Journal articles: 'WR'

1

Yammine, Halim. "“WR”." Methodist DeBakey Cardiovascular Journal 12, no. 4 (November 2016): 238. http://dx.doi.org/10.14797/mdcj-12-4-238.

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Fahey, Robert C., and Gerald L. Newton. "Measurement of WR-2721, WR-1065, and WR-33278 in plasma." International Journal of Radiation Oncology*Biology*Physics 11, no. 6 (June 1985): 1193–97. http://dx.doi.org/10.1016/0360-3016(85)90069-0.

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Spence, A. M., K. A. Krohn, J. E. Steele, S. E. Edmondson, and J. S. Rasey. "WR-2721, WR-77913 and WR-3689 radioprotection in the rat spinal cord." Pharmacology & Therapeutics 39, no. 1-3 (January 1988): 89–91. http://dx.doi.org/10.1016/0163-7258(88)90044-7.

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&NA;. "WR 6026." Inpharma Weekly &NA;, no. 1191 (June 1999): 11. http://dx.doi.org/10.2165/00128413-199911910-00020.

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Liu, Yang, Chengdong Lin, and Zhenjiang Li. "WR-Hand." Proceedings of the ACM on Interactive, Mobile, Wearable and Ubiquitous Technologies 5, no. 3 (September 9, 2021): 1–27. http://dx.doi.org/10.1145/3478112.

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This paper presents WR-Hand, a wearable-based system tracking 3D hand pose of 14 hand skeleton points over time using Electromyography (EMG) and gyroscope sensor data from commercial armband. This system provides a significant leap in wearable sensing and enables new application potentials in medical care, human-computer interaction, etc. A challenge is the armband EMG sensors inevitably collect mixed EMG signals from multiple forearm muscles because of the fixed sensor positions on the device, while prior bio-medical models for hand pose tracking are built on isolated EMG signal inputs from isolated forearm spots for different muscles. In this paper, we leverage the recent success of neural networks to enhance the existing bio-medical model using the armband's EMG data and visualize our design to understand why our solution is effective. Moreover, we propose solutions to place the constructed hand pose reliably in a global coordinate system, and address two practical issues by providing a general plug-and-play version for new users without training and compensating for the position difference in how users wear their armbands. We implement a prototype using different commercial armbands, which is lightweight to execute on user's phone in real-time. Extensive evaluation shows the efficacy of the WR-Hand design.

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Mellema, G., and P. Lundqvist. "Stellar wind bubbles around WR and [WR] stars." Astronomy & Astrophysics 394, no. 3 (October 21, 2002): 901–9. http://dx.doi.org/10.1051/0004-6361:20021164.

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Arnal, E. M., C. E. Cappa, J. R. Rizzo, and S. Cichowolski. "The Interstellar Medium around Galactic WN Stars: WR 2, WR 128, and WR 151." Astronomical Journal 118, no. 4 (October 1999): 1798–805. http://dx.doi.org/10.1086/301043.

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Cichowolski, S., and E. M. Arnal. "An Effelsberg HI study of the ISM around WR 126, WR 154 and WR 155." Astronomy & Astrophysics 414, no. 1 (January 2004): 203–9. http://dx.doi.org/10.1051/0004-6361:20031620.

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9

de Nicolau, C. Cappa, V. S. Niemela, U. Herbstmeier, and B. Koribalski. "Search for HI Bubbles Around WR Stars: WR 149." Symposium - International Astronomical Union 169 (1996): 619–20. http://dx.doi.org/10.1017/s0074180900230465.

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The interaction of strong stellar winds with the interstellar medium creates large cavities or interstellar bubbles surrounded by expanding outer shells. 21-cm line (HI) observations have revealed the presence of such neutral gas bubbles around several WR stars (e.g. Niemela & Cappa de Nicolau 1991 and references therein; Dubner et al. 1992).Continuing our search for HI bubbles around WR stars, we have analyzed the neutral hydrogen distribution in the vicinity of the Wolf-Rayet star WR149, a highly reddened WN6-7 star located at 6.5 kpc in the direction (l,b) = (89.°53,+0.°65).

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Xiaoxin Zhou, Shashi Phadtare, Jefferey Schmidt, Krishna Agrawal, and Vimal Kishore. "Synthesis and radioprotective effects of new phosphorothioate esters of WR-2721, WR-3689 and WR-151327." Bioorganic & Medicinal Chemistry Letters 7, no. 6 (March 1997): 693–98. http://dx.doi.org/10.1016/s0960-894x(97)00081-4.

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11

Hamann, Wolf-Rainer, Götz Gräfener, and Lars Koesterke. "WR Central Stars." Symposium - International Astronomical Union 209 (2003): 203–10. http://dx.doi.org/10.1017/s0074180900208516.

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Wallace, Debra J., Douglas R. Gies, Anthony F. J. Moffat, Michael M. Shara, and Virpi S. Niemela. "Hubble Space TelescopeImaging of the WR 38/WR 38a Cluster." Astronomical Journal 130, no. 1 (July 2005): 126–33. http://dx.doi.org/10.1086/430671.

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Wallace, Debra J., Anthony F. J. Moffat, Michael M. Shara, Douglas R. Gies, Virpi S. Niemela, and Edmund Nelan. "A HST imaging survey of a sample of 61 Galactic Wolf-Rayet stars — the WC8-9 subsample." Symposium - International Astronomical Union 212 (2003): 578–80. http://dx.doi.org/10.1017/s0074180900212941.

