Danny Steeghs University of Warwick
|
|
|
- Maude Harrison
- 5 years ago
- Views:
Transcription
1 Lecture 4 Danny Steeghs University of Warwick
2 Reconstruction techniques Danny Steeghs University of Warwick
3 Non-parametric methods Astro-tomography reconstruction tools: - Eclipse mapping Doppler Tomography Roche Tomography Echo Tomography
4 Eclipse Mapping Baptista (2015)
5 Regularized image reconstruction Baptista (2015)
6 Temperature profiles Baptista (2015)
7 The observers toolbox : spectroscopy accretion in compact binaries ; broad emission lines
8 Emission lines from a disk
9 Emission line diagnostics The presence of strong and Doppler broadened emission lines is indeed a key characteristic of accretion flows line emissivity radial velocity (km/s)
10 Doppler tomography using line profiles Time-dependent line profiles provide a powerful diagnostic as the binary components go through their orbits Each spectrum provides a snapshot of the binary dynamics at a given orbital phase = orientation Phase-resolved spectroscopy can build up a dataset of line profiles that contain sufficient information to invert these into images resolving the dynamics of accretion = image reconstruction through (de)projection = tomography Marsh & Horne (1986), Marsh (2001), Steeghs (2004)
11 Medical CAT: from sample to tomogram sample tomogram tomogram data scanne r computerized axial tomography
12 Imaging through fast spectroscopy time velocity we can observe the time dependent line profiles as a function of the binary orbit! The tomogram reconstructs the mean emission line distribution in the co-rotating frame Since our diagnostic is Doppler shift, our projection space is in velocity and not Cartesian coordinates
13 The inversion from data to image Just like CT-scanning, the inversion problem in its simplest form represents a Radon transform One performs a back-projection through the data I(Vx,Vy) = D(v, ) d Generally this is done together with Fourier-filtering to sharpen up the PSF of the reconstruction ; filtered backprojection Data is not perfect (noise, limited sampling, gaps) and often produced significant back-projection artifacts A more robust (but computationally expensive) reconstruction is obtained using regularised maximum likelihood methods
14 Iterative and regularised reconstruction Default DATA Entropy Goodness of fit Minimisation problem: IMAGE Lagrange multiplier represents balance between realism versus simplicity Q2 = 2 S
15 Numerical implementation Iterate the image values along a MEM trajectory until the maximum entropy solution is reached for the chosen Local 2 and entropy gradients are evaluated each iteration in order to steer the image =0 visualisation of a twoparameter problem best fit, complex image after Horne (1994) = poor fit, simplest image A numerical convergence criterion is evaluated in order to test whether the current solution is indeed the maximum entropy one
16 Reconstruction techniques compared observed data filtered straightback-projection back-projection
17 Entropy regularised fitting maximum (image) entropy serves as our Occam s razor in regularising the fit
18 Doppler coordinates angular resolution = time resolution Since our diagnostic is Doppler shift, our projection space is in velocity and not Cartesian coordinates Sensible compromise between spectral resolution, time resolution and S/N radial resolution = spectral resolution (after Horne 1991)
19 Mapping the accretion disks in binaries binary phase H velocity (km/s)
20 An accreting white dwarf (IP Peg) hydrogen helium the donor star in emission ionized helium (from Steeghs, 2001) the extended accretion disc
21 Tidal asymmetries revisited Smak 2001 Ogilvie 2002 Danny Steeghs
22 Modeling in Doppler space Do data versus model comparison in velocity space ; either (Vr, ) or (Vx,Vy) Danny Steeghs
23 Tidally induced and spiral in shape Model simulation Synthetic data from Steeghs & Stehle (1999) Dynamics easy to compare, quantitative emissivity modelling much harder Danny Steeghs
24 The 2001 outburst of WZ Sge ~35 nights with spectroscopy Period: 82 minutes White dwarf: M1~ 1 M Donor: 0.03 < M2 < 0.11 Distance: ~ 45pc
25 Time-lapsed reconstructions
26 Key snapshots day 3: two armed spiral, donor star, orbital humps day 13: weakened asymmetries, faded donor star, super-humps re-brightening of disc AND mass donor star day 19: cooler disk, strong donor star plus major growth in stream emission. Steeghs (2004) Danny Steeghs
27 Extra continuum & line emission near stream/spot start of super-humps, re-brightening prominent donor irradiation peak of gas stream feature in maps Apparent bright spot eclipse strength in photometry (Patterson et al. 2002) Danny Steeghs
