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Artículos de revistas sobre el tema "Ceti"

Autor: Grafiati

Publicado: 11 de marzo de 2023

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1

Zhang, Tong, Wenge Qiu, Hongtai Zhu, Xinlei Ding, Rui Wu y Hong He. "Promotion Effect of the Keggin Structure on the Sulfur and Water Resistance of Pt/CeTi Catalysts for CO Oxidation". Catalysts 12, n.º 1 (22 de diciembre de 2021): 4. http://dx.doi.org/10.3390/catal12010004.

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Developing a catalyst with high SO2 and H2O resistance to achieve high-performance CO oxidation for specific industrial applications is highly desirable. Here, three catalysts were prepared using cerium titanium composite oxide (CeTi), molybdophosphate with Keggin structure-modified CeTi (Keg-CeTi), and molybdophosphate without Keggin structure-modified CeTi (MoP-CeTi) as supports, and their sulfur and water resistance in CO oxidation were tested. The characterization of XRD, BET, SO2/H2O-DRIFTS, XPS, TEM, SEM, NH3/SO2-TPD, H2-TPR, and ICP techniques revealed that the high SO2 and H2O resistance of Pt/Keg-CeTi in CO oxidation was related to its stronger surface acidity, better reduction of surface cerium and molybdenum species, and lower SO2 adsorption and transformation compared to Pt/CeTi and Pt/MoP-CeTi.

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2

Nhung, Pham T., Do T. Hoai, Pham Tuan-Anh, Pierre Darriulat, Pham N. Diep, Nguyen B. Ngoc y Tran T. Thai. "Mira Ceti, Atypical Archetype". Astrophysical Journal 927, n.º 2 (1 de marzo de 2022): 169. http://dx.doi.org/10.3847/1538-4357/ac4f61.

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Abstract With the aim of unraveling the complexity of the morphokinematics of the circumstellar envelope (CSE) of Mira Ceti, we review, extend, and in some cases revisit Atacama Large Millimeter/submillimeter Array observations of the emission of the SiO(5–4) and CO(3–2) molecular lines. In addition, we present a detailed analysis of the optically thin 13CO(3–2) emission, which provides several important new results. In agreement with observations at infrared and visible wavelengths, we give evidence for the confinement and probably rotation of a dense gas volume within ∼50 au from the star and for a large SiO line width within ∼15 au. We show that the mass-loss process is episodic and takes the form of clumps having a very low SiO/CO abundance ratio compared with similar oxygen-rich long-period variables, probably a result of depletion on dust grains and photodissociation. We evaluate the mass-loss rate associated with the main clumps and compare it with values obtained from single-dish observations. We argue that the SiO emission observed in the southwestern quadrant is not related to the mechanism of generation of the nascent wind but to a mass ejection that occurred 11 years before the observations. We remark that Mira Ceti is not a good archetype in terms of its wind: models aiming at describing the very complex gas-dust chemistry in action in the CSE of oxygen-rich AGB stars may find it difficult to account for its peculiar features and small variations in the parameters deciding when and where mass loss can proceed significantly.

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3

Mukadam, Anjum S., Agnes Kim, Oliver Fraser, D. E. Winget, S. O. Kepler, D. J. Sullivan, D. Reaves et al. "Watching ZZ Ceti evolve". Journal of Physics: Conference Series 172 (1 de junio de 2009): 012074. http://dx.doi.org/10.1088/1742-6596/172/1/012074.

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4

Davison, NJ, MP Dagleish, EJ Dale, M. ten Doeschate, J. Muchowski, LL Perrett, M. Rocchi, AM Whatmore y AC Brownlow. "First confirmed reports of the isolation of Brucella ceti from a Risso’s dolphin Grampus griseus and a killer whale Orcinus orca". Diseases of Aquatic Organisms 145 (15 de julio de 2021): 191–95. http://dx.doi.org/10.3354/dao03612.

