DOCSLIB.ORG

Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity Open Research Online The Open University’s repository of research publications and other research outputs Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity Thesis How to cite: Pagomenos, George (2019). Gas and Dust in Galactic Planetary Nebulae at Sub-Solar Metallicity. PhD thesis The Open University. For guidance on citations see FAQs. c 2018 The Author https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.21954/ou.ro.0000e4a2 https://drive.google.com/file/d/1wKDTzpp87LQPAbsS0OZ45eT59LQXUmjX/view?usp=sharing Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Gas and dust in Galactic planetary nebulae at sub-solar metallicity George James Steven Pagomenos School of Physical Sciences, Faculty of STEM The Open University This thesis is submitted for the degree of Doctor of Philosophy August 2018 Abstract Planetary nebulae are the final phases of evolution for low- to intermediate-mass stars(∼ 0.8– 8 M⊙). They consist of a central star surrounded predominantly by a circumstellar envelope containing the products of nuclear processing, and a photodissociation region containing dust and molecules. These include silicates and large organic molecules such as polycyclic aromatic hydrocarbons (PAHs), which are ubiquitous throughout the Universe, and fullerenes, which are the largest molecules to be firmly detected in space. All of this material coasts away from the central star, causing enrichment of the interstellar medium. Although there have been significant advances in studies of this circumstellar material, we still do not fully understand how the metallicity (i.e. the abundance of elements heavier than helium) of the local environment affects the dust composition around these stars, or the processes that govern the formation and evolution of these large organic molecules. This thesis presents a series of studies in which the abundances and dust composition around planetary nebulae are characterised in the low metallicity regions of the Milky Way, with use of data from the Spitzer Space Telescope and SOFIA. These include investigations into the metallicity and dust content of planetary nebulae in the outer thin disk and the halo of the Galaxy, and the physical conditions in which large organic molecules form. I find that the outer regions of the Galactic disk have a lower metallicity than thesolar neighbourhood, and that regions of low metallicity favour carbon-rich dust production over oxygen-rich dust (i.e. silicates), except for within the Galactic halo. These regions show a greater diversity of carbonaceous material than observed towards the Galactic bulge and in the solar neighbourhood. Fullerenes are preferentially formed in environments with low hydrogen density. Acknowledgements Firstly, I could not have been able to chase my dream of being a scientist if it wasn’t for my family. In particular, I would like to thank Mum, Dad, Gran, Mike, Yiayia, Pappou, Isabel, Tony, Nick and Chris for all their love and support over the years. I am incredibly fortunate to have worked with my two supervisors, Jeronimo Bernard- Salas and Helen Fraser. Jeronimo, thank you for providing me with the incredible opportunity to carry out this research, and with another to get involved with the JWST Evolved Stars working group. You have always pushed me to strive to do better, and your support and patience has always been appreciated. Helen, thank you for keeping me on track, and for providing a positive outlook when I needed perspective. You have both been amazing. To everyone else with whom I have collaborated, namely Jan Cami, Els Peeters, Greg Sloan, Albert Zijlstra and the late Stuart Pottasch: thank you for everything, it has genuinely been wonderful working with all of you. I would also like to thank Maria Lugaro and Carolyn Doherty for inviting me to give a seminar talk at the Konkoly Observatory, Harriet Dinerstein for the inspiring scientific conversations, all members of the Astrochemistry Group and Astronomy Journal Club at the Open University with whom I have been able to share ideas, Geoff Bradshaw for the IT assistance, and Stephen Serjeant, Nicolas Peretto and Judith Croston for reading this thesis and