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On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: the Urc Ious Case of WR124 Jesus A
East Tennessee State University Digital Commons @ East Tennessee State University ETSU Faculty Works Faculty Works 12-10-2018 On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The urC ious Case of WR124 Jesus A. Toala UNAM Campus Morelia Lidi Oskinova University of Potsdam W.R. Hamann University of Potsdam Richard Ignace East Tennessee State University, [email protected] A.A. C. Sander University of Potsdam See next page for additional authors Follow this and additional works at: https://dc.etsu.edu/etsu-works Citation Information Toala, Jesus A.; Oskinova, Lidi; Hamann, W.R.; Ignace, Richard; Sander, A.A. C.; Todt, H.; Chu, Y.H.; Guerrero, M. A.; Hainich, R.; Hainich, R.; and Terrejon, J. M.. 2018. On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The urC ious Case of WR124. Astrophysical Journal Letters. Vol.869 https://doi.org/10.3847/2041-8213/aaf39d ISSN: 2041-8205 This Article is brought to you for free and open access by the Faculty Works at Digital Commons @ East Tennessee State University. It has been accepted for inclusion in ETSU Faculty Works by an authorized administrator of Digital Commons @ East Tennessee State University. For more information, please contact [email protected]. On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The Curious Case of WR124 Copyright Statement © 2018. The American Astronomical Society. Reproduced by permission of the AAS. Creator(s) Jesus A. Toala, Lidi Oskinova, W.R. Hamann, Richard Ignace, A.A. C. Sander, H. Todt, Y.H. Chu, M. A. Guerrero, R. Hainich, R. Hainich, and J. M. -
Lo N G H O R
NATIONAL CHAMPIONS • 1963, ’69, ’70, 2005 BIG 12 CHAMPIONS • ‘96, ‘05, ‘09 SOUTHWESTTEXAS CONFERENCE CHAMPIONS • 1920, ’28, ’30, ’42, ’43, ’45, ’50, ’52, ’53*, LONGHORNS ’59*, ’61*, ’62, ’63, ’68*, ’69, ’70, ’71 , ’72, ’73, ’75*, ’77, ’83, ’90, ’94*, ’95 (*co-champs) Athletics Media Relations Department • P.O. Box 7399 • Austin, TX 78713-7399 • Office: 512/471-6036 • Fax: 512/471-6040 TEXAS WINS FOURTH STRAIGHT: • Mike Davis ranks first in the Big 12 and BYE WEEK Texas piled up 609 yards of total offense, seventh in the FBS in yards per reception including a career-high 364 passing yards at 18.6 (minimum 30 catches). from David Ash, in an emotional 33-7 • The Longhorns ranks tied for 18th in the victory over Iowa State Saturday. The FBS in turnover margin (+0.80 per game). Longhorns won for the fourth-straight The Horns have forced 16 turnovers and time on a day they remembered former committed just eight (fifth fewest in the Next Up: coach Darrell Royal, who died last week, FBS). They have turned those miscues into points, outscoring the opposition 77-10 #18/15 TEXAS (8-2, 5-2 Big 12) and recognized Veteran’s Day. While Ash this season off turnovers. Texas has not vs. was completing 25 of 31 passes, includ- ing a 61-yard TD pass to Mike Davis, the committed a turnover in its last nine quar- TCU (6-4, 3-4 Big 12) defense held the Cyclones to 277 total ters of action. • Texas is fourth in the FBS in offensive Darrell K Royal - Texas Memorial Stadium/ yards, including just 64 in the second half. -
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A&A 551, A71 (2013) Astronomy DOI: 10.1051/0004-6361/201219816 & c ESO 2013 Astrophysics Carbon monoxide in the environs of the star WR 16 N. U. Duronea1,3,E.M.Arnal1,2, and L. Bronfman3 1 Instituto Argentino de Radioastronomía, CONICET, CCT-La Plata, C.C.5., 1894 Villa Elisa, Argentina e-mail: [email protected] 2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina 3 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile Received 14 June 2012 / Accepted 6 December 2012 ABSTRACT Aims. We analyze the carbon monoxide emission around the star WR 16 aiming to study the physical characteristics of the molecular gas linked to the star and to achieve a better understanding of the interaction between massive stars with their surroundings. Methods. We study the molecular gas in a region ∼86.4 × 86.4insizeusingCOJ = 1 → 0and13CO J = 1 → 0 line data obtained with the 4-m NANTEN telescope. Radio continuum archival data at 4.85 GHz, obtained from the Parkes-MIT-NRAO Southern Radio Survey, are also analyzed to account for the ionized gas. Available IRAS (HIRES) 60 μm and 100 μm images are used to study the characteristics of the dust around the star. Results. Our new CO and 13CO data allow the low/intermediate density molecular gas surrounding the WR nebula to be completely mapped. We report two molecular features at −5kms−1 and −8.5 km s−1 (components 1 and 2, respectively) having a good mor- phological resemblance with the Hα emission of the ring nebula. -
Football Bowl Subdivision Records
FOOTBALL BOWL SUBDIVISION RECORDS Individual Records 2 Team Records 24 All-Time Individual Leaders on Offense 35 All-Time Individual Leaders on Defense 63 All-Time Individual Leaders on Special Teams 75 All-Time Team Season Leaders 86 Annual Team Champions 91 Toughest-Schedule Annual Leaders 98 Annual Most-Improved Teams 100 All-Time Won-Loss Records 103 Winningest Teams by Decade 106 National Poll Rankings 111 College Football Playoff 164 Bowl Coalition, Alliance and Bowl Championship Series History 166 Streaks and Rivalries 182 Major-College Statistics Trends 186 FBS Membership Since 1978 195 College Football Rules Changes 196 INDIVIDUAL RECORDS Under a three-division reorganization plan adopted by the special NCAA NCAA DEFENSIVE FOOTBALL STATISTICS COMPILATION Convention of August 1973, teams classified major-college in football on August 1, 1973, were placed in Division I. College-division teams were divided POLICIES into Division II and Division III. At the NCAA Convention of January 1978, All individual defensive statistics reported to the NCAA must be compiled by Division I was divided into Division I-A and Division I-AA for football only (In the press box statistics crew during the game. Defensive numbers compiled 2006, I-A was renamed Football Bowl Subdivision, and I-AA was renamed by the coaching staff or other university/college personnel using game film will Football Championship Subdivision.). not be considered “official” NCAA statistics. Before 2002, postseason games were not included in NCAA final football This policy does not preclude a conference or institution from making after- statistics or records. Beginning with the 2002 season, all postseason games the-game changes to press box numbers. -
All-Time All-America Teams
1944 2020 Special thanks to the nation’s Sports Information Directors and the College Football Hall of Fame The All-Time Team • Compiled by Ted Gangi and Josh Yonis FIRST TEAM (11) E 55 Jack Dugger Ohio State 6-3 210 Sr. Canton, Ohio 1944 E 86 Paul Walker Yale 6-3 208 Jr. Oak Park, Ill. T 71 John Ferraro USC 6-4 240 So. Maywood, Calif. HOF T 75 Don Whitmire Navy 5-11 215 Jr. Decatur, Ala. HOF G 96 Bill Hackett Ohio State 5-10 191 Jr. London, Ohio G 63 Joe Stanowicz Army 6-1 215 Sr. Hackettstown, N.J. C 54 Jack Tavener Indiana 6-0 200 Sr. Granville, Ohio HOF B 35 Doc Blanchard Army 6-0 205 So. Bishopville, S.C. HOF B 41 Glenn Davis Army 5-9 170 So. Claremont, Calif. HOF B 55 Bob Fenimore Oklahoma A&M 6-2 188 So. Woodward, Okla. HOF B 22 Les Horvath Ohio State 5-10 167 Sr. Parma, Ohio HOF SECOND TEAM (11) E 74 Frank Bauman Purdue 6-3 209 Sr. Harvey, Ill. E 27 Phil Tinsley Georgia Tech 6-1 198 Sr. Bessemer, Ala. T 77 Milan Lazetich Michigan 6-1 200 So. Anaconda, Mont. T 99 Bill Willis Ohio State 6-2 199 Sr. Columbus, Ohio HOF G 75 Ben Chase Navy 6-1 195 Jr. San Diego, Calif. G 56 Ralph Serpico Illinois 5-7 215 So. Melrose Park, Ill. C 12 Tex Warrington Auburn 6-2 210 Jr. Dover, Del. B 23 Frank Broyles Georgia Tech 6-1 185 Jr. -
General Disclaimer One Or More of the Following Statements May Affect
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) I Si (NASA-CR-170758) FEASI73ILIIY ETUC'Y CF AN N8=-25!45 OPTICALLI CCHERENT T:EL,ESCOFE AfFl y I'N SPACE Final Report, 19 May 1960 - 31 rec. 1982 (Sni"63,sonilz u Astrophysical Cbsetvatcry) Unclds 235 p HC A 1 1/ME A01 CSCL '2OF G3/74 1176C FEASIBILITY STUDY OF AN OPTICALLY COHERENT TELESCOPE ARRAY IN SPACE CONTRACT NAS8-33893 r Final Report and Technical Report No. 2 For the period 19 May 1980 to 31 December 1982 Dr. Wesley A, Traub Principal Investigator February 1983 s r Prepared f6r1^Z+-°`'^^^ National Aeronautics and Space Administra T Marshall Space Flight Center n MAY 1 983 Alabama 35812 RECEIVED SILFACIUR awn Smithsonian Institution Astrophysical Observatory Cambridge, Massachusetts 02138 The Smithsonian Astrophysical Observatory and the Harvard College Observatory are members of the Center for Astrophysics ,- The NASA Technical. -
Wolf-Rayet Stars and O-Star Runaways with HIPPARCOS II. Photometry?
UvA-DARE (Digital Academic Repository) Wolf-Rayet stars and O-stars runaways with HIPPARCOS. II. Photometry Marchenko, S.V.; Moffat, A.F.J.; van der Hucht, K.A.; Seggewiss, W.; Schrijver, H.; Stenholm, B.; Lundstrom, I.; Setia Gunawan, D.Y.A.; Sutantyo, W.; van den Heuvel, E.P.J.; Cuyper, J.- P.; Gomez, A.E. Publication date 1998 Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Marchenko, S. V., Moffat, A. F. J., van der Hucht, K. A., Seggewiss, W., Schrijver, H., Stenholm, B., Lundstrom, I., Setia Gunawan, D. Y. A., Sutantyo, W., van den Heuvel, E. P. J., Cuyper, J-P., & Gomez, A. E. (1998). Wolf-Rayet stars and O-stars runaways with HIPPARCOS. II. Photometry. Astronomy & Astrophysics, 331, 1022-1036. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:30 Sep 2021 Astron. -
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A&A 411, 465–475 (2003) Astronomy DOI: 10.1051/0004-6361:20031330 & c ESO 2003 Astrophysics Shocked gas layers surrounding the WR nebula NGC 2359 J. R. Rizzo1;2,J.Mart´ın-Pintado3, and J.-F. Desmurs2 1 Departamento de F´ısica, Universidad Europea de Madrid, Urb. El Bosque, Tajo s/n, 28670 Villaviciosa de Od´on, Spain 2 Observatorio Astron´omico Nacional, Aptdo. Correos 1143, 28800 Alcal´a de Henares, Spain 3 Departamento de Astrof´ısica Molecular e Infrarroja, Instituto de Estructura de la Materia, CSIC, Serrano 121, 28006 Madrid, Spain Received 11 June 2003 / Accepted 22 August 2003 Abstract. NGC 2359 is a Wolf-Rayet (W-R) nebula partially bound by a rather dense and warm molecular cloud. We present 13 the results derived from CO and CO fully sampled maps of the molecular material with angular resolutions up to 1200.Wehave detected three different velocity components, and determined their spatial distribution and physical properties. The kinematics, morphology, mass and density are clearly stratified with respect to the W-R star. These features allow us to learn about the recent evolutionary history of HD 56925, because the multiple layers could be associated to several energetic events which have acted upon the surrounding circumstellar medium. Hence, a careful study of the different shockfronts contain clues in determining the present and past interaction of this evolved massive star with its surroundings. From the analysis of the mass-loss history in massive stars like HD 56925, we suggest that the multiple layers of shocked molecular gas are likely to be produced during the earlier LBV phase and/or the actual W-R stage of HD 56925. -
Hot Gas in the Wolf-Rayet Nebula NGC3199
Accepted for publication in ApJ - 2017 HOT GAS IN THE WOLF-RAYET NEBULA NGC 3199 J.A. Toala(´ 杜宇君) 1,2, A.P. Marston3, M.A.Guerrero4, Y.-H.Chu(朱有花) 1, and R.A.Gruendl5 1Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA), Taipei 10617, Taiwan 2Instituto de Radioastronom´ıa y Astrof´ısica, UNAM Campus Morelia, Apartado postal 3-72, Morelia 58090, Michoac´an, Mexico 3European Space Agency/STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA 4Instituto de Astrof´ısica de Andaluc´ıa, IAA-CSIC, Glorieta de la Astronom´ıa s/n, Granada 18008, Spain 5Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801, USA ABSTRACT The Wolf-Rayet (WR) nebula NGC 3199 has been suggested to be a bow shock around its central star WR 18, presumably a runaway star, because optical images of the nebula show a dominating arc of emission south-west of the star. We present the XMM-Newton detection of extended X-ray emission from NGC 3199, unveiling the powerful effect of the fast wind from WR 18. The X-ray emission is brighter in the region south-east of the star and analysis of the spectral properties of the X-ray emission reveals abundance variations: i) regions close to the optical arc present nitrogen-rich gas enhanced by the stellar wind from WR 18 and ii) gas at the eastern region exhibits abundances close to those reported for nebular abundances derived from optical studies, signature of an efficient mixing of the nebular material with the stellar wind. The dominant plasma temperature and electron density are 6 −3 estimated to be T ≈ 1.2×10 K and ne=0.3 cm with an X-ray luminosity in the 0.3–3.0 keV energy 34 −1 range of LX=2.6×10 erg s . -
Diagnostics of the Unstable Envelopes of Wolf-Rayet Stars L
Astronomy & Astrophysics manuscript no. 27873_am c ESO 2021 September 13, 2021 Diagnostics of the unstable envelopes of Wolf-Rayet stars L. Grassitelli1,? , A.-N. Chené2 , D. Sanyal1 , N. Langer1 , N. St.Louis3 , J.M. Bestenlehner4; 1, and L. Fossati5; 1 1 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany 2 Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720, USA 3 Département de Physique, Pavillon Roger Gaudry, Université Montréal, CP 6128, Succ. Centre-Ville, Montréal, H3C 3J7 Quebec, Canada 4 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 5 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria Received //, 2015 ABSTRACT Context. The envelopes of stars near the Eddington limit are prone to various instabilities. A high Eddington factor in connection with the iron opacity peak leads to convective instability, and a corresponding envelope inflation may induce pulsational instability. Here, we investigate the occurrence and consequences of both instabilities in models of Wolf-Rayet stars. Aims. We determine the convective velocities in the sub-surface convective zones to estimate the amplitude of the turbulent velocity at the base of the wind that potentially leads to the formation of small-scale wind structures, as observed in several Wolf-Rayet stars. We also investigate the effect of stellar wind mass loss on the pulsations of our stellar models. Methods. We approximated solar metallicity Wolf-Rayet stars in the range 2−17 M by models of mass-losing helium stars, computed with the Bonn stellar evolution code. We characterized the properties of convection in the envelope of these stars adopting the standard mixing length theory. -
Diagnostics of the Unstable Envelopes of Wolf-Rayet Stars L
A&A 590, A12 (2016) Astronomy DOI: 10.1051/0004-6361/201527873 & c ESO 2016 Astrophysics Diagnostics of the unstable envelopes of Wolf-Rayet stars L. Grassitelli1, A.-N. Chené2, D. Sanyal1, N. Langer1, N. St-Louis3, J. M. Bestenlehner4;1, and L. Fossati5;1 1 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: [email protected] 2 Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720, USA 3 Département de Physique, Pavillon Roger Gaudry, Université Montréal, CP 6128, Succ. Centre-Ville, Montréal, H3C 3J7 Québec, Canada 4 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 5 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria Received 1 December 2015 / Accepted 1 March 2016 ABSTRACT Context. The envelopes of stars near the Eddington limit are prone to various instabilities. A high Eddington factor in connection with the iron opacity peak leads to convective instability, and a corresponding envelope inflation may induce pulsational instability. Here, we investigate the occurrence and consequences of both instabilities in models of Wolf-Rayet stars. Aims. We determine the convective velocities in the sub-surface convective zones to estimate the amplitude of the turbulent velocity at the base of the wind that potentially leads to the formation of small-scale wind structures, as observed in several Wolf-Rayet stars. We also investigate the effect of stellar wind mass loss on the pulsations of our stellar models. Methods. We approximated solar metallicity Wolf-Rayet stars in the range 2−17 M by models of mass-losing helium stars, computed with the Bonn stellar evolution code. -
Bowl/All Star Game Records
BOWL/ALL STAR GAME RECORDS All-Time Bowl-Game Results And Attendance 3 Team-By-Team Results 18 Major Bowl-Game Annual Attendance Totals 33 Bowl Individual Record List 34 Bowl Team Record List 41 Bowl Longest Plays 52 Bowl Championship Series Results (1998-99 Through 2013-14) 54 College Football Playoff Results (Since 2014-15) 55 Bowl Championship Series Individual Record Lists (1998-99 Through 2013-14) 56 Bowl Championship Series Team Records List (1998-99 Through 2013-14) 62 BCS Longest Plays (1998-99 through 2013-14) 70 College Football Playoff Individual Record Lists (Since 2014- 15) 71 College Football Playoff Team Records List (Since 2014-15) 78 College Football Playoff Longest Plays (Since 2014-15) 88 Bowl Coaching Records 89 Conference Bowl Won Lost Records 128 Award Winners in Bowl Games 130 Heisman Trophy Winners in Bowl Games 143 Bowls and Polls 145 Bowl Game Facts 153 Special Regular- and Postseason Games 158 ALL-TIME BOWL-GAME RESULTS AND ATTENDANCE Date Game Result Attendance MAJOR BOWL GAMES 1/1/1969 Ohio St. 27, Southern California 16 102,063 1/1/1970 Southern California 10, Michigan 3 103,878 Rose Bowl 1/1/1971 Stanford 27, Ohio St. 17 103,839 Present Site: Pasadena, CA 1/1/1972 Stanford 13, Michigan 12 103,154 Stadium (Capacity): Rose Bowl (92,542) 1/1/1973 Southern California 42, Ohio St. 17 *106,869 1/1/1974 Ohio St. 42, Southern California 21 105,267 Playing Sites: Tournament Park, Pasadena (1902, 1916-22); Rose Bowl, 1/1/1975 Southern California 18, Ohio St.