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Brucella ceti has been recovered from a number species of cetaceans worldwide over the last 25 yr. Here we report, for the first time, the recovery of B. ceti from a Risso’s dolphin Grampus griseus and a killer whale Orcinus orca. Recovery from an abdominal mass in the dolphin provides further evidence of the systemic pathogenic potential for B. ceti infection in cetaceans. The isolation of B. ceti ST23 (porpoise cluster) from a killer whale from a group known to eat other marine mammals raises the possibility of infection via ingestion. This report takes the number of cetacean species in UK coastal waters from which B. ceti has been isolated to 11 and highlights the value of routine, comprehensive and specific screening for significant pathogens such as Brucella sp. by strandings networks.

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5

Castanheira, B. G. y S. O. Kepler. "Seismological studies of ZZ Ceti stars - II. Application to the ZZ Ceti class". Monthly Notices of the Royal Astronomical Society 396, n.º 3 (1 de julio de 2009): 1709–31. http://dx.doi.org/10.1111/j.1365-2966.2009.14855.x.

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6

Angelucci, Clotilde Beatrice, Roberto Giacominelli-Stuffler, Marina Baffoni, Cristina Esmeralda Di Francesco, Gabriella Di Francesco, Ludovica Di Renzo, Manuela Tittarelli et al. "Cellular Prion Protein Expression in the Brain Tissue from Brucella ceti-Infected Striped Dolphins (Stenella coeruleoalba)". Animals 12, n.º 10 (19 de mayo de 2022): 1304. http://dx.doi.org/10.3390/ani12101304.

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Brucella ceti, a zoonotic pathogen of major concern to cetacean health and conservation, is responsible for severe meningo-encephalitic/myelitic lesions in striped dolphins (Stenella coeruleoalba), often leading to their stranding and death. This study investigated, for the first time, the cellular prion protein (PrPc) expression in the brain tissue from B. ceti-infected, neurobrucellosis-affected striped dolphins. Seven B. ceti-infected, neurobrucellosis-affected striped dolphins, found stranded along the Italian coastline (6) and in the Canary Islands (1), were investigated, along with five B. ceti-uninfected striped dolphins from the coast of Italy, carrying no brain lesions, which served as negative controls. Western Blot (WB) and immunohistochemistry (IHC) with an anti-PrP murine monoclonal antibody were carried out on the brain parenchyma of these dolphins. While PrPc IHC yielded inconclusive results, a clear-cut PrPc expression of different intensity was found by means of WB analyses in the brain tissue of all the seven herein investigated, B. ceti-infected and neurobrucellosis-affected cetacean specimens, with two dolphins stranded along the Italian coastline and one dolphin beached in Canary Islands also exhibiting a statistically significant increase in cerebral PrPc expression as compared to the five Brucella spp.-negative control specimens. The significantly increased PrPc expression found in three out of seven B. ceti-infected, neurobrucellosis-affected striped dolphins does not allow us to draw any firm conclusion(s) about the putative role of PrPc as a host cell receptor for B. ceti. Should this be the case, an upregulation of PrPc mRNA in the brain tissue of neurobrucellosis-affected striped dolphins could be hypothesized during the different stages of B. ceti infection, as previously shown in murine bone marrow cells challenged with Escherichia coli. Noteworthy, the inflammatory infiltrates seen in the brain and in the cervico-thoracic spinal cord segments from the herein investigated, B. ceti-infected and neurobrucellosis-affected striped dolphins were densely populated by macrophage/histiocyte cells, often harboring Brucella spp. antigen in their cytoplasm, similarly to what was reported in macrophages from mice experimentally challenged with B. abortus. Notwithstanding the above, much more work is needed in order to properly assess the role of PrPc, if any, as a host cell receptor for B. ceti in striped dolphins.

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7

Kepler, S. O. y B. G. Castanheira. "New pulsating ZZ ceti stars". Journal of Physics: Conference Series 172 (1 de junio de 2009): 012064. http://dx.doi.org/10.1088/1742-6596/172/1/012064.