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A HST-wfpc2 survey of Galactic Wolf-Rayet stars was undertaken over a five year period, in an effort to discover new close visual companions, tight clusters, and/or association memberships. In total, 61 Galactic WR stars were observed, with nine objects being members of the subclasses WC8 and WC9, which are associated with dust production. For these nine, we present images of WR 11, WR 48a, WR 69, WR 70, WR 81, and WR 92. We refer to Wallace et al. (2002) for discussion of WR 98a, WR 104, and WR 112. Overall, we find for separations of approximately ≥ 150 mas, that the binary/association properties of the WC8/WC9 sample are statistically indistinguishable from the overall WR population. These statistics are limited, however, by the small numbers of each WR subclass observed.

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Drissen, Laurent, Carmelle Robert, and Anthony F. J. Moffat. "Polarization variability among Wolf-Rayet stars. VII - The single stars WR 14, WR 25, and WR 69." Astrophysical Journal 386 (February 1992): 288. http://dx.doi.org/10.1086/171014.

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15

Marchenko, Sergey V., and Anthony F. J. Moffat. "Time-Frequency Analysis of Three Strongly Variable Wolf-Rayet Stars: WR 6, WR 134, and WR 123." Astrophysical Journal 499, no. 2 (June 1, 1998): L195—L198. http://dx.doi.org/10.1086/311358.

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Stamatović, B., S. R. Milovanović, M. Pluškovski, J. Stanošević, B. Bošković, B. Nagy, and M. Simović. "The effect of WR-2721, WR-1065 and WR-2823 on the activity of the isolated rat uterus." European Journal of Pharmacology 183, no. 6 (July 1990): 2415. http://dx.doi.org/10.1016/0014-2999(90)93986-z.

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17

ZHOU, X., S. PHADTARE, J. SCHMIDT, K. AGRAWAL, and V. KISHORE. "ChemInform Abstract: Synthesis and Radioprotective Effects of New Phosphorothioate Esters of WR-2721, WR-3689 and WR-151327." ChemInform 28, no. 28 (August 3, 2010): no. http://dx.doi.org/10.1002/chin.199728207.

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18

Gosset, E., Y. Nazé, H. Sana, G. Rauw, and J. M. Vreux. "Phase-resolvedXMM-Newtonobservations of the massive WR+O binary WR 22." Astronomy & Astrophysics 508, no. 2 (August 11, 2009): 805–21. http://dx.doi.org/10.1051/0004-6361/20077981.

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19

Williams, Felicia N., Kamil Nurczyk, Sanja Sljivic, Lori Chrisco, Catherine Calvert, Rabia Nizamani, Samuel W. Jones, and Bruce Cairns. "553 Work-related Burn Injuries Among Burn Patients in a Tertiary Care Burn Facility, 2013 – 2018." Journal of Burn Care & Research 41, Supplement_1 (March 2020): S116—S117. http://dx.doi.org/10.1093/jbcr/iraa024.181.

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Abstract Introduction The characteristics of work-related (WR) burn injuries compared to non-work-related (non-WR) burns are not well defined in the literature. In an effort to determine the potential impact of commonly accepted prevention efforts, we compared WR and non-WR burn injuries in our facility for the last five years. Methods All patients admitted to the burn center between January 1st, 2013 and December 31st, 2018, of working age were included. Demographics, burn characteristics, and patient outcomes were evaluated using Student’s t-test and chi-squared test where appropriate, significance was accepted at p< 0.05. Results 3,545 patients were included in this study. WR patients were 22% of all patients in this cohort. The majority of patients in both cohorts were white males in their twenties. Compared to non-WR patients, WR patients had fewer comorbidities with 30% smaller total body surface area burns, and shorter lengths of stay (see table). WR patients were more likely to suffer chemical (14.5% vs 2.3%) and electrical burns (11.9% vs 1.2%) compared to non-WR patients, respectively. 67% percent of WR burn fatalities were from electrical injuries, while flame was the leading cause of death in non-WR patients. Conclusions WR burn injured patients are young males with fewer co-morbid conditions. Etiologies of injuries are vastly different between non-lethal and lethal WR and non-WR injuries. Classic burn prevention strategies that target flame burn injuries and fatalities will have little impact on WR burn injuries. Applicability of Research to Practice This study highlights the importance of focusing prevention campaigns to industry as well as schools and homes.

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Eenens, P. R. J., P. M. Williams, and R. Wade. "Identification and Analysis of Infrared Lines of WC Stars." Symposium - International Astronomical Union 143 (1991): 99. http://dx.doi.org/10.1017/s0074180900044958.

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We present 1 – 3.4 μm spectra of six Wolf-Rayet stars: WR 146 (WC4), WR 111 (WC5), WR 86 (WC7), WR 140 (WC7+O4), WR 135 (WC8) and WR 88 (WC9). Examination of the relative strengths of the emission lines has enabled us to make over 20 new line identifications. Recombination analyses of the carbon and helium lines yield C/He abundance ratios much in excess of the solar value and correlated with spectral subtype.