assessing my viva. Thanks to Philip, for being like a brother; Kieran, for the wine evenings and the con- versations in which we set the world to rights; Jack and Tania, for hosting us in Japan for the week; Laura and David, for helping me take the next steps in my career and generally being awesome people; Lawrence, Ashley and Paul for being brilliant flatmates; everyone in the DPS House Band; the Goat Army (you know who you are); Rachel, Mark, Helen and vi Graham for the semi-regular chats over coffees; and the rest of the “DeanSoc” crew: Dean, Joe, Meredith, Heidi, Aaron and Andy. Thanks also to Helen, Amit, Dan, Catherine, Natalia, Olivier, Paul, Pam, Calum, James, Jana, Ayo, Brendan, Maria, Vincent, Pete, Rhian, Amy, George, Aleksi, Sabrina, Feargus, Tom, Candice, Matt, Anton, Yasmin, Mike, Joe, Chris, Joanna and Alex; and anyone else who has been an essential component of my past few years but I have regrettably forgotten to mention here. And last but certainly not least, I wish to thank my partner of almost seven years, Anastasia. I am so lucky to have you in my life. Table of contents List of figures xii List of tables xxi 1 Introduction1 1.1 Low- to intermediate-mass stellar evolution . .2 1.1.1 The life cycle of a star . .2 1.1.2 Mixing episodes . .5 1.2 Dust . .6 1.2.1 Carbon-rich dust . .7 1.2.2 Oxygen-rich dust . 12 1.2.3 Dual-dust chemistry . 14 1.3 Planetary nebulae . 14 1.3.1 Morphology . 15 1.3.2 Shocks . 17 1.3.3 Photodissociation regions . 19 1.4 Current status . 22 1.4.1 Influence of metallicity on dust composition . 22 1.4.2 Diversity of large organic molecules . 24 1.5 Thesis overview . 26 2 Methods of data reduction and analysis 27 2.1 Spectroscopy . 27 viii Table of contents 2.1.1 Atomic spectroscopy . 28 2.1.2 Molecular spectroscopy . 33 2.2 Infrared emission lines . 36 2.2.1 Metallicity and abundance . 36 2.2.2 Probing physical conditions . 38 2.3 Infrared airborne and space telescopes . 40 2.3.1 History . 40 2.3.2 The Spitzer Space Telescope ..................... 42 2.3.3 Stratospheric Observatory for Infrared Astronomy (SOFIA) . 43 2.4 Data processing . 47 2.4.1 Spectroscopic Modelling Analysis and Reduction Tool (SMART) . 47 2.4.2 FLUXER . 50 2.5 Summary . 52 3 Neon, sulphur and argon abundances of planetary nebulae in the sub-solar metallicity Galactic anti-centre 54 3.1 Introduction . 54 3.2 Data . 57 3.2.1 Observations . 57 3.2.2 Data reduction and extraction . 59 3.3 Analysis . 61 3.3.1 Ionic abundances . 61 3.3.2 Line flux measurements . 61 3.3.3 Extinction corrections . 62 3.3.4 Hb intensity . 64 3.3.5 Electron densities and temperatures . 66 3.3.6 Elemental abundances . 69 3.3.7 Galactocentric distances . 84 3.4 Discussion . 85 Table of contents ix 3.4.1 Comparison of abundances with literature . 85 3.4.2 The abundance gradient . 87 3.4.3 a-process elements . 90 3.5 Summary . 93 4 Dust composition of PNe in the Galactic anti-centre 95 4.1 Introduction . 95 4.2 Sample overview . 97 4.3 Polycyclic aromatic hydrocarbons (PAHs) . 99 4.3.1 Profiles . 99 4.3.2 Ionisation fractions . 103 4.4 PAH decomposition . 104 4.4.1 Gaussian curve fitting . 105 4.4.2 Components . 105 4.4.3 Decomposition analysis . 107 4.5 Silicon carbide . 113 4.6 Fullerenes . 115 4.7 The 30 mm feature . 117 4.8 Silicates . 119 4.9 Featureless spectra . 120 4.10 The link between dust composition and metallicity . 121 4.11 Conclusions . 123 5 Abundances and dust compositions of planetary nebulae from the Galactic halo126 5.1 Introduction . 126 5.2 Data . 128 5.2.1 Sample . 128 5.2.2 Data handling and reduction . 133 5.3 Abundances . 133 x Table of contents 5.4 Dust . 138 5.5 Discussion . 142 5.5.1 Comparisons with other Galactic PNe . 142 5.5.2 The Sagittarius stream . 144 5.5.3 Shocks and dust destruction . 146 5.6 Summary . 148 6 Investigating the astrophysical environments of fullerene emission around PNe 150 6.1 Introduction . 150 6.2 Data acquisition and handling . 153 6.3 Analysis . 153 6.3.1 Intensity maps . 156 6.3.2 Line intensity offsets . 159 6.3.3 Line velocities . 160 6.4 PDR modelling . 164 6.4.1 Model description . 164 6.4.2 Inputs . 165 6.4.3 Analysis of model outputs . 166 6.5 Discussion and conclusions . 169 7 Conclusions and future work 171 7.1 Summary of findings . ..