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8

Blown, Eric James, John Kirkland, Claire McLachlan‐Smith, Jan McPherson y Bill Anderson. "CETI. Metaphor and universal language". Early Child Development and Care 55, n.º 1 (enero de 1990): 67–74. http://dx.doi.org/10.1080/0300443900550110.

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9

Szabados, L., L. L. Kiss y A. Derekas. "The anomalous Cepheid XZ Ceti". Astronomy & Astrophysics 461, n.º 2 (4 de octubre de 2006): 613–18. http://dx.doi.org/10.1051/0004-6361:20065690.

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10

Kanaan, A., S. O. Kepler y D. E. Winget. "The ZZ Ceti red edge". Astronomy & Astrophysics 389, n.º 3 (julio de 2002): 896–903. http://dx.doi.org/10.1051/0004-6361:20020485.

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11

Srivastava, R. K. "Period study of XY Ceti". Astrophysics and Space Science 150, n.º 1 (1988): 173–79. http://dx.doi.org/10.1007/bf00714160.

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12

Vauclair, G., N. Dolez, Fu Jian Ning, M. Chevreton, D. Homeier y D. Koester. "Surveys and the Discovery of New Variable White Dwarfs". International Astronomical Union Colloquium 176 (2000): 516–17. http://dx.doi.org/10.1017/s0252921100058681.

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13

De Gerónimo, F. C., L. G. Althaus, A. H. Córsico, A. D. Romero y S. O. Kepler. "Asteroseismology of ZZ Ceti stars with full evolutionary white dwarf models". Astronomy & Astrophysics 613 (mayo de 2018): A46. http://dx.doi.org/10.1051/0004-6361/201731982.

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Context. The thermally pulsing phase on the asymptotic giant branch (TP-AGB) is the last nuclear burning phase experienced by most low- and intermediate-mass stars. During this phase, the outer chemical stratification above the C/O core of the emerging white dwarf (WD) is built up. The chemical structure resulting from progenitor evolution strongly impacts the whole pulsation spectrum exhibited by ZZ Ceti stars, which are pulsating C/O core white dwarfs located on a narrow instability strip at Teff ~ 12 000 K. Several physical processes occurring during progenitor evolution strongly affect the chemical structure of these stars; those found during the TP-AGB phase are the most relevant for the pulsational properties of ZZ Ceti stars. Aims. We present a study of the impact of the chemical structure built up during the TP-AGB evolution on the stellar parameters inferred from asteroseismological fits of ZZ Ceti stars. Methods. Our analysis is based on a set of carbon–oxygen core white dwarf models with masses from 0.534 to 0.6463 M⊙ derived from full evolutionary computations from the ZAMS to the ZZ Ceti domain. We computed evolutionary sequences that experience different number of thermal pulses (TP). Results. We find that the occurrence or not of thermal pulses during AGB evolution implies an average deviation in the asteroseimological effective temperature of ZZ Ceti stars of at most 8% and on the order of ≲5% in the stellar mass. For the mass of the hydrogen envelope, however, we find deviations up to 2 orders of magnitude in the case of cool ZZ Ceti stars. Hot and intermediate temperature ZZ Ceti stars show no differences in the hydrogen envelope mass in most cases. Conclusions. Our results show that, in general, the impact of the occurrence or not of thermal pulses in the progenitor stars is not negligible and must be taken into account in asteroseismological studies of ZZ Ceti stars.

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14

Pfeiffer, B., G. Vauclair, N. Dolez, M. Chevreton, J. R. Fremy, G. Herpe, M. Barstow et al. "Observation of a Variable, ZZ Ceti White Dwarf: GD154". International Astronomical Union Colloquium 134 (1993): 201–4. http://dx.doi.org/10.1017/s0252921100014196.