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RASA, K., R. HORN, and M. RÄTY. "Water repellency of clay, sand and organic soils in Finland." Agricultural and Food Science 16, no. 3 (December 4, 2008): 267. http://dx.doi.org/10.2137/145960607783328218.

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Water repellency (WR) delays soil wetting process, increases preferential flow and may give rise to surface runoff and consequent erosion. WR is commonly recognized in the soils of warm and temperate climates. To explore the occurrence of WR in soils in Finland, soil R index was studied on 12 sites of different soil types. The effects of soil management practice, vegetation age, soil moisture and drying temperature on WR were studied by a mini-infiltrometer with samples from depths of 0-5 and 5-10 cm. All studied sites exhibited WR (R index >1.95) at the time of sampling. WR increased as follows: sand (R = 1.8-5.0) < clay (R = 2.4-10.3) < organic (R = 7.9-undefined). At clay and sand, WR was generally higher at the soil surface and at the older sites (14 yr.), where organic matter is accumulated. Below 41 vol. % water content these mineral soils were water repellent whereas organic soil exhibited WR even at saturation. These results show that soil WR also reduces water infiltration at the prevalent field moisture regime in the soils of boreal climate. The ageing of vegetation increases WR and on the other hand, cultivation reduces or hinders the development of WR.;

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22

Mohammed, Eman H. M., Dindyal Mandal, Saghar Mozaffari, Magdy Abdel-Hamied Zahran, Amany Mostafa Osman, Rakesh Kumar Tiwari, and Keykavous Parang. "Comparative Molecular Transporter Properties of Cyclic Peptides Containing Tryptophan and Arginine Residues Formed through Disulfide Cyclization." Molecules 25, no. 11 (June 2, 2020): 2581. http://dx.doi.org/10.3390/molecules25112581.

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We have previously reported cyclic cell-penetrating peptides [WR]5 and [WR]4 as molecular transporters. To optimize further the utility of our developed peptides for targeted therapy in cancer cells using the redox condition, we designed a new generation of peptides and evaluated their cytotoxicity as well as uptake behavior against different cancer cell lines. Thus, cyclic [C(WR)xC] and linear counterparts (C(WR)xC), where x = 4–5, were synthesized using Fmoc/tBu solid-phase peptide synthesis, purified, and characterized. The compounds did not show any significant cytotoxicity (at 25 µM) against ovarian (SK-OV-3), leukemia (CCRF-CEM), gastric adenocarcinoma (CRL-1739), breast carcinoma (MDA-MB-231), and normal kidney (LLCPK) cells after 24 and 72 h incubation. Both cyclic [C(WR)5C] and linear (C(WR)5C) demonstrated comparable molecular transporter properties versus [WR]5 in the delivery of a phosphopeptide (F′-GpYEEI) in CCRF-CEM cells. The uptake of F′-GpYEEI in the presence of 1,4-dithiothreitol (DTT) as the reducing agent was significantly improved in case of l(C(WR)5C), while it was not changed by [C(WR)5C]. Fluorescence microscopy also demonstrated a significant uptake of F′-GpYEEI in the presence of l(C(WR)5C). Cyclic [C(WR)5C] improved the uptake of the fluorescent-labeled anti-HIV drugs F′-d4T, F′-3TC, and F′-FTC by 3.0–4.9-fold. These data indicate that both [C(WR)5C] and linear (C(WR)5C) peptides can act as molecular transporters.

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Masuo, Kazuko, Hiroshi Mikami, Toshio Ogihara, and Michael L. Tuck. "Differences in Mechanisms Between Weight Reduction Sensitive and Insensitive Blood Pressure Reduction in Obese Subjects." Hypertension 36, suppl_1 (October 2000): 725. http://dx.doi.org/10.1161/hyp.36.suppl_1.725-d.

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P180 This study was conducted to clarify the differences in mechanisms between weight reduction (WR) sensitive and insensitive BP reduction, and to evaluate the contribution of family history of obesity (FH) to WR-induced BP reduction. In 61 obese hypertensive men (HT, 28.1±0.9 kg/m2, 35±3 years, 171±6/106±5 mmHg) and 52 obese normotensive men (NT, 27.9±0.6 kg/m2, 34±4 years, 131±5/83±4 mmHg), BMI, BP, fasting plasma norepinephrine (NE), angiotensin II (Ang II), PRA, leptin, insulin were measured every 2 week for 24 weeks with weight loss program (low caloric diet 1000kcal, 7gNaCl + excercise≥1 hr/day). WR and WR sensitive BP reduction were defined as >10% reduction in BMI or mean BP at week 12. 64% of HT and 63% of NT succeeded in WR, and 59% of HT with WR (sensitive vs insensitive P<.05) and 70% of NT with WR (P<.01) were sensitive in BP reduction. When FH+ was defined as at least one parent was obese (BMI>27.0 kg/m2), prevalence of FH+ was higher in 86% of HT and 95% of NT who failed in WR, and higher in 94% of HT and 80% of NT with WR insensitive BP reduction. Only the subjects who succeeded in WR were analyzed in this study. At entry, BP, NE, Ang II, PRA and insulin were higher in HT than in NT, although BMI and leptin were similar. However, the parameters at entry were similar between WR sensitive and insensitive BP reduction in each NT and HT. The decrements (Δ) in BP, NE, Ang II, leptin,insulin were significantly greater in subjects with WR sensitive BP reduction than subjects with WR insensitive BP reduction regardless of BP status during the study, although ΔBMI was similar. Significant decreases in the parameters were noted in earlier period in subjects with WR sensitive BP reduction than in subjects with insensitive BP reduction, and in NT than in HT. In the 4 study groups regardless of BP status or WR induced BP reduction, the decrease in NE preceded BP decline, and the decreases in Ang II, insulin, leptin & PRA followed BP decline with WR. These results suggest that a family history of obesity appears to contribute closely to resistance in weight loss and also to WR insensitive BP reduction. Suppression on sympathetic overactivity is a major mechanism in WR induced BP reduction.

