Curriculum Vitae Stephan Robert Mccandliss
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Accretion Flows in Nonmagnetic White Dwarf Binaries As Observed in X-Rays
Accretion Flows in Nonmagnetic White Dwarf Binaries as Observed in X-rays Şölen Balmana,< aKadir Has University, Faculty of Engineering and Natural Sciences, Cibali 34083, Istanbul, Turkey ARTICLEINFO ABSTRACT Keywords: Cataclysmic Variables (CVs) are compact binaries with white dwarf (WD) primaries. CVs and other cataclysmic variables - accretion, accre- accreting WD binaries (AWBs) are useful laboratories for studying accretion flows, gas dynamics, tion disks - thermal emission - non-thermal outflows, transient outbursts, and explosive nuclear burning under different astrophysical plasma con- emission - white dwarfs - X-rays: bina- ditions. They have been studied over decades and are important for population studies of galactic ries X-ray sources. Recent space- and ground-based high resolution spectral and timing studies, along with recent surveys indicate that we still have observational and theoretical complexities yet to an- swer. I review accretion in nonmagnetic AWBs in the light of X-ray observations. I present X-ray diagnostics of accretion in dwarf novae and the disk outbursts, the nova-like systems, and the state of the research on the disk winds and outflows in the nonmagnetic CVs together with comparisons and relations to classical and recurrent nova systems, AM CVns and Symbiotic systems. I discuss how the advective hot accretion flows (ADAF-like) in the inner regions of accretion disks (merged with boundary layer zones) in nonmagnetic CVs explain most of the discrepancies and complexities that have been encountered in the X-ray observations. I stress how flickering variability studies from optical to X-rays can be probes to determine accretion history and disk structure together with how the temporal and spectral variability of CVs are related to that of LMXBs and AGNs. -
Správa O Činnosti Organizácie SAV Za Rok 2017
Astronomický ústav SAV Správa o činnosti organizácie SAV za rok 2017 Tatranská Lomnica január 2018 Obsah osnovy Správy o činnosti organizácie SAV za rok 2017 1. Základné údaje o organizácii 2. Vedecká činnosť 3. Doktorandské štúdium, iná pedagogická činnosť a budovanie ľudských zdrojov pre vedu a techniku 4. Medzinárodná vedecká spolupráca 5. Vedná politika 6. Spolupráca s VŠ a inými subjektmi v oblasti vedy a techniky 7. Spolupráca s aplikačnou a hospodárskou sférou 8. Aktivity pre Národnú radu SR, vládu SR, ústredné orgány štátnej správy SR a iné organizácie 9. Vedecko-organizačné a popularizačné aktivity 10. Činnosť knižnično-informačného pracoviska 11. Aktivity v orgánoch SAV 12. Hospodárenie organizácie 13. Nadácie a fondy pri organizácii SAV 14. Iné významné činnosti organizácie SAV 15. Vyznamenania, ocenenia a ceny udelené organizácii a pracovníkom organizácie SAV 16. Poskytovanie informácií v súlade so zákonom o slobodnom prístupe k informáciám 17. Problémy a podnety pre činnosť SAV PRÍLOHY A Zoznam zamestnancov a doktorandov organizácie k 31.12.2017 B Projekty riešené v organizácii C Publikačná činnosť organizácie D Údaje o pedagogickej činnosti organizácie E Medzinárodná mobilita organizácie F Vedecko-popularizačná činnosť pracovníkov organizácie SAV Správa o činnosti organizácie SAV 1. Základné údaje o organizácii 1.1. Kontaktné údaje Názov: Astronomický ústav SAV Riaditeľ: Mgr. Martin Vaňko, PhD. Zástupca riaditeľa: Mgr. Peter Gömöry, PhD. Vedecký tajomník: Mgr. Marián Jakubík, PhD. Predseda vedeckej rady: RNDr. Luboš Neslušan, CSc. Člen snemu SAV: Mgr. Marián Jakubík, PhD. Adresa: Astronomický ústav SAV, 059 60 Tatranská Lomnica http://www.ta3.sk Tel.: 052/7879111 Fax: 052/4467656 E-mail: [email protected] Názvy a adresy detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty Dúbravská cesta 9, 845 04 Bratislava Vedúci detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty prof. -
Red Giant Mass-Loss: Studying Evolved Stellar Winds with FUSE and HST/STIS