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The ZZ Ceti stars form a class of variable white dwarfs: the hydrogen dominated atmosphere ones, which do pulsate in an instability strip in the effective temperature range 13000K-11500K. We know 22 such ZZ Ceti white dwarfs. Their variations are caused by nonradial g-mode pulsations with periods are in the range 100-1000 seconds.A subsample of the ZZ Ceti stars shows amplitude variations on time scales of the order of one month. These variations could be driven by nonlinear phenomena.

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15

Vincent, Olivier, Pierre Bergeron y David Lafrenière. "Searching for ZZ Ceti white dwarfs in the Gaia survey". Proceedings of the International Astronomical Union 15, S357 (octubre de 2019): 123–26. http://dx.doi.org/10.1017/s1743921320000265.

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AbstractThe Gaia satellite recently released parallax measurements for nearly 400,000 white dwarf stars, allowing for precise measurements of their physical parameters. By combining these parallaxes with Pan-STARRS and CFIS-u photometry, we measured the effective temperatures and surface gravities for all white dwarfs within 100 pc and identified a sample of ZZ Ceti white dwarf candidates within the instability strip. We report the results of a photometric follow-up, currently under way, aimed at identifying new ZZ Ceti stars among this sample using the PESTO camera attached to the 1.6-m telescope at the Mont Mégantic Observatory. Our goal is to verify that ZZ Ceti stars occupy a region in the logg-Teff plane where no nonvariable stars are found, supporting the idea that ZZ Ceti pulsators represent a phase through which all hydrogen-line (DA) white dwarfs must evolve.

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16

Fekel, Francis C. y Joseph J. Eitter. "Chromospherically active stars. VII - 39 Ceti = AY Ceti, HD 185151 = V1764 Cygni, and binary synchronization". Astronomical Journal 97 (abril de 1989): 1139. http://dx.doi.org/10.1086/115056.

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17

Marín Padilla, Encarnación. "Inútil rebeldía de Ceti Leredi en relación con su matrimonio (siglo XV)". Sefarad 52, n.º 2 (30 de diciembre de 1992): 501. http://dx.doi.org/10.3989/sefarad.1992.v52.i2.973.

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Este estudio está dedicado a la inconformista personalidad de Ceti Leredi, la judía que intentó rebelarse contra su concertado matrimonio con Jaco Abenbitas. Ceti, hija de Hahim Leredi y de Duenya Gallur, residió en Épila, villa aragonesa del señorio de los Ximénez de Urrea, en el siglo XV.

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18

Miguel, Enrique de, Joseph Patterson, Jonathan Kemp, Gordon Myers, Robert Rea, Thomas Krajci, Berto Monard y Lewis M. Cook. "Orbital Period Increase in ES Ceti". Astrophysical Journal 852, n.º 1 (28 de diciembre de 2017): 19. http://dx.doi.org/10.3847/1538-4357/aa9ed6.

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19

Zanfi, Federico y Gaia Caramellino. "Costruire la cittŕ dei ceti medi". TERRITORIO, n.º 64 (febrero de 2013): 61–65. http://dx.doi.org/10.3280/tr2013-064010.

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This section reports the first results of a research project which examines residential architecture built for the middle classes from the 1950s until the 1970s in the cities of Turin, Milan and Rome. These essays - which focus mainly on Milan and Turin - dwell on various aspects of the phenomenon which include the following: the relationship between urban planning and the contraction of middle class cities, the role of private sector operators; the involvement of the public sector through forms of housing that are subsidised with concessions by government; the role of property developers; the issue of the ‘translation' of high-end and standard international architectural models towards a broader market connected with consumer models and tastes expressed by the growing middle classes.

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20

Park, Seung-Kyun y Namhee Ryoo. "A Case of Flavobacterium ceti Meningitis". Annals of Laboratory Medicine 36, n.º 6 (1 de noviembre de 2016): 614–16. http://dx.doi.org/10.3343/alm.2016.36.6.614.