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Viola, Teresa Herr, Andréa Machado Leal Ribeiro, Antônio Mário Penz Júnior, and Eduardo Spillari Viola. "Influence of water restriction on the performance and organ development of young broilers." Revista Brasileira de Zootecnia 38, no. 2 (February 2009): 323–27. http://dx.doi.org/10.1590/s1516-35982009000200015.

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The experiment was carried out to evaluate the effect of 0%, 10%, 20%, 30%, and 40% water restriction (WR) on broiler performance, behavior, organ development (heart, leg, proventriculus and gizzard, liver, and intestines), and intestinal micrometry. Four hundred and eighty ROSS 308 male broilers were raised in battery cages measuring 0.72 m², from 1 to 21 days of age. Feed was offered ad libitum, and environmental temperatures were kept in thermoneutral conditions. Water intake was estimated based on a control group, two days older than the experimental birds, with same initial weight. A linear reduction on bird performance, duodenal villi height, and fresh organs weight were observed as WR increased. At 21 days of age, for each 1% WR, a weight loss of 8.5 g was observed. However, the mortality rate was not affected by any WR level. Organ weight, relative to body weight, was not affected by WR, except for heart, which weight increased with WR. Villi numbers and crypts depth were not affected by WR. Birds under WR changed their behavior, becoming aggressive and irritated. Electron microscopy data showed higher villi extrusion in WR broilers. In conclusion, WR, regardless its magnitude, should be avoided in broiler production.

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Schulte-Ladbeck, Regina E. "Spectropolarimetry and wind asymmetries of Wolf-Rayet stars." Symposium - International Astronomical Union 163 (1995): 176–85. http://dx.doi.org/10.1017/s0074180900201939.

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Motivated by the question of what drives the winds of Wolf-Rayet (WR) stars, I have been investigating the structure of WR winds. Observational evidence has been accumulated which demonstrates that the winds of some (but not all) WR stars are not spherically symmetric or homogeneous. I review results of work in the literature pertaining to the detection of such wind asymmetries in single WR stars and WR binary components. Particular emphasis is placed on the technique of spectropolarimetry, and how it has contributed to our knowledge of the wind-geometry of WR stars.

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De Greve, J. P. "WR Binaries: Theoretical Aspects." Symposium - International Astronomical Union 143 (1991): 213–28. http://dx.doi.org/10.1017/s0074180900045174.

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The different channels for the formation of WR-stars, as suggested in the literature, are investigated. The presently available tools, in terms of evolutionary recipies, are reviewed and the results investigated of the use of these tools, with respect to the WR-binaries.Two of the three basic formation channels, mentioned in the literature, may serve as ways to obtain the presently observed group of WR-binaries: stellar wind mass loss in O-stars during the pre-WR phase and mass transfer in a massive close binary system. Discrepancies with observations necessitated the incorporation of stellar wind in the binary scenario.Theoretical developments in the last years are reviewed and confronted with the observations. The necessity of mass transfer in the formation process is argued for a major fraction of the double-lined WR-binaries. Using specific evolutionary ingredients, the original parameters of the systems are calculated. We also discuss the appearance and disappearance of double-lined WR-systems as well as the existence of eccentric WR-systems after mass transfer. The evolution of a number of specific systems is discussed individually.

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Annuk, K. "Long Period WR Binaries." Symposium - International Astronomical Union 143 (1991): 245–50. http://dx.doi.org/10.1017/s0074180900045204.

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Now it is clear that there exist some long period (periods exceed a year) Wolf-Rayet binaries. This paper presents the results of our radial velocity study for three WR binaries: HD193077 (WN6 + O9), HD193793 (WC7 + O5-6) and HD192641 (WC7 + O9). Our spectroscopic observations confirm that HD193077 and HD193793 are long period systems with the periods of 1538 and 2886 days. Most likely, HD192641 is also a long period WR binary (P ≥4400 days).

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Vilchez, J. M., and C. Esteban. "Abundances in WR Nebulae." Symposium - International Astronomical Union 143 (1991): 379–84. http://dx.doi.org/10.1017/s0074180900045472.

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Within an ongoing program of long slit spectroscopy of the known WR nebulae, we show here some results for eight objects of the sample selected from the master list of Chu et al. (1983). We present an analysis of their ionisation structure and determine abundances of oxygen, nitrogen and helium in as many positions as possible. The implications of the abundance results for the chemical enrichment of the Interstellar Medium and stellar nucleosynthesis are briefly reviewed.

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O'Rourke, N., E. McCloskey, and J. Kanis. "WR-2721 and hypocalcemia." Journal of Clinical Oncology 12, no. 1 (January 1994): 232. http://dx.doi.org/10.1200/jco.1994.12.1.232.