28 Extra mass transfer, stream-disc interaction, or pure disc? emission lies along the ballistic stream which is independently fixed by the donor star the donor star is irradiated evolution is strictly along the stream amplitude of the event much stronger than the modulations on the super-cycle that correspond to the stream-disc interaction due to flexing disc and standard stream Day 19 a similar sequence of events in both photometry (bright spot like humps) as well as spectroscopy (stream like emission) certainly looks like a mass transfer burst Danny Steeghs
29 Mass transfer variations do happen Long-term AM Her Hessman et al. (2000) Low-states in BB Dor Rogriguez-Gil et al. 12 Danny Steeghs
30 From disks to binary parameters Ca II triplet reveals mass donor star L. van Spaandonk (2011)
WANTED THE TRUE BOUNCE -BACK SYSTEMS
WANTED THE TRUE BOUNCE -BACK SYSTEMS Paczynski, B. & Sienkiewicz, R., 1981, ApJ, 248, L27 Paczynski, 1981, AcA, 31, 1 After reach the period minimum the CVs should be evolving back toward longer periods
Accretion disk evolution in dwarf novae through outbursts: disk instability and mass-transfer instability cases
Mem. S.A.It. Vol. 83, 530 c SAIt 2012 Memorie della Accretion disk evolution in dwarf novae through outbursts: disk instability and mass-transfer instability cases R. Baptista Departamento de Física, Universidade
Short-period cataclysmic variables at Observatorio Astronomico Nacional IA UNAM.
Contrib. Astron. Obs. Skalnaté Pleso 43, 294 299, (214) Short-period cataclysmic variables at Observatorio Astronomico Nacional IA UNAM. S. Zharikov Observatorio Astronomico Nacional, Instituto de Astronomia,
arxiv:astro-ph/ v1 15 Jan 2002
1 arxiv:astro-ph/21233v1 15 Jan 22 On the Origin of Early Superhumps in WZ Sge-Type Stars Taichi Kato Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 66-852 tkato@kusastro.kyoto-u.ac.jp Abstract
Cataclysmic Variable Stars
Cataclysmic Variable Stars Modern Astronomy in Motion Jeffrey M. Bryant Product Manager Wolfram Research, Inc. Champaign, IL 61820 jeffb@wolfram.com October 22, 2002 1. Introduction. Cataclysmic variable
Doppler Imaging & Doppler Tomography. Ilian Iliev Institute of Astronomy & Rozhen NAO
Doppler Imaging & Doppler Tomography Ilian Iliev Institute of Astronomy & Rozhen NAO Indirect imaging of stellar surfaces and flattened structures means restoring spatial distribution of some physical
Synthetic Doppler maps of gaseous flows in semidetached binaries based on the results of 3D gas dynamical simulations
Hot Points in Astrophysics JINR, Dubna, Russia, August 22-26, 2 Synthetic Doppler maps of gaseous flows in semidetached binaries based on the results of 3D gas dynamical simulations D.V.Bisikalo, A.A.Boyarchuk,
High Time Resolution Photometry of V458 Vul
High Time Resolution Photometry of V458 Vul Samia Bouzid 2010 NSF/REU Program Physics Department, University of Notre Dame Advisor: Dr. Peter Garnavich High Time-Resolution Photometry of Nova V458 Vul
Radial velocity study of the intermediate polar EX Hydrae
Mem. S.A.It. Vol. 83, 637 c SAIt 2012 Memorie della Radial velocity study of the intermediate polar EX Hydrae A. Ramirez-Torres 1, J. Echevarria 1 and R. Michel 2 1 Instituto de Astronomía, Universidad
Unstable Mass Transfer
Unstable Mass Transfer When the mass ratios are large, or when the donor star has a deep convective layer (so R M-1/3), mass loss will occur on a dynamical timescale. The result will be common envelope
arxiv:astro-ph/ v1 25 Feb 1999
Mon. Not. R. Astron. Soc. 000, 1 12 (1999) Printed 1 February 2008 (MN LATEX style file v1.4) On the observability of spiral structures in CV accretion discs D. Steeghs 1, R. Stehle 2 1 Physics and Astronomy,
University of Warwick institutional repository:
University of Warwick institutional repository: http://go.warwick.ac.uk/wrap This paper is made available online in accordance with publisher policies. Please scroll down to view the document itself. Please
PoS(SSC2015)051. Multi-tomography of polars from SALT spectroscopy
from SALT spectroscopy Stephen B. Potter 1 South African Astronomical Observatory Cape Town, South Africa E-mail: sbp@saao.ac.za Enrico J. Kotze South African Astronomical Observatory and Astrophysics,
arxiv:astro-ph/ v1 3 Feb 2004
Astron. Nachr./AN 325, No. 0, 001 005 (2004) / DOI 10.1002/asna.20041XXXX What can we learn from Accretion Disc Eclipse Mapping experiments? RAYMUNDO BAPTISTA arxiv:astro-ph/0402059v1 3 Feb 2004 1. Introduction
Extreme gravity in neutron-star systems with XEUS
Extreme gravity in neutron-star systems with XEUS Mariano Méndez Kapteyn Astronomical Institute, University of Groningen, The Netherlands Probing strong gravitational fields Adapted from Kramer et al.