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21

Lacy, C. H. S., F. C. Fekel, R. D. Mathieu, N. I. Morrell, J. A. Morse, G. Torres y D. Willmarth. "The Spectroscopic Orbit of Pi Ceti". Astronomical Journal 113 (marzo de 1997): 1088. http://dx.doi.org/10.1086/118325.

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22

Simon, Theodore y George Sonneborn. "The ultraviolet variability of AY Ceti". Astronomical Journal 94 (diciembre de 1987): 1657. http://dx.doi.org/10.1086/114597.

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23

Castanheira, B. G. y S. O. Kepler. "Seismological studies of ZZ Ceti stars". Journal of Physics: Conference Series 172 (1 de junio de 2009): 012068. http://dx.doi.org/10.1088/1742-6596/172/1/012068.

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24

Gray, David F. y Sallie L. Baliunas. "The activity cycle of tau Ceti". Astrophysical Journal 427 (junio de 1994): 1042. http://dx.doi.org/10.1086/174210.

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25

Teays, T. J. y N. R. Simon. "The unusual pulsating variable XZ Ceti". Astrophysical Journal 290 (marzo de 1985): 683. http://dx.doi.org/10.1086/163025.

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26

Copperwheat, C. M., T. R. Marsh, V. S. Dhillon, S. P. Littlefair, P. A. Woudt, B. Warner, J. Patterson et al. "The photometric period in ES Ceti". Monthly Notices of the Royal Astronomical Society 413, n.º 4 (25 de marzo de 2011): 3068–74. http://dx.doi.org/10.1111/j.1365-2966.2011.18382.x.

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27

Clemens, J. Christopher. "Seismology of the ZZ Ceti Stars". Symposium - International Astronomical Union 185 (1998): 253–60. http://dx.doi.org/10.1017/s0074180900238734.

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The pulsations of white dwarf stars are potentially a rich source of information about white dwarf structural properties. Extracting and applying this information to improve our knowledge of white dwarf interiors requires measuring individual eigenperiods in a complex power spectrum, and identifying the character of the eigenmodes they represent. This review will summarize observational progress in these areas for the ZZ Ceti pulsators.

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28

Mukadam, Anjum S., S. O. Kepler, D. E. Winget, R. E. Nather, M. Kilic, F. Mullally, T. von Hippel et al. "Constraining the Evolution of ZZ Ceti". Astrophysical Journal 594, n.º 2 (10 de septiembre de 2003): 961–70. http://dx.doi.org/10.1086/377044.

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29

Srivastava, R. K. "Constancy of period in TX Ceti". Astrophysics and Space Science 166, n.º 2 (abril de 1990): 205–10. http://dx.doi.org/10.1007/bf01094893.

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30

Panchuk, V. E. y V. G. Klochkova. "Mira Ceti-Type Variables. Atomic Spectra". Astrophysical Bulletin 77, n.º 4 (diciembre de 2022): 446–57. http://dx.doi.org/10.1134/s1990341322040071.

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31

Robertson, Paul. "Aliasing in the Radial Velocities of YZ Ceti: An Ultra-short Period for YZ Ceti c?" Astrophysical Journal 864, n.º 2 (6 de septiembre de 2018): L28. http://dx.doi.org/10.3847/2041-8213/aadc0b.

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32

Garofolo, Giuliano, Katiuscia Zilli, Pasquale Troiano, Antonio Petrella, Francesca Marotta, Gabriella Di Serafino, Massimo Ancora y Elisabetta Di Giannatale. "Brucella ceti from two striped dolphins stranded on the Apulia coastline, Italy". Journal of Medical Microbiology 63, n.º 2 (1 de febrero de 2014): 325–29. http://dx.doi.org/10.1099/jmm.0.065672-0.