Red Giant Mass-Loss: Studying Evolved Stellar Winds with FUSE and HST/STIS A dissertation submitted to the University of Dublin for the degree of Doctor of Philosophy Cian Crowley Supervisor: Dr. Brian R. Espey Trinity College Dublin, July 2006 School of Physics University of Dublin Trinity College Dublin ii For Mam and Dad Declaration I hereby declare that this thesis has not been submitted as an exercise for a degree at this or any other University and that it is entirely my own work. I agree that the Library may lend or copy this thesis upon request. Signed, Cian Crowley July 25, 2006. Publications Crowley, C., Espey, B. R.,. & McCandliss, S. R., 2006, In prep., ‘FUSE and HST/STIS Observations of the Eclipsing Symbiotic Binary EG Andromedae’ Acknowledgments I wish to acknowledge and thank Brian Espey, Stephan McCandliss and Peter Hauschildt for their contributions to this work. Most especially I would like to express my gratitude to my supervisor Brian Espey for his enthusiastic supervision, patience and encourage- ment. His help, support and advice is very much appreciated. In addition, the helpful and insightful comments and advice from numerous people, inlcuding, Graham Harper, Philip Bennett, Alex Brown, Gary Ferland, Tom Ake, B-G Anderson and Dugan With- erick, were invaluable and again, very much appreciated. Also, a special word of thanks for their viva comments and feedback for Alex Brown and Peter Gallagher. This work was supported by Enterprise Ireland Basic Research grant SC/2002/370 from EU funded NDP. The FUSE data were obtained under the Guest Investigator Pro- gram and supported by NASA grants NAG5-8994 and NAG5-10403 to the Johns Hopkins University (JHU). -
Spectropolarimetry As a Probe of Stellar Winds
Spectropolarimetry as a Probe of Stellar Winds Timothy James Harries Thesis submitted for the degree of Doctor of Philosophy in the Faculty of Science of the University of London. UCL Department of Physics & Astronomy U n iv e r s it y • C o l l e g e • L o n d o n February 1995 ProQuest Number: 10045605 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest. ProQuest 10045605 Published by ProQuest LLC(2016). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States Code. Microform Edition © ProQuest LLC. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 Abstract The use of spectropolarimetry as a diagnostic probe of stellar-wind structure is inves tigated by using high-quality observations and state-of-the-art analytical and numerical models. The winds of late-type giant stars are studied through the highly polarized 6830Â and 7088Â Raman-scattered emission hnes that are observed in many symbiotic systems. A spectropolarimetric survey of 28 symbiotic stars is presented. A Monte-Carlo code is developed in order to aid interpretation of the hnes and the parameter sensitivity of the Raman hne polarization spectrum is investigated. -
Appendix: Spectroscopy of Variable Stars
Appendix: Spectroscopy of Variable Stars As amateur astronomers gain ever-increasing access to professional tools, the science of spectroscopy of variable stars is now within reach of the experienced variable star observer. In this section we shall examine the basic tools used to perform spectroscopy and how to use the data collected in ways that augment our understanding of variable stars. Naturally, this section cannot cover every aspect of this vast subject, and we will concentrate just on the basics of this field so that the observer can come to grips with it. It will be noticed by experienced observers that variable stars often alter their spectral characteristics as they vary in light output. Cepheid variable stars can change from G types to F types during their periods of oscillation, and young variables can change from A to B types or vice versa. Spec troscopy enables observers to monitor these changes if their instrumentation is sensitive enough. However, this is not an easy field of study. It requires patience and dedication and access to resources that most amateurs do not possess. Nevertheless, it is an emerging field, and should the reader wish to get involved with this type of observation know that there are some excellent guides to variable star spectroscopy via the BAA and the AAVSO. Some of the workshops run by Robin Leadbeater of the BAA Variable Star section and others such as Christian Buil are a very good introduction to the field. © Springer Nature Switzerland AG 2018 M. Griffiths, Observer’s Guide to Variable Stars, The Patrick Moore 291 Practical Astronomy Series, https://doi.org/10.1007/978-3-030-00904-5 292 Appendix: Spectroscopy of Variable Stars Spectra, Spectroscopes and Image Acquisition What are spectra, and how are they observed? The spectra we see from stars is the result of the complete output in visible light of the star (in simple terms). -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
Wind Mass Transfer in S-Type Symbiotic Binaries III. Confirmation of a Wind
