Stellar magnetic fields. 1: The role of a magnetic field in the peculiar M giant, HD 4174

Coronal heating by resonant absorption of Alfvenic surface waves (quiescent), and magnetic tearing instabilities (impulsive), is discussed with emphasis on three principles which may have application to late-type evolved stars. (1) If sq B/8 pi greater than sq. rho V is observed 2 in a stellar atmosphere, then the observed magnetic field must originate in an interior dynamo. (2) Low mass loss rates could imply the presence of closed magnetic flux loops within the outer atmosphere which constrain hydrodynamic flows when the magnetic body forces exceed the driving forces. (3) given that such magnetic loops effect an enhancement of the local heating rate, a positive correlation is predicted between the existence of a corona and low mass loss rates. These principles are applied to the M giant star HD 4174, which is purported to have a kilogauss magnetic field. Several of its spectroscopic peculiarities are shown to be consistent with the above principles, and further observational checks are suggested

Ingress observations of the 1980 eclipse of the symbiotic star CI Cyngni

One of the major results from the IUE may prove to be the knowledge gained by studies of the ultraviolet spectra of symbiotic stars. Symbiotics combine spectral features of a cool M giant like photosphere with strong high excitation emission lines of nebular origin, superposed. The UV spectra are dominated by intense permitted and semiforbidden emission lines and weak continua indicative of hot compact objects and accretion disks. Two symbiotics, AR Pav and CI Cyg are thought to be eclipsing binaries and IUE observations during the 1980 eclipse of CI Cygni are discussed

Direct UV observations of the circumstellar envelope of alpha Orionis

Observations were made in the IUE LWP camera, low dispersion mode, with alpha Ori being offset various distances from the center of the Long Wavelength Large Aperture along its major axis. Signal was acquired at all offset positions and is comprised of unequal components of background/dark counts, telescope-scattered light, and scattered light emanating from the extended circumstellar shell. The star is known from optical and infrared observations to possess an extended, arc-minute sized, shell of cool material. Attempts to observe this shell with the IUE are described, although the deconvolution of the stellar signal from the telescope scattered light requires further calibration effort

Urinary leukotriene E4 at 12 months and influencing factors

Stencel-Gabriel K, Czuba Z, Gabriel I, Majda A. Urinary leukotriene E4 at 12 months and influencing factors. Journal of Education, Health and Sport. 2016;6(1):197-206. eISSN 2391-8306. DOI http://dx.doi.org/10.5281/zenodo.45337http://ojs.ukw.edu.pl/index.php/johs/article/view/45337https://pbn.nauka.gov.pl/works/709857   The journal has had 7 points in Ministry of Science and Higher Education parametric evaluation. Part B item 755 (23.12.2015).755 Journal of Education, Health and Sport eISSN 2391-8306 7© The Author (s) 2016; This article is published with open access at Licensee Open Journal Systems of Kazimierz Wielki University in Bydgoszcz, PolandOpen Access. This article is distributed under the terms of the Creative Commons Attribution Noncommercial License which permits any noncommercial use, distribution, and reproduction in any medium,provided the original author(s) and source are credited. This is an open access article licensed under the terms of the Creative Commons Attribution Non Commercial License(http://creativecommons.org/licenses/by-nc/4.0/) which permits unrestricted, non commercial use, distribution and reproduction in any medium, provided the work is properly cited.This is an open access article licensed under the terms of the Creative Commons Attribution Non Commercial License (http://creativecommons.org/licenses/by-nc/4.0/) which permits unrestricted, non commercialuse, distribution and reproduction in any medium, provided the work is properly cited.The authors declare that there is no conflict of interests regarding the publication of this paper.Received: 15.12.2015. Revised 12.01.2016. Accepted: 25.01.2016.  Urinary leukotriene E4 at 12 months and influencing factors Stencel-Gabriel K ( 1 ), Czuba Z ( 2 ), Gabriel I ( 3 ), Majda A ( 1 ) 1.        Departament of Pediatrics, Bytom, Medical University of Silesia2.        Departament of Microbiology and Immunology, Zabrze, Medical University of Silesia3.        Department of Gynecology, Obstetrics and Oncological Gynecology, Bytom, Medical University of Silesia   Corresponding author:Krystyna Stencel-Gabrielul. Batorego 1541-902 Bytom Keywords: leukotriene E4, infants, allergy, urine. SummaryObjectiveLTE4 is the end point of cysLTs pathway and its only stable product. Its role was discussed in asthma and AEDS.We aimed to investigate the impact of genetic and environmental factors ( sex, maternal positive family atopy history, breastfeeding, passive smoking and pet exposure ).60 newborns ( including 30 boys ) were enrolled in the study. Each child was examined at 12 months and urine samples for urinary LTE4 measurement were collected. All samples were processed using ACETM Enzyme Immunoassay Kit ( Cayman Chemical, Ann Arbor, MI, USA ).The mean level of urinary LTE4 at 12 months was 186,99 pg/ml ( median: 159,0; CI 95%: 157,79- 221,59 ). The Shapiro- Wilk test showed that the distribution of the levels of urinary LTE4 were abnormal. 12- month- old girls had higher urinary LTE4 levels than boys( mean: 270,50 vs. 193,55 ), but maternal positive atopy history, pet exposure, tobacco smoking or length of breastfeeding had no impact on urinary LTE4 excretion.ConclusionsIn conclusion, most of genetic or environmental factors do not change levels of urinary LTE4 in infants.