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Since 1994, when Brucella ceti was first isolated from an aborted dolphin fetus, several cases have been reported worldwide. The first case of B. ceti in the Mediterranean (and in Italy), however, was recorded only in 2012, off the coast of Tuscany. Extensive studies, using serological and microbiological methods, have documented this bacterium in dolphins and demonstrated its zoonotic potential. We describe the typing of two B. ceti strains isolated from striped dolphins (Stenella coeruleoalba) stranded on the southern Apulia coastline. B. ceti isolates were conventionally typed, and then genotyped by both the multilocus sequence typing (MLST) and the multilocus variable number of tandem repeats typing (MLVA) methodologies to infer phylogeny and potential epidemiological links between the two cases. The two isolates were identified through MLST analysis as belonging to the common sequence type 26 (ST26), while MLVA analysis, having established that the two isolates have identical profiles, assigned them to a novel genotype within cluster A – a unique representative of a new Mediterranean subcluster. The results thus revealed a link between the two cases studied, demonstrating the usefulness of MLST and MLVA for the epidemiological investigation of brucellae among marine mammals.

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33

McFee, WE, D. Wu, K. Colegrove, K. Terio, L. Balthis y R. Young. "Occurrence of Brucella ceti in stranded bottlenose dolphins Tursiops truncatus coincides with calving season". Diseases of Aquatic Organisms 141 (22 de octubre de 2020): 185–93. http://dx.doi.org/10.3354/dao03526.

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Brucellosis is a disease caused by the Gram-negative facultative intracellular bacterium Brucella spp. In terrestrial species, this zoonotic bacterium is a global public health risk, but there is also concern over the zoonotic potential of marine forms, such as B. ceti, which affects cetaceans. Due to the detection of B. ceti in samples from bottlenose dolphins Tursiops truncatus during the 2010-2014 Gulf of Mexico Unusual Mortality Event, a long-term study of the prevalence of Brucella in stranded bottlenose dolphins from South Carolina, USA, was conducted. From 2012 through 2017, 282 stranded bottlenose dolphins were tested for B. ceti via real-time PCR. Nearly 32% of the dolphins tested positive in at least one sample (brain, lung, blowhole swab). Very little information exists in the literature on the occurrence of Brucella spp. in marine mammals, though in terrestrial species, such as cattle and elk, higher prevalence is often reported in spring. Similar results were found in this study with the peak occurrence being between March and June, a known period of calving in South Carolina. Results from this study provide important insights into the occurrence of the marine bacterium B. ceti.

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34

De Pieri, Filippo. "La legge 167 e i ceti medi". TERRITORIO, n.º 64 (febrero de 2013): 75–81. http://dx.doi.org/10.3280/tr2013-064012.

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The 1962 Law n. 167 played an important role in favouring the construction of residential buildings for middle classes in various Italian cities. Often associated with the construction of large social housing complexes, Law n. 167 also included support for large sectors of the middle classes to achieve home ownership among its objectives, following on from post-war ‘economical' housing policies. It was in fact the more ambitious interpretations of Law No. 167 in the 1960s and 1970s in Italy (those which saw it as the first step towards a structural reform of the 1942 law), which pushed for the inclusion of substantial quotas of construction for middle classes in zoning plans. Results in this period differed according to the local context and left behind them a varied building and social landscape, which still awaits a full assessment.

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35

Mukadam, Anjum S., M. H. Montgomery, D. E. Winget, S. O. Kepler y J. C. Clemens. "Ensemble Characteristics of the ZZ Ceti Stars". Astrophysical Journal 640, n.º 2 (abril de 2006): 956–65. http://dx.doi.org/10.1086/500289.

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36

O'Donoghue, D. "On mode changes in ZZ Ceti stars". Monthly Notices of the Royal Astronomical Society 220, n.º 1 (1 de mayo de 1986): 19P—22P. http://dx.doi.org/10.1093/mnras/220.1.19p.