ASTRONOMY AND ASTROPHYSICS. Double dataset eclipse mapping of IP Peg
stron. strophys. 348, 145 153 (1999) ouble dataset eclipse mapping of IP Peg STRONOMY N STROPHYSIS ndreas obinger 1, Heinz arwig 1, Hauke Fiedler 1, Karl-Heinz Mantel 1, amir Šimić 2, and Sebastian Wolf
Dark spot, Spiral waves and the SW Sex behaviour: it is all about UX Ursae Majoris
Mon. Not. R. Astron. Soc., 1 16 (21) Printed 15 June 21 (MN LATEX style file v2.2) Dark spot, Spiral waves and the SW Sex behaviour: it is all about UX Ursae Majoris V. V. Neustroev 1, V. F. Suleimanov
The Chandra Galactic Bulge Survey. Manuel Torres (SRON/Nijmegen! RU)
The Chandra Galactic Bulge Survey Manuel Torres (SRON/Nijmegen RU) Peter Jonker 1,2, Rob Hynes 3, Chris Johnson 3, Tom Maccarone 4, Chris Britt 4, Gijs Nelemans 2, Serena Repetto 2, Tom Wevers 2, Danny
arxiv:astro-ph/ v1 1 Nov 2000
Doppler Tomography T.R. Marsh Department of Physics and Astronomy, Southampton University, Highfield, Southampton SO17 1BJ arxiv:astro-ph/0011020 v1 1 Nov 2000 Abstract. I review the method of Doppler
Dr. Reed L. Riddle. Close binaries, stellar interactions and novae. Guest lecture Astronomy 20 November 2, 2004
Dr. Reed L. Riddle Close binaries, stellar interactions and novae Guest lecture Astronomy 20 November 2, 2004 Gravitational Tides Look at the forces acting on one body orbiting another - more pull on closer
The role of SW Sex stars in the evolution of CVs
European Southern Observatory Chile Wild Stars in the West II, Tucson 2009 The orbital period distribution SW Sextantis stars in a nutshell Original definition (Thorstensen et al. 1991, AJ 102, 272): novalike
Astronomy. The Nature of Stars
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am The Nature of Stars Distances to stars A Star's brightness and Luminosity A Magnitude scale Color indicates a Star's temperature
Magnetic mapping of solar-type stars
Magnetic mapping of solar-type stars Pascal Petit figure: M. Jardine Magnetic mapping of solar-type stars introduction: scientific context tomographic tools magnetic maps of active stars stellar differential
Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Observing Highlights. Stars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Announcements Lab Observing Trip Next week: Tues (9/28) & Thurs (9/30) let me know ASAP if you have an official conflict (class, work) - website: http://astro.physics.uiowa.edu/~clang/sgu_fall10/observing_trip.html
NEW VIEWS OF SU UMA-TYPE DWARF NOVAE FROM SIMULTANEOUS OPTICAL AND NEAR- INFRARED OBSERVATIONS
NEW VIEWS OF SU UMA-TYPE DWARF NOVAE FROM SIMULTANEOUS OPTICAL AND NEAR- INFRARED OBSERVATIONS Makoto Uemura (Hiroshima University), and the Kanata team OUTLINE Superhump with time-series photometry with
Determining the Orbital Period of the Cataclysmic Variable CSS1204 Using Data from the Vatican Advanced Technology Telescope
Determining the Orbital Period of the Cataclysmic Variable CSS1204 Using Data from the Vatican Advanced Technology Telescope Amy Applegate 2012 NSF/REU Program Physics Department, University of Notre Dame
