Annual Report 2009
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Multi-Periodic Photospheric Pulsations and Connected Wind Structures in HD 64760
A&A 447, 325–341 (2006) Astronomy DOI: 10.1051/0004-6361:20053847 & c ESO 2006 Astrophysics Multi-periodic photospheric pulsations and connected wind structures in HD 64760 A. Kaufer1,O.Stahl2,R.K.Prinja3, and D. Witherick3, 1 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 Landessternwarte Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 3 Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Received 18 July 2005 / Accepted 17 October 2005 ABSTRACT We report on the results of an extended optical spectroscopic monitoring campaign on the early-type B supergiant HD 64760 (B0.5 Ib) designed to probe the deep-seated origin of spatial wind structure in massive stars. This new study is based on high-resolution echelle spectra obtained with the Feros instrument at ESO La Silla. 279 spectra were collected over 10 nights between February 14 and 24, 2003. From the period analysis of the line-profile variability of the photospheric lines we identify three closely spaced periods around 4.810 h and a splitting of ±3%. The velocity – phase diagrams of the line-profile variations for the distinct periods reveal characteristic prograde non-radial pulsation patterns of high order corresponding to pulsation modes with l and m in the range 6−10. A detailed modeling of the multi-periodic non-radial pulsations with the Bruce and Kylie pulsation-model codes (Townsend 1997b, MNRAS, 284, 839) favors either three modes with l = −m and l = 8, 6, 8 or m = −6andl = 8, 6, 10 with the second case maintaining the closely spaced periods in the co-rotating frame. -
Luminous Blue Variables
Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs. -
A 1 Case-PR/ }*Rciofft.;Is Report
.A 1 case-PR/ }*rciofft.;is Report (a) This eruption site on Mauna Loa Volcano was the main source of the voluminous lavas that flowed two- thirds of the distance to the town of Hilo (20 km). In the interior of the lava fountains, the white-orange color indicates maximum temperatures of about 1120°C; deeper orange in both the fountains and flows reflects decreasing temperatures (<1100°C) at edges and the surface. (b) High winds swept the exposed ridges, and the filter cannister was changed in the shelter of a p^hoehoc (lava) ridge to protect the sample from gas contamination. (c) Because of the high temperatures and acid gases, special clothing and equipment was necessary to protect the eyes. nose, lungs, and skin. Safety features included military flight suits of nonflammable fabric, fuil-face respirators that are equipped with dual acidic gas filters (purple attachments), hard hats, heavy, thick-soled boots, and protective gloves. We used portable radios to keep in touch with the Hawaii Volcano Observatory, where the area's seismic activity was monitored continuously. (d) Spatter activity in the Pu'u O Vent during the January 1984 eruption of Kilauea Volcano. Magma visible in the circular conduit oscillated in a piston-like fashion; spatter was ejected to heights of 1 to 10 m. During this activity, we sampled gases continuously for 5 hours at the west edge. Cover photo: This aerial view of Kilauea Volcano was taken in April 1984 during overflights to collect gas samples from the plume. The bluish portion of the gas plume contained a far higher density of fine-grained scoria (ash). -
POSTERS SESSION I: Atmospheres of Massive Stars
Abstracts of Posters 25 POSTERS (Grouped by sessions in alphabetical order by first author) SESSION I: Atmospheres of Massive Stars I-1. Pulsational Seeding of Structure in a Line-Driven Stellar Wind Nurdan Anilmis & Stan Owocki, University of Delaware Massive stars often exhibit signatures of radial or non-radial pulsation, and in principal these can play a key role in seeding structure in their radiatively driven stellar wind. We have been carrying out time-dependent hydrodynamical simulations of such winds with time-variable surface brightness and lower boundary condi- tions that are intended to mimic the forms expected from stellar pulsation. We present sample results for a strong radial pulsation, using also an SEI (Sobolev with Exact Integration) line-transfer code to derive characteristic line-profile signatures of the resulting wind structure. Future work will compare these with observed signatures in a variety of specific stars known to be radial and non-radial pulsators. I-2. Wind and Photospheric Variability in Late-B Supergiants Matt Austin, University College London (UCL); Nevyana Markova, National Astronomical Observatory, Bulgaria; Raman Prinja, UCL There is currently a growing realisation that the time-variable properties of massive stars can have a funda- mental influence in the determination of key parameters. Specifically, the fact that the winds may be highly clumped and structured can lead to significant downward revision in the mass-loss rates of OB stars. While wind clumping is generally well studied in O-type stars, it is by contrast poorly understood in B stars. In this study we present the analysis of optical data of the B8 Iae star HD 199478. -
Annual Report 2008
Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Mensen voor Aarde en Ruimte , Aarde en Ruimte voor Mensen Des hommes et des femmes pour la Terre et l'Espace, La Terre et l'Espace pour l'Homme Jaarverslag 2008 Rapport Annuel 2008 Annual Report 2008 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid / Le SPP Politique Scientifique De Nationale Loterij La Loterie Nationale De Europese Gemeenschap Het Europees Ruimtevaartagentschap La Communauté Européenne L’Agence Spatiale Européenne Het Fond voor Wetenschappelijk Onderzoek Le Fonds de la Recherche Scientifique – Vlaanderen Le Fonds pour la formation à la Recherche dans l’Industrie et dans l’Agriculture (FRIA) Instituut voor de aanmoediging van innovatie door Wetenschap & Technologie in Vlaanderen Privé-sponsoring door Mr. G. Berthault / Sponsoring privé par M. G. Berthault 2 Deel 1: Wetenschappelijke activiteiten Partie 1: Activités Scientifiques Part 1: Scientific Activities 3 4 Summary Abbreviations.................................................................................................................................. 7 A. GNSS Positioning and Time............................................................................................. 14 A.1. Time and Time transfer .............................................................................................................15 -
New Journal of Physics the Open-Access Journal for Physics
New Journal of Physics The open-access journal for physics www.njp.org Highlights of 2011 Advancing physics research globally NJP is evolving We won’t just publish your work; we will help you share your research with others in new and innovative ways. By featuring the people WIth a NJP vIdeO abstract yOu caN: behind the science, video abstracts have •showcase your research the potential to convey •engage with your community inspiration and •raise your visibility enthusiasm, and thereby the significance •make an impact of scientific results, beyond the concise text By including a video abstract you can enhance the visibility of your of articles. article by more than five times. In 2011, NJP articles with video abstracts were downloaded (on average) more than1400 times each. Achim Kempf, Waterloo University, Canada To see the latest video abstracts and for more information visit www.njp.org/videoabstracts. New Journal of Physics: Highlights of 2011 New Journal of Physics – extending the global reach of physics research ImPact Factor 1,500,000 At a time when more and more journals are introducing open-access options in response to increasing demand from researchers, librarians, funding bodies and the general 1,000,0003.849* * As listed in ISI®’s 2010 Science public, New Journal of Physics (NJP) is proud to have the highest Impact Factor of all Citation Index Journal citation reports 500,000 ‘gold’ open-access journals in physics. 0 Providing a showcase for just some of our article highlights of the last 12 months, the 2007 2008 2009 2010 2011 citation performance abstracts collected here have been selected by our editorial team as a reflection of the 4.5 Impact Factor 1.4 quality, and the subject and geographical diversity of NJP’s broad coverage in 2011. -
Member Services 2018
AMERICAN PHYSICAL SOCIETY Member Services 2018 JANUARY – DECEMBER 2018 GUIDELINES FOR PROFESSIONAL CONDUCT The Constitution of the American Physical Society states that the objective of the Society shall be the advancement and diffusion of the knowledge of physics. It is the purpose of this statement to advance that objective by presenting ethical guidelines for Society members. Each physicist is a citizen of the community of science. Each shares responsibility for the welfare of this community. Science is best advanced when there is mutual trust, based upon honest behavior, throughout the community. Acts of deception, or any other acts that deliberately compromise the advancement of science, are unacceptable. Honesty must be regarded as the cornerstone of ethics in science. Professional integrity in the formulation, conduct, and report- ing of physics activities reflects not only on the reputations of individual physicists and their organizations, but also on the image and credibility of the physics profession as perceived by scientific colleagues, government and the public. It is important that the tradition of ethical behavior be carefully maintained and transmitted with enthusiasm to future generations. The following are the minimal standards of ethical behavior relating to several critical aspects of the physics profession. Physicists have an individual and a collective responsibility to ensure that there is no compromise with these guidelines. RESEARCH RESULTS The results of research should be recorded and maintained in a form that allows analysis and review. Research data should be immediately available to scientific collaborators. Following publication, the data should be retained for a reasonable period in order to be available promptly and completely to responsible scientists. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
Runaways and Shells Around the Cma OB1 Association B
Astronomy & Astrophysics manuscript no. cmashellpart1_rev c ESO 2019 June 4, 2019 Runaways and shells around the CMa OB1 association B. Fernandes1; 2, T. Montmerle1, T. Santos-Silva1; 2, and J. Gregorio-Hetem2 1 Institut d’Astrophysique de Paris, 75014, Paris, France 2 Universidade de São Paulo, IAG, Departamento de Astronomia, São Paulo, 05508-090, Brazil e-mail: [email protected] ABSTRACT Context. The origin of the arc-shaped Sh 2-296 nebula is still unclear. Mainly due to its morphology, the nebula has been suggested to be a 0.5 Myr-old supernova remnant (SNR) that could be inducing star formation in the CMa OB1 association. Therefore, this region can be an excellent laboratory for the investigation of the influence of massive stars on their surroundings. Aims. We aim to show, for the first time, that the nebula is part of a large, shell-like structure, which we have designated the “CMa shell”, enclosing a bubble created by successive supernova (SN) explosions. We identified three runaway stars, associated with bow- shock structures, in the direction of the CMa shell and we investigate the possibility that they have originated in the center of the shell. Methods. By analyzing images of the CMa OB1 association at several wavelengths, we clearly see that the Sh 2-296 nebula is in fact part of a large structure, which can be approximated by a large (with a diameter of ∼ 60 pc) elliptical shell. Using the recent Gaia-DR2 astrometric data, we trace back the path of the three runaway stars, in order to find their original position in the past, with relation to the CMa shell. -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
Curriculum Vitae Danny E. P. Vanpoucke
Curriculum Vitae Dr. Dr. Danny E. P. Vanpoucke Current Affiliation: Maastricht University Institute for Materials Research (IMO) Campus Diepenbeek, Wetenschapspark 1, 3590 Diepenbeek Belgium room: IMO-1.06 e-mail: [email protected] [email protected] personal webpage: https://dannyvanpoucke.be Work Experience 2020–2021: guest professor Hasselt University At the department of Chemistry of the UHasselt. (Belgium) Contributing to the development of a new master’s program at UHasselt. 2020–2021: Lecturer Hasselt University At the department of Physics of the UHasselt. (Belgium) Teaching experience: Lecturer : Statistical Physics 2019–2020: postdoc Maastricht University In the Aachen–Maastricht Institute for Biobased Materials (AMIBM) with Prof. Dr. K. Bernaerts (AMIBM) and Prof. Dr. S. Mehrkanoon (DKE), at the UMaastricht. (The Ne- therlands) Developing a Machine-Learning framework for small (experimental) data sets. 2017–2019: postdoc Hasselt University In the Wide Bandgap Materials group (WBGM) of Prof. Dr. K. Haenen, at the UHasselt. (Belgium) Teaching experience: Teaching assistant : Biophysics Lecturer : Functional Molecular Modeling 1/15 Curriculum Vitae Danny E. P. Vanpoucke Coordinator/Lecturer : Experimental Techniques Promoter Bachelor projects: -“Benchmarking DFT-functionals for periodic C-based materials” -“Are there atoms in molecules” 2014–2017: FWO postdoctoral Fellow Ghent University and Hasselt University In the Wide Bandgap Materials group (WBGM) of Prof. Dr. K. Haenen, at the UHasselt. (Belgium) Teaching -
Luminous Blue Variables: an Imaging Perspective on Their Binarity and Near Environment?,??
A&A 587, A115 (2016) Astronomy DOI: 10.1051/0004-6361/201526578 & c ESO 2016 Astrophysics Luminous blue variables: An imaging perspective on their binarity and near environment?;?? Christophe Martayan1, Alex Lobel2, Dietrich Baade3, Andrea Mehner1, Thomas Rivinius1, Henri M. J. Boffin1, Julien Girard1, Dimitri Mawet4, Guillaume Montagnier5, Ronny Blomme2, Pierre Kervella7;6, Hugues Sana8, Stanislav Štefl???;9, Juan Zorec10, Sylvestre Lacour6, Jean-Baptiste Le Bouquin11, Fabrice Martins12, Antoine Mérand1, Fabien Patru11, Fernando Selman1, and Yves Frémat2 1 European Organisation for Astronomical Research in the Southern Hemisphere, Alonso de Córdova 3107, Vitacura, 19001 Casilla, Santiago de Chile, Chile e-mail: [email protected] 2 Royal Observatory of Belgium, 3 avenue Circulaire, 1180 Brussels, Belgium 3 European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany 4 Department of Astronomy, California Institute of Technology, 1200 E. California Blvd, MC 249-17, Pasadena, CA 91125, USA 5 Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l’Observatoire, France 6 LESIA (UMR 8109), Observatoire de Paris, PSL, CNRS, UPMC, Univ. Paris-Diderot, 5 place Jules Janssen, 92195 Meudon, France 7 Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 8 ESA/Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218,