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37

Espaillat, Catherine, Joseph Patterson, Brian Warner y Patrick Woudt. "The Helium‐rich Cataclysmic Variable ES Ceti". Publications of the Astronomical Society of the Pacific 117, n.º 828 (febrero de 2005): 189–98. http://dx.doi.org/10.1086/427959.

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38

Shostack, S. "In search of Galactic company [SETI/CETI]". IEEE Potentials 16, n.º 1 (1997): 5–7. http://dx.doi.org/10.1109/45.565600.

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39

Downes, Ronald A. "IUE observations of WX Ceti in outburst". Astronomical Journal 99 (enero de 1990): 339. http://dx.doi.org/10.1086/115332.

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40

Castanheira, B. G., S. O. Kepler, F. Mullally, D. E. Winget, D. Koester, B. Voss, S. J. Kleinman et al. "Discovery of eleven new ZZ Ceti stars". Astronomy & Astrophysics 450, n.º 1 (abril de 2006): 227–31. http://dx.doi.org/10.1051/0004-6361:20053500.

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41

Castanheira, B. G., S. O. Kepler, A. F. M. Costa, O. Giovannini, E. L. Robinson, D. E. Winget, S. J. Kleinman et al. "Towards a pure ZZ Ceti instability strip". Astronomy & Astrophysics 462, n.º 3 (13 de noviembre de 2006): 989–93. http://dx.doi.org/10.1051/0004-6361:20065886.

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42

Levenhagen, R. S., R. Künzel y N. V. Leister. "Physical parameters and chemical abundances of Ceti". New Astronomy 18 (enero de 2013): 55–61. http://dx.doi.org/10.1016/j.newast.2012.06.003.

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43

Melikian, N. D. y V. S. Shevchenko. "Photoelectric observations of flares on UV Ceti". Symposium - International Astronomical Union 137 (1990): 31–32. http://dx.doi.org/10.1017/s0074180900187352.

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Synchronous observations of the UV Cet flares were carried out in 1987. Two 60-cm telescopes in U-band were used. Accuracy of syncronous registration on two telescopes is 0.001s. 15 flares were registered simultaneously during observations. Single short-time (up to 2s) light increases were observed in quiescent state and flares, which are the result of observation errors. No light increase with duration shorter than 10s was registered simultaneously on two telescopes.

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44

Bingham, R., R. A. Cairns y B. J. Kellett. "Coherent cyclotron maser radiation from UV Ceti". Astronomy & Astrophysics 370, n.º 3 (mayo de 2001): 1000–1003. http://dx.doi.org/10.1051/0004-6361:20010290.

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45

Vučković, M., R. H. Østensen, C. Aerts, V. S. Dhillon y T. R. Marsh. "Multicolour photometry of EO Ceti (PB 8783)". Astrophysics and Space Science 329, n.º 1-2 (10 de julio de 2010): 183–87. http://dx.doi.org/10.1007/s10509-010-0401-3.

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46

Poveda, A., C. Allen y M. A. Herrera. "Kinematics and Ages of UV Ceti Stars". International Astronomical Union Colloquium 151 (1995): 57–60. http://dx.doi.org/10.1017/s0252921100034576.

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AbstractThe kinematic properties of 93 UV Ceti stars of the solar neighborhood are studied, based on a list of flares within 25 pc of the Sun (π ≥ 0".04). With updated values for their distances, proper motions and radial velocities (Gliese & Jahreiss 1991) space velocity dispersions are calculated for these stars. It is found that the total velocity dispersion of the flare stars (σ=30±3 km s−1) is similar to that of the F5 V stars from the same catalogue, for which the conventionally estimated mean age is about 3 · 109 years. A number of flare stars are identified as members of the Hyades, Sirius or Pleiades groups. The velocity dispersions found for the nearby flare stars, as well as their scale height and the membership of some of them to young kinematic groups, indicate that they belong to the young disk population. A small number (7) of UV Ceti stars have kinematics corresponding to the thick disk or halo population. Their long-lived chromospheric activity is interpreted as due to coalescence of old contact binaries. The question of the age of Proxima Centauri is examined in the context of our results, and found to be compatible with the ages of a Centauri A and B.