Original citation: van Spaandonk, L., et al. (2010). The mass of the white dwarf in GW Libra. Astrophysical Journal Letters, 715(2), pp. L109-L112. Permanent WRAP url: http://wrap.warwick.ac.uk/5734 Copyright
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
White Dwarfs in Binary Systems
Tom Marsh, Department of Physics, University of Warwick Slide 1 / 39 White Dwarfs in Binary Systems Tom Marsh Department of Physics, University of Warwick Collaborators: Steven Parsons, Madelon Bours,
arxiv:astro-ph/ v1 12 Dec 2003
Astronomy & Astrophysics manuscript no. revised February 2, 2008 (DOI: will be inserted by hand later) XMM-Newton observations of OY Car III: OM light curve modelling, X-ray timing and spectral studies
Stellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
! p. 1. Observations. 1.1 Parameters
1 Observations 11 Parameters - Distance d : measured by triangulation (parallax method), or the amount that the star has dimmed (if it s the same type of star as the Sun ) - Brightness or flux f : energy
U Gem Rediscussion of Radial Velocities and System Parameters. Józef I. S m a k
ACTA ASTRONOMICA Vol. 51 (2001) pp. 279 293 U Gem Rediscussion of Radial Velocities and System Parameters by Józef I. S m a k N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18,
Low state transitions in the nova-like cataclysmic variable HS Jeremy Shears. Abstract
Low state transitions in the nova-like cataclysmic variable HS 0506+7725 Jeremy Shears Abstract The twelve-year light curve of the nova-like cataclysmic variable HS 0506+7725 between 2006 April and 2018
X-ray observations of X-ray binaries and AGN
X-ray observations of X-ray binaries and AGN Tomaso M. Be!oni (INAF - Osservatorio Astronomico di Brera) (Visiting Professor, Univ. of Southampton) OUTLINE Lecture I: Accretion onto compact objects, X-ray
Accretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk
Accretion Disks Accretion Disks 1. Accretion Efficiency 2. Eddington Luminosity 3. Bondi-Hoyle Accretion 4. Temperature profile and spectrum of accretion disk 5. Spectra of AGN 5.1 Continuum 5.2 Line Emission
Photometry of the Dwarf Nova SDSS J in Outburst
Wils and Krajci, JAAVSO Volume 38, 2010 33 Photometry of the Dwarf Nova SDSS J094002.56+274942.0 in Outburst Tom Krajci Astrokolkhoz Observatory, P.O. Box 1351, Cloudcroft, New Mexico 88317; tom_krajci@tularosa.net
Black Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
arxiv:astro-ph/ v3 7 Jul 1999
Draft version November 23, 2013 Preprint typeset using L A TEX style emulateapj v. 04/03/99 THE QUIESCENT ACCRETION DISK IN IP PEG AT NEAR-INFRARED WAVELENGTHS C. S. Froning, E. L. Robinson, William F.
Lecture 16 The Measuring the Stars 3/26/2018
Lecture 16 The Measuring the Stars 3/26/2018 Test 2 Results D C B A Questions that I thought were unfair: 13, 18, 25, 76, 77, 80 Curved from 85 to 79 Measuring stars How far away are they? How bright are
7. BINARY STARS (ZG: 12; CO: 7, 17)
7. BINARY STARS (ZG: 12; CO: 7, 17) most stars are members of binary systems or multiple systems (triples, quadruples, quintuplets,...) orbital period distribution: P orb = 11 min to 10 6 yr the majority
AG Draconis. A high density plasma laboratory. Dr Peter Young Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B.
