Wind Structure of Late B Supergiants I. Multi-Line Analyses of Near-Surface
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1970Aj 75. . 602H the Astronomical Journal
602H . 75. THE ASTRONOMICAL JOURNAL VOLUME 75, NUMBER 5 JUNE 19 70 The Space Distribution and Kinematics of Supergiants 1970AJ Roberta M. Humphreys *f University of Michigan, Ann Arbor, Michigan (Received 15 January 1970; revised 1 April 1970) The distribution and kinematics of the supergiants of all spectral types are investigated with special emphasis on the correlation of these young stars and the interstellar gas. The stars used for this study are included as a catalogue of supergiants. Sixty percent of these supergiants occur in stellar groups. Least- squares solutions for the Galactic rotation constants yield 14 km sec-1 kpc-1 for Oort’s constant and a meaningful result for the second-order coefficient of —0.6 km sec-1 kpc-2. A detailed comparison of the stellar and gas velocities in the same regions shows good agreement, and these luminous stars occur in relatively dense gas. The velocity residuals for the stars also indicate noncircular group motions. In the Carina-Centaurus region, systematic motions of 10 km/sec were found between the two sides of the arm in agreement with Lin’s density-wave theory. The velocity residuals in the Perseus arm may also be due in part to these shearing motions. I. INTRODUCTION II. THE CATALOGUE OF SUPERGIANTS SINCE the pioneering work of Morgan et al. (1952) The observational data required for this study were on the distances of Galactic H 11 regions, many largely obtained from the literature. Use of a card file investigators have studied the space distribution of compiled by Dr. W. P. Bidelman was very helpful in various Population I objects, the optical tracers of this regard. -
The Star Newsletter
THE HOT STAR NEWSLETTER ? An electronic publication dedicated to A, B, O, Of, LBV and Wolf-Rayet stars and related phenomena in galaxies ed. Philippe Eenens [email protected] No. 15 http://webhead.com/∼sergio/hot/ November-December 1995 http://www.inaoep.mx/∼eenens/hot/ From the editor This issue contains what we hope to be the first of a series of short commentaries. This one is on the photospheric connection. It would be useful to hear your comments, critics and complementary views. If you wish to write a commentary on another topic, please contact the newsletter editor. The news this month include plans for an X-ray observing campaign, notice of the launch of a newsletter on the Magellanic Clouds and information on the Liege colloquium (July) and on a colloquium on LBV stars (October). Best season wishes! Contents of this newsletter Commentary . 2 Abstracts of 10 accepted papers . 5 Abstracts of 5 submitted papers . 10 Abstracts of 3 proceedings papers . 12 Abstract of 1 dissertation thesis . 13 News ......................................................................14 1 Commentary Variability in the Photospheres and Stellar Winds of Hot Stars: The “Photospheric Connection” At Last? Alex Fullerton1,2 and Lex Kaper3 1 Max-Planck-Institut f¨urAstrophysik, Karl-Schwarzschild-Str. 1, 85740 Garching, Germany 2 Universit¨atsSternwarte M¨unchen, Scheinerstr. 1, 81679 M¨unchen, Germany 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany It has been slightly more than 10 years since a seminal workshop on “The Connection Between Non- radial Pulsations and Stellar Winds in Massive Stars” was hosted by JILA and the University of Colorado (Abbott et al. -
Simulación Y Análisis De La Capacidad Operativa Del Canal De Panamá
SIMULACIÓN Y ANÁLISIS DE LA CAPACIDAD OPERATIVA DEL CANAL DE PANAMÁ ANEXO B Tabla de Buques Típicos TableOfTypicalVessels Table Of Typical Vessels Sail Through Main Upper Dimension Limits (ft) Panamax Post-panamax LOA 966 1200 Beam 107 180 Copy Draft 39.5 46 Internal No. NAME Market Segment LR# BR# SR# Length Beam Laden Draft Ballast Draft PCUMS ACP I.N 1 18 DE MARZO Tankers 7 17 263 680.54 105.94 Tria(36.34, 37.92, 39.50) 26.67 25201 202312 1 2 550--1 Others 5 10 149 501.25 74.08 Tria(26.58, 26.58, 26.58) 17.22 9370 3002213 2 3 550--1 Others 5 10 149 501.25 74.08 Tria(22.75, 22.75, 22.75) 17.22 9370 3002328 3 4 AALSMEERGRACHT General Cargo 4 8 116 425.85 62.11 Tria(30.25, 30.25, 30.25) 17.87 6429 332585 4 5 ABAVA Refrigerated 4 8 116 408.46 63.06 Tria(22, 22, 22) 18.75 5208 329436 5 6 ABRA Dry Bulk 5 12 181 526.18 80.84 Tria(20.92, 20.92, 20.92) 19.10 11974 740519 6 7 ABSALON Others 7 12 183 604.82 83.19 Tria(27.92, 31.36, 33.75) 20.36 15316 268968 7 8 ACACIA N Dry Bulk 5 12 181 524.39 80.78 Tria(22.25, 30.76, 33.67) 20.91 11810 787434 8 9 ACTIVE Dry Bulk 4 9 132 420.08 69.65 Tria(24.5, 25.38, 26.25) 17.84 6700 809900 9 10 JOYOUS LAND Dry Bulk 8 17 264 738.12 105.77 Tria(38.42, 38.83, 39.25) 27.71 29707 792691 10 11 ACHILLES Dry Bulk 8 17 264 738.19 105.77 Tria(37.17, 38.58, 39.33) 22.77 30618 771694 11 12 ACHTERGRACHT General Cargo 4 8 116 425.85 62.07 Tria(23.17, 23.17, 23.17) 17.87 6611 329622 12 13 ACTIVE Dry Bulk 4 9 132 420.08 69.65 Tria(22.92, 25.75, 27.92) 17.84 6700 809900 13 14 ACUSHNET Tankers 6 16 246 587.93 99.84 Tria(31.5, -
Long-Term Spectroscopic Monitoring of BA Type Supergiants
Astron. Astrophys. 320, 273–286 (1997) ASTRONOMY AND ASTROPHYSICS Long-term spectroscopic monitoring of BA-type supergiants III. Variability of photospheric lines? A. Kaufer1, O. Stahl1, B. Wolf1, A.W. Fullerton4;5, Th. Gang¨ 1;3, C.A. Gummersbach1, I. Jankovics2,J.Kovacs´ 2, H. Mandel1, J. Peitz1, Th. Rivinius1, and Th. Szeifert1 1 Landessternwarte Heidelberg-Konigstuhl,¨ D-69117 Heidelberg, Germany 2 Gothard Astrophysical Observatory, H-9707 Szombathely, Hungary, 3 STScI, Homewood Campus, 3700 San Martin Drive, Baltimore MD 21218, USA 4 Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85740 Garching, Germany 5 Universitats-Sternwarte¨ Munchen,¨ Scheinerstr. 1, D-81679 Munchen,¨ Germany Received 5 September 1996 / Accepted 26 September 1996 Abstract. We obtained time series of spectra with high S/N 1. Introduction and high resolution in wavelength and time of early-type A and late-type B supergiants (cf. Kaufer et al. 1996a, Paper i, and Our extended spectroscopic monitoring of late B-type and early Kaufer et al. 1996b, Paper ii for the analysis of the variability A-type supergiants (Kaufer et al. 1996a, Paper i, Kaufer et of the stellar envelopes). In this work we inspect the time vari- al. 1996b, Paper ii; Stahl et al. 1995) has revealed for the first ations of the numerous photospheric line profiles in the optical time the complexity of the circumstellar structures of these lu- spectrum. We find complex cyclical variations of the radial ve- minous objects. The time-series analysis of the Hα line-profile 1 locities with a typical velocity dispersion of σ 3kms− . The variability gave strong hints that the envelopes deviate from corresponding equivalent-width variations are≈ less than 1% of spherical symmetry. -
The Flamsteed Collection
The Flamsteed Collection Compiled by Richard Dibon-Smith © 2001-2012 Richard Dibon-Smith all rights reserved Andromeda (I) AND HD HIP α δ B-V µ(α)″ µ(δ)″ µ″ Dir Spect. Var? α 358 677 00h08m23.2 s +29º05′26″ -0.038 0.1357 -0.1630 0.212 140º B9IV:pHgMn (ACV) β 6860 5447 01 09 43.9 +35 37 14 1.576 0.1756 -0.1122 0.208 123 M0IIIvar γ1 12533 9640A 02 03 53.9 +42 19 47 1.370 0.0431 -0.0509 0.067 140 K3IIb γ2B 12534 9640B 02 03 54.7 +42 19 51 0.030 0.0431 -0.0509 0.067 140 B9V γ2C 12534 9640C 02 03 54.7 +42 19 51 0.030 0.0431 -0.0509 0.067 140 A0V δ 3627 3092 00 39 19.6 +30 51 40 1.268 0.1154 -0.0831 0.142 126 K3III ε 3546 3031 00 38 33.3 +29 18 43 0.871 -0.2294 -0.2541 0.342 222 G5IIIcomp ζ 4502 3693 00 47 20.3 +24 16 02 1.100 -0.1012 -0.0819 0.130 231 K1II (EB/GS) η 5516 4463 00 57 12.4 +23 25 04 0.940 -0.0437 -0.0461 0.064 224 G8III-IV ϑ 1280 1366 00 17 05.4 +38 40 54 0.059 -0.0500 -0.0179 0.053 250 A2V ι 222173 116631 23 38 08.1 +43 16 05 -0.083 0.0277 -0.0012 0.028 92 B8V κ 222439 116805 23 40 24.4 +44 20 02 -0.071 0.0813 -0.0190 0.084 103 B9IVn λ 222107 116584 23 37 33.8 +46 27 30 0.984 0.1592 -0.4215 0.451 159 G8III-IV (RS) µ 5448 4436 00 56 45.1 +38 29 58 0.130 0.1528 0.0368 0.157 76 A5V ν 4727 3881 00 49 48.8 +41 04 44 -0.136 0.0227 -0.0181 0.029 129 B5V SB ξ 8207 6411 01 22 20.3 +45 31 44 1.077 0.0322 0.0087 0.033 75 K0III-IV οΑ 217675 113726A 23 01 55.2 +42 19 34 -0.099 0.0225 0.0002 0.022 89 B6IIIpe+A2p (GCAS) οΒ 217675 113726B 23 01 55.2 +42 19 34 -0.099 0.0225 0.0002 0.022 89 – π 3369 2912 00 36 52.8 +33 43 10 -0.123 0.0152 -0.0036