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47

Mukadam, Anjum S., D. E. Winget, Ted von Hippel, M. H. Montgomery, S. O. Kepler y A. F. M. Costa. "Redefining the Empirical ZZ Ceti Instability Strip". Astrophysical Journal 612, n.º 2 (10 de septiembre de 2004): 1052–59. http://dx.doi.org/10.1086/422551.

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48

Grinin, V. P. y V. V. Sobolev. "Initial flare phase of UV Ceti stars". Astrophysics 28, n.º 2 (1988): 208–12. http://dx.doi.org/10.1007/bf01004071.

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49

Althaus, Leandro G., Alejandro H. Córsico y Francisco De Gerónimo. "Effect of Coulomb diffusion of ions on the pulsational properties of DA white dwarfs". Astronomy & Astrophysics 644 (diciembre de 2020): A55. http://dx.doi.org/10.1051/0004-6361/202039557.

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Context. Element diffusion is a key physical process that substantially affects the superficial abundances, internal structure, pulsation properties, and evolution of white dwarfs. Aims. We study the effect of Coulomb separation of ions on the cooling times of evolving white dwarfs, their chemical profiles, the Brunt–Väisälä (buoyancy) frequency, and the pulsational periods at the ZZ Ceti instability strip. Methods. We followed the full evolution of white dwarf models in the range 0.5 − 1.3 M⊙ derived from their progenitor history on the basis of a time-dependent element diffusion scheme that incorporates the effect of gravitational settling of ions due to Coulomb interactions at high densities. We compared the results for the evolution and pulsation periods of ZZ Ceti stars with the case where this effect is neglected. Results. We find that Coulomb sedimentation profoundly alters the chemical profiles of ultra-massive (M⋆ ≳ 1 M⊙) white dwarfs throughout their evolution, preventing helium from diffusing inward toward the core, and thus leading to much narrower chemical transition zones. As a result, significant changes in the g-mode pulsation periods as high as 15% are expected for ultra-massive ZZ Ceti stars. For lower mass white dwarfs, the effect of Coulomb separation is much less noticeable. It causes period changes in ZZ Ceti stars that are below the period changes that result from uncertainties in progenitor evolution, but larger than the typical uncertainties of the observed periods. Conclusions. Coulomb diffusion of ions profoundly affects the diffusion flux in ultra-massive white dwarfs, driving the gravitational settling of ions with the same A/Z (mass to charge number). We show that it strongly alters the period spectrum of such white dwarfs, which should be taken into account in detailed asteroseismological analyses of ultra-massive ZZ Ceti stars.

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50

Baltrinic, Eric R. y Eric G. Suddeath. "A Q Methodology Study of a Doctoral Counselor Education Teaching Instruction Course". Professional Counselor 10, n.º 4 (diciembre de 2020): 472–87. http://dx.doi.org/10.15241/erb.10.4.472.

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Many counselor education and supervision (CES) doctoral programs offer doctoral-level teaching instruction courses as part of their curriculum to help prepare students for future teaching roles, yet little is known about the essential design, delivery, and evaluation components of these courses. Accordingly, the authors investigated instructor and student views on the essential design, delivery, and evaluation components of a doctoral counselor education teaching instruction (CETI) course using Q methodology. Eight first-year CES doctoral students and the course instructor from a large Midwestern university completed Q-sorts, which were factor analyzed. Three factors were revealed, which were named The Course Designer, The Future Educator, and The Empathic Instructor. The authors gathered post–Q-sort qualitative data from participants using a semi-structured questionnaire, and the results from the questionnaires were incorporated into the factor interpretations. Implications for incorporating the findings into CES pedagogy and for designing, delivering, and evaluating CETI courses are presented. Limitations and future research suggestions for CETI course design and delivery are discussed.

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