AG Draconis A high density plasma laboratory Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B. Ake p.r.young@rl.ac.uk Overview CHIANTI database Symbiotic Stars AG Draconis FUSE FUSE observations of AG
Evolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
White Dwarf Binaries in Contact: Dynamical Stability at the Onset of Mass Transfer
White Dwarf Binaries in Contact: Dynamical Stability at the Onset of Mass Transfer Sterl Phinney* Caltech (*poor substitute for Danny Steeghs) KITP, Paths to Exploding Stars E.S. Phinney, 3/19/2007, 1
Energy Sources of the Far IR Emission of M33
Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also
Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION
Accretion Discs Mathematical Tripos, Part III Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION 0.1. Accretion If a particle of mass m falls from infinity and comes to rest on the surface of a star of mass
Lecture 13: Binary evolution
Lecture 13: Binary evolution Senior Astrophysics 2017-04-12 Senior Astrophysics Lecture 13: Binary evolution 2017-04-12 1 / 37 Outline 1 Conservative mass transfer 2 Non-conservative mass transfer 3 Cataclysmic
Based on the reduction of the intensity of the light from a star with distance. It drops off with the inverse square of the distance.
6/28 Based on the reduction of the intensity of the light from a star with distance. It drops off with the inverse square of the distance. Intensity is power per unit area of electromagnetic radiation.
Doppler tomography in cataclysmic variables: an historical perspective
Mem. S.A.It. Vol. 83, 570 c SAIt 2012 Memorie della Doppler tomography in cataclysmic variables: an historical perspective J. Echevarría Instituto de Astronomía, Universidad Nacional Autónoma de México,
Charles Keeton. Principles of Astrophysics. Using Gravity and Stellar Physics. to Explore the Cosmos. ^ Springer
Charles Keeton Principles of Astrophysics Using Gravity and Stellar Physics to Explore the Cosmos ^ Springer Contents 1 Introduction: Tools of the Trade 1 1.1 What Is Gravity? 1 1.2 Dimensions and Units
Chapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard 18.1 White Dwarfs What is a white dwarf? What can happen to a white dwarf in a close binary system? What supports
arxiv:astro-ph/ v1 25 Mar 1998
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 8 August 2018 (MN LATEX style file v1.4) A new method of determining the inclination angle in interacting binaries Tariq Shahbaz University of Oxford,
Relativistic Jets from the Black Hole in SS 433
Relativistic Jets from the Black Hole in SS 433 Herman L. Marshall and Laura A. Lopez with Claude R. Canizares, Norbert S. Schulz, and Julie F. Kane MIT Center for Space Research using NASA s Chandra X-ray
Indirect imaging of the accretion stream in eclipsing polars ± I. Method and tests
Mon. Not. R. Astron. Soc. 302, 362±372 (1999) Indirect imaging of the accretion stream in eclipsing polars ± I. Method and tests M. K. Harrop-Allin, 1 P. J. Hakala 1;2 and Mark Cropper 1 1 Mullard Space
U GEMINORUM: A TEST CASE FOR ORBITAL PARAMETER DETERMINATION
The Astronomical Journal, 134:262Y273, 2007 July # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. A U GEMINORUM: A TEST CASE FOR ORBITAL PARAMETER DETERMINATION Juan Echevarría,
Revealing the evolution of disks at au from high-resolution IR spectroscopy
Protoplanetary seen through the eyes of new-generation high-resolution instruments - Rome, June 6, 08 Revealing the evolution of at 0.0-0 au from high-resolution IR spectroscopy VLT IR interferometry (not
The Death of Stars. Today s Lecture: Post main-sequence (Chapter 13, pages ) How stars explode: supernovae! White dwarfs Neutron stars
The Death of Stars Today s Lecture: Post main-sequence (Chapter 13, pages 296-323) How stars explode: supernovae! White dwarfs Neutron stars White dwarfs Roughly the size of the Earth with the mass of