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Shaw, Leslie M., Donna Glover, Andrew Turrisi, Darrel Q. Brown, Heather S. Bonner, A. Lorraine Norfleet, Claire Weiler, John H. Glick, and Morton M. Kligerman. "Pharmacokinetics of WR-2721." Pharmacology & Therapeutics 39, no. 1-3 (January 1988): 195–201. http://dx.doi.org/10.1016/0163-7258(88)90061-7.

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Benaglia, Paula, and Gustavo E. Romero. "Gamma-ray production in selected Wolf-Rayet binaries." Symposium - International Astronomical Union 212 (2003): 150–51. http://dx.doi.org/10.1017/s0074180900211765.

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In the colliding wind region of early-type binaries, electrons can be accelerated up to relativistic energies, as demonstrated by the detection of non-thermal radio emission from several WR+OB systems. The particle acceleration region is exposed to strong photon fields, and inverse-Compton cooling of the electrons could result in a substantial high-energy non-thermal flux. We present here preliminary results of a study of the binaries WR 140, WR 146, and WR 147 in the light of recent radio and γ-ray observations. We show that under reasonable assumptions WR 140 can produce the γ-ray flux from the GRO-egret source 3EG J 2022+4317. WR 146 and WR 147 are below the detection threshold.

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Gosset, Eric, Pierre Royer, Gregor Rauw, Jean Manfroid, and Jean-Marie Vreux. "New observational results on the colliding wind WR+O binary WR 30a." Symposium - International Astronomical Union 193 (1999): 354–55. http://dx.doi.org/10.1017/s0074180900205706.

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WR30a (MS 4) was first suspected as a possible Wolf-Rayet star by McConnell & Sanduleak (1970) during a deep objective-prism survey performed around the Carina Nebula region. From subsequent studies, the spectrum turned out to be composite, with a WR component classified W04 (or alternatively WC4, W05 and WC3) and an 0 component classified 04. Niemela (1995) reported the first, and up-to-now unique, radial velocity study for that star. She noticed large variations of CIV λ4658 from night to night, suggesting that WR30a might be a short period binary. A plot of the C IV emission-line velocities versus the He II absorption ones clearly indicates that they are exhibiting opposite binary motions. The apparent velocity amplitudes imply a rather low mass ratio Mwo4/Mo4 = 0.15, although the radial velocities of the C IV line could be distorted due to line-profile variations.

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Herald, J. E., D. J. Hillier, and R. E. Schulte‐Ladbeck. "Tailored Analyses of the WN 8 Stars WR 40 and WR 16." Astrophysical Journal 548, no. 2 (February 20, 2001): 932–52. http://dx.doi.org/10.1086/319007.

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Booth, Valerie K., Jeanette C. Roberts, Raymond L. Warters, Britta H. Wilmore, and James R. Lepock. "Radioprotective Thiolamines WR-1065 and WR-33278 Selectively Denature Nonhistone Nuclear Proteins." Radiation Research 153, no. 6 (June 2000): 813–22. http://dx.doi.org/10.1667/0033-7587(2000)153[0813:rtwaws]2.0.co;2.

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Ring, S. M., P. Tippett, and D. M. Swallow. "Comparative Immunochemical Analysis of Wr^a and Wr^b Red Cell Antigens." Vox Sanguinis 67, no. 2 (1994): 226–30. http://dx.doi.org/10.1159/000462595.

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McDonough, John H., Paul C. Mele, and Carol G. Franz. "Comparison of behavioral and radioprotective effects of WR-2721 and WR-3689." Pharmacology Biochemistry and Behavior 42, no. 2 (June 1992): 233–43. http://dx.doi.org/10.1016/0091-3057(92)90521-g.

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Livesey, John C., Janet S. Rasey, Sarah Vertrees, Lynne M. Freeman, Sara Magee, Norma J. Nelson, Lay Chin, Zdenka Grunbaum, and Kenneth A. Krohn. "In vitro metabolism of the phosphorothioate radioprotectors WR-2721 and WR-3689." Pharmacology & Therapeutics 39, no. 1-3 (January 1988): 215–17. http://dx.doi.org/10.1016/0163-7258(88)90064-2.

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Arnal, E. Marcelo. "A high resolution H I study of the ISM local to WR 132 and WR 140." Symposium - International Astronomical Union 193 (1999): 334–35. http://dx.doi.org/10.1017/s0074180900205603.

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The neutral matter distribution from the interstellar medium located in the vicinity of the galactic WR stars WR 132 and WR 140 has been examined by means of the H I 21-cm line observations obtained with high angular resolution observations. The most interesting discoveries are the presence of huge ovoidal H I minimum spanning the velocity range +13 to +21kms−1 (WR132) and −18 to −7kms−1 (WR 140). These minima were created, very likely, by the joint action of the progenitor of both WR stars and the WR star itself. Inside each cavity, two minima are clearly discernible. The WR star is offset with respect to either the geometrical centre of the main H I void or the inner H I minima. The dual H I minimum geometry observed inside the main H I cavity, a feature also seen in the H I distribution of the ISM located close to other galactic WR stars, may be a consequence of the interaction process itself.