Astronomy & Astrophysics manuscript no. 39103 ©ESO 2020 December 16, 2020 Wind mass transfer in S-type symbiotic binaries⋆ III. Confirmation of a wind focusing in EG Andromedae from the nebular [O iii] λ5007 line N. Shagatova1, A. Skopal1, S. Yu. Shugarov1, 2, R. Komžík1, E. Kundra1, and F. Teyssier3 1 Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia e-mail: [email protected] 2 P.K. Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia 3 Observatoire Rouen Sud (FR) - ARAS group, 76100 Rouen, France Received / Accepted ABSTRACT Context. The structure of the wind from the cool giants in symbiotic binaries carries important information for understanding the wind mass transfer to their white dwarf companions, its fuelling, and thus the path towards different phases of symbiotic-star evolution. Aims. In this paper, we indicate a non-spherical distribution of the neutral wind zone around the red giant (RG) in the symbiotic binary star, EG And. We concentrate in particular on the wind focusing towards the orbital plane and its asymmetry alongside the orbital motion of the RG. Methods. We achieved this aim by analysing the periodic orbital variations of fluxes and radial velocities of individual components of the Hα and [O iii] λ5007 lines observed on our high-cadence medium (R 11 000) and high-resolution (R 38 000) spectra. Results. The asymmetric shaping of the neutral wind zone at the near-orbital-plane∼ region is indicated by: (i)∼ the asymmetric course of the Hα core emission fluxes along the orbit; (ii) the presence of their secondary maximum around the orbital phase ϕ = 0.1, which is possibly caused by the refraction effect; and (iii) the properties of the Hα broad wing emission originating by Raman scattering on H0 atoms. -
The Search for the Elusive Companion of EG Andromedae
The Search for the Elusive Companion of EG Andromedae Joseph E. Pesce and Robert E. Stencel Center for Astrophysics and Space Astronomy University of Colorado Boulder, CO 80309-0391 USA and Nancy A. Oliversen Computer Sciences Corporation Greenbelt, Maryland USA Abstract: We report observations at opposite quadratures of the interacting symbiotic binary EG Andromedae (HD 4174, Period = 470d). Correcting for absolute motion at the system, it appears that many of the nebular lines arise from material that moves with the red giant star. The He II feature appears to track the hot component. It may be possible to use this feature in other, similar systems in order to "pin-down" the mass ratio. The optical spectrum of EG Andromedae was first noted by Wilson (1950) to consist _1 of a high velocity (vr= -96 km s : Oliversen et al, 1985) M2 giant upon which were superposed the optical emission lines of 0 III] and the Balmer series. The ultraviolet spectrum exhibits a far UV continuum and emission lines of C IV, He II, 0 III] and other species. The companion star is thought to be similar to the central star of a planetary nebula (Kenyon 1983). Oliversen et al (1985) have used the spectroscopic motion of the red giant features and an estimate of the mass of the hot object (0.7 M©) to approximate the mass ratio of about 3.5. Oliversen et al report that the red giant optical absorption features undergo an esti mated 15 km s_1 total velocity excursion between orbital quadratures. With a mass ratio of 3.5, we predict that the hot object should exhibit 53 km s_1 in spectral line displace ment. -
Thermodynamics and Statistical Mechanics
Thermodynamics and Statistical Mechanics Richard Fitzpatrick Professor of Physics The University of Texas at Austin Contents 1 Introduction 7 1.1 IntendedAudience.................................. 7 1.2 MajorSources.................................... 7 1.3 Why Study Thermodynamics? ........................... 7 1.4 AtomicTheoryofMatter.............................. 7 1.5 What is Thermodynamics? . ........................... 8 1.6 NeedforStatisticalApproach............................ 8 1.7 MicroscopicandMacroscopicSystems....................... 10 1.8 Classical and Statistical Thermodynamics . .................... 10 1.9 ClassicalandQuantumApproaches......................... 11 2 Probability Theory 13 2.1 Introduction . .................................. 13 2.2 What is Probability? . ........................... 13 2.3 Combining Probabilities . ........................... 13 2.4 Two-StateSystem.................................. 15 2.5 CombinatorialAnalysis............................... 16 2.6 Binomial Probability Distribution . .................... 17 2.7 Mean,Variance,andStandardDeviation...................... 18 2.8 Application to Binomial Probability Distribution . ................ 19 2.9 Gaussian Probability Distribution . .................... 22 2.10 CentralLimitTheorem............................... 25 Exercises ....................................... 26 3 Statistical Mechanics 29 3.1 Introduction . .................................. 29 3.2 SpecificationofStateofMany-ParticleSystem................... 29 2 CONTENTS 3.3 Principle -
UV Spectroscopy of Massive Stars
galaxies Review UV Spectroscopy of Massive Stars D. John Hillier Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA; [email protected] Received: 11 July 2020; Accepted: 6 August 2020; Published: 12 August 2020 Abstract: We present a review of UV observations of massive stars and their analysis. We discuss O stars, luminous blue variables, and Wolf–Rayet stars. Because of their effective temperature, the UV (912 − 3200 Å) provides invaluable diagnostics not available at other wavebands. Enormous progress has been made in interpreting and analysing UV data, but much work remains. To facilitate the review, we provide a brief discussion on the structure of stellar winds, and on the different techniques used to model and interpret UV spectra. We discuss several important results that have arisen from UV studies including weak-wind stars and the importance of clumping and porosity. We also discuss errors in determining wind terminal velocities and mass-loss rates. Keywords: massive stars; O stars; Wolf–Rayet stars; UV; mass loss; stellar winds 1. Introduction According to Wien’s Law, the peak of a star’s energy distribution occurs in the UV for a star whose temperature exceeds 10,000 K. In practice, the temperature needs to exceed 10,000 K because of the presence of the Balmer jump. Temperatures greater than 10,000 K correspond to main-sequence stars of mass greater than ∼ 2 M and spectral types B9 and earlier. Early UV observations were made by rocket-flown instruments (e.g., [1,2]). -
COMMISSION 27 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 3001
COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 3001 - 3100 1987 March - 1987 October EDITORS: L. SZABADOS and B. SZEIDL KONKOLY OBSERVATORY H-1525 BUDAPEST P.O. Box 67, HUNGARY HU ISSN 0374 - 0676 CONTENTS 3001 PHOTOELECTRIC ELEMENTS AND REVISED SPECTRAL TYPES OF XX Cas R.K. Srivastava 18 March 1987 3002 HR 2554 - A POSSIBLE NEW Zeta Aur SYSTEM Thomas B. Ake, S.B. Parsons 19 March 1987 3003 53 PISCIUM - LARGER AMPLITUDE Marek Wolf 23 March 1987 3004 OBSERVATIONS AND A TIME OF MINIMUM OF TV Cet Daniel B. Caton, R. Lee Hawkins 25 March 1987 3005 ON THE PRIMARY MINIMUM OF ECLIPSING BINARY AY Cam J.B. Srivastava, C.D. Kandpal 30 March 1987 3006 AN UNEXPECTEDLY EARLY FADING OF V644 Cen (CPD -60d3278) J.K. Davies, A. Evans, M.F. Bode, D.C.B Whittet 3 April 1987 3007 PHOTOELECTRIC OBSERVATIONS OF TT ARIETIS ON 1/2 OCTOBER 1986 S. Rossiger 6 April 1987 3008 DELTA Cap: A POSSIBLE RS CVn BINARY R.K. Srivastava 9 April 1987 3009 ON THE CONSTANCY OF SOME STARS IN NGC 2287 = MESSIER 41 Brian A. Skiff 13 April 1987 3010 AN IMPROVEMENT OF THE ROTATIONAL PERIOD OF CQ UMa Zdenek Mikulasek 16 April 1987 3011 CORRECT PERIOD OF THE ECLIPSING STAR MN AURIGAE H. Gessner 16 April 1987 3012 JHK LIGHT CURVES OF CG CYGNI J.K. Davies, D.K. Bedford, J.J. Fuensalida, M.J. Arevalo 17 April 1987 3013 OPTICAL BEHAVIOUR OF THE X-RAY BINARY V1727 CYGNI = 4U 2129+47 IN 1986 W. -
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A&A 639, A18 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937305 & c ESO 2020 Astrophysics The nature of the companion in the Wolf-Rayet system EZ Canis Majoris G. Koenigsberger1 and W. Schmutz2 1 Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Ave. Universidad S/N, Cuernavaca 62210, Morelos, México e-mail: [email protected], [email protected] 2 Physikalisch-Meteorologisches Observatorium Davos and World Radiation Center, Dorfstrasse 33, 7260 Davos Dorf, Switzerland e-mail: [email protected] Received 12 December 2019 / Accepted 29 April 2020 ABSTRACT Context. EZ Canis Majoris is a classical Wolf-Rayet star whose binary nature has been debated for decades. It was recently modeled as an eccentric binary with a periodic brightening at periastron of the emission originating in a shock heated zone near the companion. Aims. The focus of this paper is to further test the binary model and to constrain the nature of the unseen close companion by searching for emission arising in the shock-heated region. Methods. We analyze over 400 high resolution International Ultraviolet Explorer spectra obtained between 1983 and 1995 and XMM- Newton observations obtained in 2010. The light curve and radial velocity (RV) variations were fit with the eccentric binary model and the orbital elements were constrained. −1 Results. We find RV variations in the primary emission lines with a semi-amplitude K1 ∼ 30 km s in 1992 and 1995, and a second −1 set of emissions with an anti-phase RV curve with K2 ∼ 150 km s . The simultaneous model fit to the RVs and the light curve yields the orbital elements for each epoch.