X-ray spectroscopy of low-mass X-ray binaries
X-ray spectroscopy of low-mass X-ray binaries Laurence Boirin Observatoire astronomique de Strasbourg (Handout version) Artistic impression of a low-mass X-ray binary An X-ray binary spectrum (from the
arxiv:astro-ph/ v1 12 Jul 1999
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 1 February 2008 (MN LATEX style file v1.4) A spatially resolved inside-out outburst of IP Pegasi arxiv:astro-ph/9907148v1 12 Jul 1999 N.A. Webb, 1
arxiv: v1 [astro-ph.sr] 4 May 2009
![arxiv: v1 [astro-ph.sr] 4 May 2009](/thumbs/93/112734420.jpg "arxiv: v1 [astro-ph.sr] 4 May 2009")
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 4 May 2009 (MN LATEX style file v2.2) The eclipsing Intermediate Polar V597 Pup (Nova Puppis 2007) arxiv:0905.0325v1 [astro-ph.sr] 4 May 2009 Brian
Review Chapter 10. 2) A parsec is slightly more than 200,000 AU. 2)
Review Chapter 10 TRUE/FALSE. Write 'T' if the statement is true and 'F' if the statement is false. 1) A parsec is about 3.3 light-years. 1) 2) A parsec is slightly more than 200,000 AU. 2) 3) The nearest
A parameter study of the eclipsing CV in the Kepler field, KIS J
doi:10.1093/mnras/stu1158 A parameter study of the eclipsing CV in the Kepler field, KIS J192748.53+444724.5 S. P. Littlefair, 1 V. S. Dhillon, 1 B. T. Gänsicke, 2 M. C. P. Bours, 2 C. M. Copperwheat 3
simulations - 1 J A Sellwood
simulations - 1 J A Sellwood Collisionless stellar systems Manifest a number of complicated collective phenomena spiral arms, bar instabilities, collapses, mergers, etc. too complicated to be calculated
Distribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars
High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars Distribution of X-ray binary stars in the Galaxy (RXTE) Robert Laing Primary Compact accreting binary systems Compact star WD NS BH
Phase-resolved high-resolution spectrophotometry of the eclipsing polar HU Aquarii
Astron. Astrophys. 319, 894 908 (1997) ASTRONOMY AND ASTROPHYSICS Phase-resolved high-resolution spectrophotometry of the eclipsing polar HU Aquarii Axel D. Schwope 1,, Karl-Heinz Mantel 2,, and Keith
Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is
Long-Term Photometry of HADS
Long-Term Photometry of HADS Patrick Wils Vereniging Voor Sterrenkunde, Belgium 1 Dwarf Cepheids / RRs Delta Scuti stars On or near the main sequence Pre- (T Tau) + post-ms Spectral type A-F Cepheid instability
arxiv:astro-ph/ v1 23 Oct 2002
Evolution of the symbiotic nova RX Puppis J. Mikołajewska, E. Brandi, L. Garcia, O. Ferrer, C. Quiroga and G.C. Anupama arxiv:astro-ph/0210505v1 23 Oct 2002 N. Copernicus Astronomical Center, Bartycka
The mathematics behind Computertomography
Radon transforms The mathematics behind Computertomography PD Dr. Swanhild Bernstein, Institute of Applied Analysis, Freiberg University of Mining and Technology, International Summer academic course 2008,
Determining the Properties of the Stars
Determining the Properties of the Stars This set of notes by Nick Strobel covers: The properties of stars--their distances, luminosities, compositions, velocities, masses, radii, and how we determine those
PoS(APCS2016)050. Superhumps in SU Uma Dwarf Novae
Sternberg Astronomical Institute, Moscow M.V.Lomonosov State University E-mail: voloshina.ira@gmail.com Dwarf novae belong to the class of cataclysmic variables and represent the close binary systems in
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Final Exam
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Physics 8.282J EAPS 12.402J May 20, 2005 Final Exam Name Last First (please print) 1. Do any
Stellar Astronomy Sample Questions for Exam 3
Stellar Astronomy Sample Questions for Exam 3 Chapter 7 1. A protostar is formed by a) the rapid expansion of gas from an exploding star. b) the gravitational collapse of a rotating interstellar cloud.