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Rate, Gemma, Paul A. Crowther, and Richard J. Parker. "Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – II. Cluster and association membership." Monthly Notices of the Royal Astronomical Society 495, no. 1 (May 12, 2020): 1209–26. http://dx.doi.org/10.1093/mnras/staa1290.

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ABSTRACT Galactic Wolf–Rayet (WR) star membership of star-forming regions can be used to constrain the formation environments of massive stars. Here, we utilize Gaia DR2 parallaxes and proper motions to reconsider WR star membership of clusters and associations in the Galactic disc, supplemented by recent near-infrared studies of young massive clusters. We find that only 18–36 per cent of 553 WR stars external to the Galactic Centre region are located in clusters, OB associations or obscured star-forming regions, such that at least 64 per cent of the known disc WR population are isolated, in contrast with only 13 per cent of O stars from the Galactic O star Catalogue. The fraction located in clusters, OB associations or star-forming regions rises to 25–41 per cent from a global census of 663 WR stars including the Galactic Centre region. We use simulations to explore the formation processes of isolated WR stars. Neither runaways, nor low-mass clusters, are numerous enough to account for the low cluster membership fraction. Rapid cluster dissolution is excluded as mass segregation ensures WR stars remain in dense, well-populated environments. Only low-density environments consistently produce WR stars that appeared to be isolated during the WR phase. We therefore conclude that a significant fraction of WR progenitors originate in low-density association-like surroundings which expand over time. We provide distance estimates to clusters and associations host to WR stars, and estimate cluster ages from isochrone fitting.

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40

Moffat, Anthony F. J. "Properties of Wolf-Rayet binaries: the key to understanding Wolf-Rayet stars." Symposium - International Astronomical Union 163 (1995): 213–22. http://dx.doi.org/10.1017/s0074180900201976.

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It is argued that, with few exceptions, WR stars in binaries are essentially indistinguishable from single WR stars of the same subtype. In particular, mass transfer from one star to the other can be neglected, being completely dominated by the winds and their interaction. Empirical masses and mass-loss rates derived for WR stars in binaries are then examined as typifying WR stars in general; they are used to derive a plausible scenario for the evolution of WR stars.

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41

Maeder, André. "Metallicity Effects in Massive Star Evolution and Number Frequencies of WR Stars in Galaxies." Symposium - International Astronomical Union 143 (1991): 445–52. http://dx.doi.org/10.1017/s0074180900045605.

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The results of new grids of models of massive stars with metallicities Z = 0.002, 0.005, 0.020 and 0.040 and mass loss rates depending on Z are shown. When integrated over the mass spectrum, the models enable us to predict number ratios, such as WR/O, WC/WN, WNE/WR, WNL/WR, WCE/WR, WCL/WR, WO/WR as a function of Z in galaxies.Comparisons between models and observations in galaxies are made and show, as was suggested by Maeder, Lequeux and Azzopardi (1980), that the effects of metallicity on the mass loss rates are the prime agent responsible for the different distributions of massive stars in galaxies.

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42

Williams, P. M. "Variable dust emission by WC type Wolf–Rayet stars observed in the NEOWISE-R survey." Monthly Notices of the Royal Astronomical Society 488, no. 1 (July 1, 2019): 1282–300. http://dx.doi.org/10.1093/mnras/stz1784.

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ABSTRACT Photometry at 3.4 and 4.6 ${\mu m}$ of 128 Population I WC type Wolf–Rayet stars in the Galaxy and 12 in the Large Magellanic Cloud (LMC) observed in the WISE NEOWISE-R survey was searched for evidence of circumstellar dust emission and its variation. Infrared spectral energy distributions (SEDs) were assembled, making use of archival r, i, Z, and Y photometry to determine reddening and stellar wind levels for the WC stars found in recent IR surveys and lacking optical photometry. From their SEDs, 10 apparently non-variable stars were newly identified as dust makers, including three, WR 102-22, WR 110-10, and WR 124-10, having subtype earlier than WC8–9, the first such stars to show this phenomenon. The 11 stars found to show variable dust emission include six new episodic dust makers, WR 47c, WR 75-11, WR 91-1, WR 122-14, and WR 125-1 in the Galaxy and HD 38030 in the LMC. Of previously known dust makers, NEOWISE-R photometry of WR 19 captured its rise to maximum in 2018 confirming the 10.1-yr period, that of WR 125 the beginning of a new episode of dust formation suggesting a period near 28.3 yr. while that of HD 36402 covered almost a whole period and forced revision of it to 5.1 yr.

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Cherepashchuk, A. M. "Wolf-Rayet Binaries: Observational Aspects." Symposium - International Astronomical Union 143 (1991): 187–200. http://dx.doi.org/10.1017/s0074180900045149.

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New data concerning observational aspects of Wolf-Rayet binaries are summarised. WR+O and WR+c binary systems are considered. All the data concerning WR binaries agree well with the modern understanding of WR stars as the helium remnants formed as a result of mass loss by massive O-type stars.

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Xiong, Zhaohui, Bao Zhang, and Yibin Yao. "Comparisons between the WRF data assimilation and the GNSS tomography technique in retrieving 3-D wet refractivity fields in Hong Kong." Annales Geophysicae 37, no. 1 (January 15, 2019): 25–36. http://dx.doi.org/10.5194/angeo-37-25-2019.

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Abstract. Water vapor plays an important role in various scales of weather processes. However, there are limited means to accurately describe its three-dimensional (3-D) dynamical changes. The data assimilation technique and the Global Navigation Satellite System (GNSS) tomography technique are two of the limited means. Here, we conduct an interesting comparison between the GNSS tomography technique and the Weather Research and Forecasting Data Assimilation (WRFDA) model (a representative of the data assimilation models) in retrieving wet refractivity (WR) in the Hong Kong area during a wet period and a dry period. The GNSS tomography technique is used to retrieve WR from the GNSS slant wet delays. The WRFDA is used to assimilate the zenith tropospheric delay to improve the background data. The radiosonde data are used to validate the WR derived from the GNSS tomography, the WRFDA output, and the background data. The root mean square (rms) of the WR derived from the tomography results, the WRFDA output, and the background data are 6.50, 4.31, and 4.15 mm km−1 in the wet period. The rms becomes 7.02, 7.26, and 6.35 mm km−1 in the dry period. The lower accuracy in the dry period is mainly due to the sharp variation of WR in the vertical direction. The results also show that assimilating GNSS ZTD into the WRFDA only slightly improves the accuracy of the WR and that the WRFDA WR is better than the tomographic WR in most cases. However, in a special experimental period when the water vapor is highly concentrated in the lower troposphere, the tomographic WR outperforms the WRFDA WR in the lower troposphere. When we assimilate the tomographic WR in the lower troposphere into the WRFDA, the retrieved WR is improved.

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Chen, Bao-An, Cheng-Yin Huang, Chui-Ping Li, Chong Gao, Jia-Hua Ding, Yun-Yu Sun, Fei Fei, and Ning-Na Chen. "Effects of Amifostine and Fengling Polysaccharide on Proliferation and Chemoprotection of Human Granulocyte-Macrophage Progenitor Cells." Blood 106, no. 11 (November 16, 2005): 4190. http://dx.doi.org/10.1182/blood.v106.11.4190.4190.

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Abstract Objective: This paper is to study the proliferation and chemoprotection effects of amifostine (WR-2721) and fengling polysaccharide (FLPS) on the human granulocyte-macrophage progenitor cells. Method: (1) Mononuclear cells (MNC) were deparated by Ficoll (1.077g/ml). The MNC of WR-2721 and FLPS treatment were cultured in methylcellulose senisolid medium, the colony forming unit-granulocyte macrophage(CFU-GM) was measured. The effects of WR-2721 and FLPS on CFU-GM were studied. (2) MNC of WR-2721 treatment or containing FLPS were cultured 14h at 37°C with VP16. The cytoprotective activity against VP16 toxic effects of WR-2721 and FLPS on CFU-GM were observed. (3)To study the effects of WR-2721 on proliferation inhibition and apoptosis of HL-60 human leukemia cell line, the cell apoptosis rate of HL-60 was determined by annexinV/PI double staining method, cell proliferation and chemotherapy sensitivity were analyzed with XTT assay, and the changes of cell cycle were observed through flow cytometry.(4) HL-60 cells of containing FLPS were cultured 14h at 37°C with VP16. The cytoprotective activity against VP16 toxic effects of FLPS on HL-60 cells were observed. Results: (1) The number of CFU-GM was significantly increased in 10 groups by addition of 0.5–25μg/ml FLPS and 12 groups treated with 0.01–5mmol/L WR-2721( 30 min, 37°C), p<0.05. The mean value of CFU-GM in groups of negative control, WR-2721 (1mmol/L), FLPS(5μg/ml) and WR-2721+FLPS were 91.4±50.4,119.8±62.9,143.2±76.4 and 179.2±97.6 per 1×105, respectively, Compared with control, singnificant differences were seen between each group, p<0.05. WR-2721+FLPS group compared with WR-2721 and FLPS group, p<0.01 and p<0.05. (2) The number of CFU-GM was significantly increased in MNC of adding FLPS or WR-2721 treatment. The mean value of CFU-GM in groups of VP-16 control, negative control, WR-2721 + VP16, FLPS + VP-16 and WR-2721 + FLPS + VP16 were 30.9±22.5, 83.2±43.8, 64.6±41.2, 55.3±33.5 and 78.3±48.2 per 1×105, respectively. Compared with VP16 control group, singnificant differences were seen between each group, p < 0.01. (3) After treatment (30min,37°C)with WR-2721, the sensitivity of HL-60 cells to VP-16 was enhanced, and the IC50 descended from 52.5μg/ml to 40.5μg/ml. After 72hours trentment of HL-60 cells with WR-2721, the early apoptotic cells (annexinV-FITC positive/PI negative) were increased from(5.5±1.9)% to (48.5±8.4)%(p<0.001), late apoptotic cells(annexinV-FITC positive/PI positive)were increased from(1.2±0.5)% to (39.0±4.0)% (p<0.001), and HL-60cells were arrested in G2-M phase. (4) HL60 cells were cultured 14h at 37°C with 20μg/ml VP16 and 50μg/ml FLPS, the cell survival rate was 88.0%±2.3%, negetive control was 90.5%±2.9%, no singnificant difference was seen between two group, n =21, p >0.05. Conclusion :(1) WR-2721 and FLPS can increase the prolification of CFU-GM. Combination of WR-2721 and FLPS show stronger effect than the WR-2721 or FLPS alone. (2) WR-2721 and FLPS selectiveiy protect human peripheral blood CFU-GM from the cytotoxicity of VP16 without decreasing its cytotoxic effect on HL60 cells. (3) WR-2721 treatment can enhance HL-60 cells chemotherapy sensitivity to VP-16, inhibit proliferation, induce HL-60 cells apoptosis and accumulation of cells in G2-M phase.

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46

Pindao, Maximilien. "Wolf-Rayet stars in extragalactic star-forming regions." Symposium - International Astronomical Union 193 (1999): 614–15. http://dx.doi.org/10.1017/s0074180900206451.

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We performed a search of Wolf-Rayet stars features in optical spectra of two large samples of H II regions and H II galaxies. The main results are a list of galaxies/regions containing WR stars (of which seven are new WR galaxies) and a second list of possible WR galaxies/regions with WR stars.

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Pendergrass, James A., Venkataraman Srinivasan, K. Sree Kumar, William E. Jackson, Thomas M. Seed, James A. Pendergrass, and Wayne A. Kleinman. "Determination of WR-1065 and WR-33278 by Liquid Chromatography with Electrochemical Detection: PVM 1:2002." Journal of AOAC INTERNATIONAL 85, no. 3 (May 1, 2002): 551–54. http://dx.doi.org/10.1093/jaoac/85.3.551.

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Abstract A liquid chromatographic method using electrochemical detection is presented for measuring the thiol WR-1065 [2-(3-aminopropylamino) ethanethiol] and its symmetrical disulfide WR-33278 [NH2(CH2)3NHCH2CH2S]2. WR-1065 is the active, radioprotective drug derived from the phosphorothioate pro-drug WR-2721 (amifostine). External standard curves for both compounds were linear over the range of 40-200 pmol injected (r2 = 0.999 and 0.996 for the thiol and disulfide, respectively). The detection and quantitation limits for WR-1065 were 9 and 18 pmol, respectively, whereas the corresponding values for WR-33278 were 30 and 59 pmol, respectively. Within- and between-day determinations of measurement precision and accuracy for both compounds validated the suitability of this assay method.

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Vanbeveren, D. "The Mass of WR Progenitors." Symposium - International Astronomical Union 143 (1991): 554. http://dx.doi.org/10.1017/s0074180900045794.

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A search through literature reveals four methods in order to derive the mass of WR progenitors, i.e.a. WR stars must be descendant from the most massive stars which share their galactic distribution,b. the computation of detailed evolutionary models of massive close binaries up to the WR phase, able to explain the observational constraints of these WR binaries,c. comparing the very narrow mass-luminosity relation of massive core helium burning stars predicted by evolution and estimated bolometric luminosities of WR members of stellar aggregates,d. the minimum mass of the progenitor of a WR member of a cluster equals the mass of the most luminous star (or the star with the earliest spectral type) in the cluster.

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Chopra, Surinder, Suzy M. Cocciolone, Shaun Bushman, Vineet Sangar, Michael D. McMullen, and Thomas Peterson. "The Maize Unstable factor for orange1 Is a Dominant Epigenetic Modifier of a Tissue Specifically Silent Allele of pericarp color1." Genetics 163, no. 3 (March 1, 2003): 1135–46. http://dx.doi.org/10.1093/genetics/163.3.1135.

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Abstract We have characterized Unstable factor for orange1 (Ufo1), a dominant, allele-specific modifier of expression of the maize pericarp color1 (p1) gene. The p1 gene encodes an Myb-homologous transcriptional activator of genes required for biosynthesis of red phlobaphene pigments. The P1-wr allele specifies colorless kernel pericarp and red cobs, whereas Ufo1 modifies P1-wr expression to confer pigmentation in kernel pericarp, as well as vegetative tissues, which normally do not accumulate significant amounts of phlobaphene pigments. In the presence of Ufo1, P1-wr transcript levels and transcription rate are increased in kernel pericarp. The P1-wr allele contains approximately six p1 gene copies present in a hypermethylated and multicopy tandem array. In P1-wr Ufo1 plants, methylation of P1-wr DNA sequences is reduced, whereas the methylation state of other repetitive genomic sequences was not detectably affected. The phenotypes produced by the interaction of P1-wr and Ufo1 are unstable, exhibiting somatic mosaicism and variable penetrance. Moreover, the changes in P1-wr expression and methylation are not heritable: meiotic segregants that lack Ufo1 revert to the normal P1-wr expression and methylation patterns. These results demonstrate the existence of a class of modifiers of gene expression whose effects are associated with transient changes in DNA methylation of specific loci.

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Munoz, Melissa, Anthony J. Moffat, Grant M. Hill, Tomer Shenar, Noel D. Richardson, Herbert Pablo, Nicole St-Louis, and Tahina Ramiaramanantsoa. "WR 148 and the not so compact companion." Proceedings of the International Astronomical Union 12, S329 (November 2016): 427. http://dx.doi.org/10.1017/s174392131700357x.

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AbstractThe objective is to determine the nature of the unseen companion of the single-lined spectroscopic binary, WR 148 (= WN7h+?). The absence of companion lines supports a compact companion (cc) scenario. The lack of hard X-rays favours a non-compact companion scenario. Is WR 148 a commonplace WR+OB binary or a rare WR+cc binary?

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Journal articles on the topic 'WR'

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