Ultraviolet Observations of the 1980 Eclipse of the Symbiotic Star CI Cygni

Secular and eclipse variations of UV lines and continua during the course of nearly a full orbit of the symbiotic binary CI Cygni are presented. High-excitation resonance lines have brightened on an orbital time scale and show minimal effects of eclipse, while intercombination lines have faded and show pronounced but nontotal eclipse effects. The data are discussed in terms of mass transfer from the extended cool envelope of the red giant to a compact secondary. The formation of an accretion disk is a transitory phenomenon in which viscosity eventually dissipates the disk over orbital time scales. A large-scale low-density nebula explains the intercombination line emission, whereas the resonance line emission apparently arises in a large volume emitting region, possibly formed through shock collision from interacting stellar winds from the primary and secondary. Mass transfer rates are briefly discussed

Observations of Two Peculiar Emission Objects in the Large Magellanic Cloud

Ultraviolet and visual wavelength spectra were obtained of two peculiar emission objects, Henize S63 and Sanduleak.\u27s star in the Large Magellanic Cloud. Previously not observed in the near- or far-ultraviolet, both objects exhibit strong permitted and semiforbidden line emission. Estimates based on the absolute continuum flux of the hot companion star in Hen S63 indicate that it rivals the luminosity of the carbon star primary. The emission-line profile structure in both objects does not suggest Wolf-Rayet type emission. Carbon in Sanduleak.\u27s star (LMC anonymous) is conspicuously absent, while N v, N IV], and N III] dominate the UV emission-line spectrum. Nitrogen is overabundant with respect to carbon and oxygen in both objects. The large overabundance of nitrogen in Sanduleak.\u27s star suggests evidence for CNO processed material similar to that seen in \u27II Car

Multi-wavelength observations of the peculiar red giant HR 3126

Ultraviolet observations of the red giant HR 3126 are combined with multi-wavelength data in order to provide a firmer basis for explaining the arc-minute sized nebula surrounding the object. Possibilities as to the location of HR 3126 on the Hertzsprung-Russel diagram, and to the formation mechanisms of the reflection nebula IC 2220 associated with it, are summarized

Morphology Studies of Iron-Manganese Thin Films

Fe-based catalysts are known to be effective for Fischer-Tropsch synthesis from coal but are sensitive to sulfur poisoning. Addition of manganese to these catalysts has been proposed in an effort to combat this catalyst deactivation. To investigate the fundamental physical aspects of Mn incorporation into Fe, different compositions of model thin films of Fe-Mn, ranging from 100% Fe to 100% Mn were studied for the very first time, using scanning tunneling microscopy (STM), atomic force microscopy (AFM) and scanning electron microscopy. Our preliminary results indicate that the grain size of iron varied from 50 nm to 150 nm using the AFM image, in general agreement with others. Also the mixture with small amounts of manganese had large oxidic area. The surface was modified by the addition of manganese. The STM images of the samples showed similarities between pure iron and 75% Fe-25% Mn, while the 25% Fe-75% Mn looked very similar to 100% Mn. The mixture of 50% Fe-50% Mn seemed to contain two distinct surface features. This leads us to believe that STM and AFM can be useful tools to further investigate the model iron-manganese thin films and hence give insight into the unknown atomic scale interactions and also to study the catalytic properties better

Ingress Observations of the 1980 Eclipse of the Symbiotic Star CI Cygni

One of the major results from the IUE may prove to be the new knowledge gained by studies of the ultraviolet spectra of symbiotic stars. Symbiotics combine spectral features of a cool M giant-like photosphere with strong high excitation emission lines of nebular origin, superposed. An excellent pre-UV review has been given by Swings (i). The UV spectra are dominated by intense permitted and semi-forbidden emission lines and weak continua indicative of hot compact objects and accretion disks. Two symbiotics, AR Pay and CI Cyg are thought to be eclipsing binaries, and we have begun IUE observations during the predicted 1980 eclipse of CI Cygni.https://digitalcommons.chapman.edu/scs_books/1004/thumbnail.jp