Exoplanet Search Techniques: Overview. PHY 688, Lecture 28 April 3, 2009
Exoplanet Search Techniques: Overview PHY 688, Lecture 28 April 3, 2009 Course administration final presentations Outline see me for paper recommendations 2 3 weeks before talk see me with draft of presentation
Superhumps in V348 Pup
Mon. Not. R. Astron. Soc. 000, 1 13 (2000) Printed 27 November 2018 (MN LATEX style file v1.4) Superhumps in V348 Pup Daniel J. Rolfe, 1 Carole A. Haswell, 1 and Joseph Patterson 2 1 Department of Physics
The cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
Searching for Other Worlds
Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats
The Binary System VV Cephei Eclipse Campaign 2017/2019 OHP-Meeting July 2017
The Binary System VV Cephei Eclipse Campaign 2017/2019 OHP-Meeting July 2017 Ernst Pollmann International Working Group Active Spectroscopy in Astronomy http://astrospectroscopy.de 3 One of the best known
Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
Atomic Structure & Radiative Transitions
Atomic Structure & Radiative Transitions electron kinetic energy nucleus-electron interaction electron-electron interaction Remember the meaning of spherical harmonics Y l, m (θ, ϕ) n specifies the
Disk Instabilities in Close Binary Systems 25 Years of the Disk-Instability Model
Disk Instabilities in Close Binary Systems 25 Years of the Disk-Instability Model Proceedings of the Disk-Instability Workshop on "Disk Instabilities in Close Binary Systems" held on October 27-30, 1998,
Photometric and spectroscopic observations of the outburst of the symbiotic star AG Draconis between March and June 2016
Photometric and spectroscopic observations of the outburst of the symbiotic star AG Draconis between March and June 2016 David Boyd Variable Star Section, British Astronomical Association, [davidboyd@orion.me.uk]
Gaia Photometric Data Analysis Overview
Gaia Photometric Data Analysis Overview Gaia photometric system Paola Marrese Sterrewacht Leiden marrese@strw.leidenuniv.nl Role of photometry in overall Gaia data analysis Photometric data analysis goals
The Gravitational Microlensing Planet Search Technique from Space
The Gravitational Microlensing Planet Search Technique from Space David Bennett & Sun Hong Rhie (University of Notre Dame) Abstract: Gravitational microlensing is the only known extra-solar planet search
Characterizing Stars
Characterizing Stars 1 Guiding Questions 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
Physics Homework Set I Su2015
1) The particles which enter into chemical reactions are the atom's: 1) _ A) protons. B) positrons. C) mesons. D) electrons. E) neutrons. 2) Which of the following type of electromagnetic radiation has
Characterizing Stars. Guiding Questions. Parallax. Careful measurements of the parallaxes of stars reveal their distances
Guiding Questions Characterizing Stars 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
Realistic limitations of detecting planets around young active stars
Realistic limitations of detecting planets around young active stars Sandra Jeffers IAG Goettingen In collaboration with: John Barnes, Hugh Jones, David Pinfield (Hertfordshire, UK) + ROPACS Impact of
Science Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
The low states of CVs at the upper edge of the period gap
Mem. S.A.It. Vol. 83, 602 c SAIt 2012 Memorie della The low states of CVs at the upper edge of the period gap P. Rodríguez-Gil 1,2, L. Schmidtobreick 3, K. S. Long 4, T. Shahbaz 1,2, B. T. Gänsicke 5,
Types of Stars 1/31/14 O B A F G K M. 8-6 Luminosity. 8-7 Stellar Temperatures
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars For nearby stars - measure distances with parallax 1 AU d p 8-2 Parallax A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3
Cataclysmic variables
Cataclysmic variables Sander Bus Kapteyn Astronomical Institute Groningen October 6, 2011 Overview Types of cataclysmic stars How to form a cataclysmic variable X-ray production Variation in outburst lightcurve,
Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances
Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers
Measuring Radial & Tangential Velocity. Radial velocity measurement. Tangential velocity measurement. Measure the star s Doppler shift
17. The Nature of the Stars Parallax reveals stellar distance Stellar distance reveals luminosity Luminosity reveals total energy production The stellar magnitude scale Surface temperature determines stellar
Rocket experiments. Sco X-1. Giacconi et al. 1962
X-ray binaries Rocket experiments. Sco X-1 Giacconi et al. 1962 Binaries are important and different! Wealth of observational manifestations: Visual binaries orbits, masses Close binaries effects of mass
Astrophysical Quantities
Astr 8300 Resources Web page: http://www.astro.gsu.edu/~crenshaw/astr8300.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html (ApJ, AJ, MNRAS, A&A, PASP, ARAA, etc.) General astronomy-type
An introduction to closure phases
An introduction to closure phases Michelson Summer Workshop Frontiers of Interferometry: Stars, disks, terrestrial planets Pasadena, USA, July 24 th -28 th 2006 C.A.Haniff Astrophysics Group, Department
Several Methods of Estimating Times of Minima in Cataclysmic Variables And Some Fesults for EX Dra
WDS'2 Proceedings of Contributed Papers, Part III, 6 22, 22. ISBN 978-8-7378-226-9 MATFYZPRESS Several Methods of Estimating Times of Minima in Cataclysmic Variables And Some Fesults for EX Dra L. Pilarčík
Accretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche