchissantes -une augmentation des zones peu couvertes et peu réfléchissantes -une augmentation des zones à couverture et réflectance intermédiaire Ces nouvelles paramétrisations ont ainsi tendance à réduire le biais “Too Few, Too Bright” au dessus des océans tropicaux dans LMDz6
In this thesis we intent to reduce the "Too Few, Too Bright" bias shared by most GCMs, that tend to underestimate the low-cloud cover and overestimate its optical depth. We work on two aspects of the low-clouds representation in LMDz6. Sub-grid Scale: We introduce a parametrisation to distinguish cloud fractions by volume CFvol and by surface CFsurf inside GCM grid boxes, and we recalibrate the calculation of condensed water by taking into account the depth of the grid boxes that use to be neglected. This step allows: -to reduce the optical depth of clouds by taking into account the depth of grid boxes in the calculation of qc -to increase the cloud fraction seen by the radiation scheme, that receive CFsurf instead of CFvol Inter-grid Scale: We propose a new parametrisation of the decorrelation length of the exponential-random overlap scheme, that allows evaluating the overlap of clouds independently in each atmospheric column, while taking into account wind shear and being adaptive to modelling choices such as the vertical resolution of the GCM. We evaluate the radiative impacts of these parametrisations with the COSP2 simulator package in which we implement the cloud-generator of the radiative code ECRad. Our diagnostics show: -a reduction of the low-covered and highly-reflective areas -an increase of the low-covered and low-reflective areas -and increase of the mid-covered and mid-reflective areas These new parametrisations then tend to reduce the "Too Few, Too Bright" bias over tropical ocean in LMDz6

This chapter stands at the midpoint of the “bright side” of this book. Its oppositional partner on the “dark side” is chapter 3 on chemical arsenals. Thus, education and war making present a core contrast in the uses of chemical knowledge in the movies. We have only to think of the closed world of Dr. Mabuse, symbolized so well by the writings in his notebook, as described in chapter 3. His inward, secret scribblings speak of outward, villainous purposes. In juxtaposition, the writing on the blackboards of this chapter’s movies is exposed; it is to be seen. This writing represents the open, cool, dispassionate transmission of facts in symbolic chemical language. But a little something more has slipped through in this section’s movie example. When we read its blackboard, we see the explosive nature of knowledge itself. “You have to see and read a movie at the same time,” says Harvard professor Tom Conley, whose creative film analyses leave readers with an appreciation of just how rich cinematic art can be (Savisky 2006). In his book Film Hieroglyphs, Conley considers writing as it appears in movies. He shows it is often an incidental and uncontrollable element that inserts itself into our movie-watching experience, leaving us to ponder nonnarrative written material observed on the movie sets. Conley calls the points where story, image, and writing are at odds with one another “ruptures.” Graphically interrupting the flow of the moving image, these points provide “slide areas” for analysis and new insights (Conley 1991). This section examines chemical notations appearing in our movie examples, and how they provide opportunities for an enhanced reading of these movies. The blackboard in The Affairs of Dobie Gillis (1953), a musical campus comedy, ruptures the movie like no other blackboard in movie history. But first, let us set the scene. Pansy Hammer (Debbie Reynolds) attends Grainbelt University to “work, work, work.” As she and her lab mates begin their first laboratory exercise, she gleefully tells them she really likes chemistry. After a few moments, the professor announces, “Don’t let the bubbles come too fast” and then Hammer’s experiment explodes.

A few months after Alan Turing’s tragically early death, in 1954, his colleague Geoffrey Jefferson (professor of neurosurgery at Manchester University) wrote what might serve as Turing’s epitaph: Alan in whom the lamp of genius burned so bright—too hot a flame perhaps it was for his endurance. He was so unversed in worldly ways, so childlike it sometimes seemed to me, so unconventional, so non-conform[ing] to the general pattern. His genius flared because he had never quite grown up, he was I suppose a sort of scientific Shelley. After his short but brilliant career Alan Mathison Turing’s life ended 15 days short of his fortysecond birthday.2 His ideas lived on, however, and at the turn of the millennium Time magazine listed him among the twentieth-century’s one hundred greatest minds, alongside the Wright brothers, Albert Einstein, DNA busters Crick and Watson, and Alexander Fleming, the discoverer of penicillin.3 Turing’s achievements during his short lifetime were legion. Best known as the mathematician who broke some of Nazi Germany’s most secret codes, Turing was also one of the ringleaders of the computer revolution. Today, all who click, tap, or touch to open are familiar with the impact of his ideas. We take for granted that we use the same slab of hardware to shop, manage our finances, type our memoirs, play our favourite music and videos, and send instant messages across the street or around the world. In an era when ‘computer’ was the term for a human clerk who did the sums in the back office of an insurance company or science lab, Turing envisaged a ‘universal computing machine’, able to do anything that a programmer could pin down in the form of a series of instructions. He could not have foreseen this at the time, but his universal computing machine changed the way we live: it eventually caught on like wildfire, with sales of personal computers now hovering around the million a day mark. Turing’s universal machine transported us into a world where many young people have never known life without the Internet.

On an ordinary spring morning in 1852, Ben Major and his wife Lucy are eating breakfast when they are interrupted by a frantic messenger. Ben’s only sister, Eliza Ann Davenport, is gravely ill with cholera. Ben rushes to her home, where he tries all his various botanical treatments for cholera, but to no avail. Eliza Ann dies, and within a short time it is clear that two of her sons and Ben are sick, too. All three of them die within a few days. With the deaths of Tolbert and Ben—six months apart—the remarkable correspondence between Bassa Cove and Walnut Grove ends, but the final letter from Liberia is not the last interaction between the Liberian colonists and the American Majors. Years later, Wesley Harlan travels from Liberia to pay his respects at Ben Major’s grave in Illinois.

Tho’ the child could not describe the gentleman’s person who handed his sister into the post-chaise, yet my suspicions fell entirely upon our young landlord, whose character for such intrigues was but too well known. I therefore directed my steps towards Thornhill-castle, resolving to upbraid him, and, if possible, to bring back my daughter: but before I had reached his seat, I was met by one of my parishioners, who said he saw a young lady resembling my daughter in a post-chaise with a gentleman, whom, by the description, I could only guess to be Mr. Burchell, and that they drove very fast. This information, however, did by no means satisfy me. I therefore went to the young ‘Squire’s, and though it was yet early, insisted upon seeing him immediately: he soon appeared with the most open familiar air, and seemed perfectly amazed at my daughter’s elopement, protesting upon his honour that he was quite a stranger to it. I now therefore condemned my former suspicions, and could turn them only on Mr. Burchell, who I recollected had of late several private conferences with her: but the appearance of another witness left me no room to doubt of his villainy, who averred, that he and my daughter were actually gone towards the wells, about thirty miles off, where there was a great deal of company. Being driven to that state of mind in which we are more ready to act precipitately than to reason right, I never debated with myself, whether these accounts might not have been given by persons purposely placed in my way, to mislead me, but resolved to pursue my daughter and her fancied deluder thither. I walked along with earnestness, and enquired of several by the way; but received no accounts, till entering the town, I was met by a person on horseback, whom I remembered to have seen at the ‘Squire’s, and he assured me that if I followed them to the races,* which were but thirty miles farther, I might depend upon overtaking them; for he had seen them dance there the night before, and the whole assembly seemed charmed with my daughter’s performance. Early the next day I walked forward to the races, and about four in the afternoon I came upon the course. The company made a very brilliant appearance, all earnestly employed in one pursuit, that of pleasure; how different from mine, that of reclaiming a lost child to virtue! I thought I perceived Mr. Burchell at some distance from me; but, as if he dreaded an interview, upon my approaching him, he mixed among a crowd, and I saw him no more. I now reflected that it would be to no purpose to continue my pursuit farther, and resolved to return home to an innocent family, who wanted my assistance. But the agitations of my mind, and the fatigues I had undergone, threw me into a fever, the symptoms of which I perceived before I came off the course. This was another unexpected stroke, as I was more than seventy miles distant from home: however, I retired to a little ale-house by the road-side, and in this place, the usual retreat of indigence and frugality, I laid me down patiently to wait the issue of my disorder. I languished here for near three weeks; but at last my constitution prevailed, though I was unprovided with money to defray the expences of my entertainment. It is possible the anxiety from this last circumstance alone might have brought on a relapse, had I not been supplied by a traveller, who stopt to take a cursory refreshment. This person was no other than the philanthropic bookseller in St. Paul’s church-yard, who has written so many little books for children: he called himself their friend; but he was the friend of all mankind. He was no sooner alighted, but he was in haste to be gone; for he was ever on business of the utmost importance, and was at that time actually compiling materials for the history of one Mr. Thomas Trip.* I immediately recollected this good-natured man’s red pimpled face; for he had published for me against the Deuterogamists* of the age, and from him I borrowed a few pieces, to be paid at my return. Leaving the inn, therefore, as I was yet but weak, I resolved to return home by easy journies of ten miles a day. My health and usual tranquillity were almost restored, and I now condemned that pride which had made me refractory to the hand of correction. Man little knows what calamities are beyond his patience to bear till he tries them; as in ascending the heights of ambition, which look bright from below, every step we rise shews us some new and gloomy prospect of hidden disappointment; so in our descent from the summits of pleasure, though the vale of misery below may appear at first dark and gloomy, yet the busy mind, still attentive to its own amusement, finds as we descend something to flatter and to please. Still as we approach, the darkest objects appear to brighten, and the mental eye becomes adapted to its gloomy situation.