Load more

Recommended publications
  • I N S I D E T H I S I S S
    Publications from February/février 1998 Volume/volume 92 Number/numero 1 [669] The Royal Astronomical Society of Canada The Beginner’s Observing Guide This guide is for anyone with little or no experience in observing the night sky. Large, easy to read star maps are provided to acquaint the reader with the constellations and bright stars. Basic information on observing the moon, planets and eclipses through the year 2000 is provided. There The Journal of the Royal Astronomical Society of Canada Le Journal de la Société royale d’astronomie du Canada is also a special section to help Scouts, Cubs, Guides and Brownies achieve their respective astronomy badges. Written by Leo Enright (160 pages of information in a soft-cover book with a spiral binding which allows the book to lie flat). Price: $12 (includes taxes, postage and handling) Looking Up: A History of the Royal Astronomical Society of Canada Published to commemorate the 125th anniversary of the first meeting of the Toronto Astronomical Club, “Looking Up — A History of the RASC” is an excellent overall history of Canada’s national astronomy organization. The book was written by R. Peter Broughton, a Past President and expert on the history of astronomy in Canada. Histories on each of the centres across the country are included as well as dozens of biographical sketches of the many people who have volunteered their time and skills to the Society. (hard cover with cloth binding, 300 pages with 150 b&w illustrations) Price: $43 (includes taxes, postage and handling) Observers Calendar — 1998 This calendar was created by members of the RASC.
    [Show full text]
  • Planetary Nebulae
    Planetary Nebulae A planetary nebula is a kind of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from old red giant stars late in their lives. The term "planetary nebula" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. The mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energizes the shell of nebulous gas around the central star, appearing as a bright colored planetary nebula at several discrete visible wavelengths. Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances. In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies.
    [Show full text]
  • Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
    Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties.
    [Show full text]
  • Observatories
    NATIONAL OPTICAL ASTRONOMY OBSERVATORIES NATIONAL OPTICAL ASTRONOMY OBSERVATORIES FY 1997 PROVISIONAL PROGRAM PLAN September 19,1996 TABLE OF CONTENTS I. INTRODUCTION AND OVERVIEW 1 II. THE DEVELOPMENT PROGRAM: MILESTONES PAST AND FUTURE 3 IE. NIGHTTIME PROGRAM 6 A. Major Projects 6 1. SOAR ".""".6 2. WIYN 8 B. Joint Nighttime Instrumentation Program 9 1. Overview 9 2. Description of Individual Major Projects 10 3. Detectors 13 4. NOAO Explorations of Technology (NExT) Program 14 C. USGP 15 1. Overview 15 2. US Gemini Instrument Program 16 D. Telescope Operations and User Support 17 1. Changes in User Services 17 2. Telescope Upgrades 18 a. CTIO 18 b. KPNO 21 3. Instrumentation Improvements 24 a. CTIO 24 b. KPNO 26 4. Smaller Telescopes 29 IV. NATIONAL SOLAR OBSERVATORY 29 A. Major Projects 29 1. Global Oscillation Network Group (GONG) 30 2. RISE/PSPT Program 33 3. SOLIS 34 4. Study of CLEAR 35 B. Instrumentation 36 1. General 36 2. Sacramento Peak 36 3. NSO/KittPeak 38 a. Infrared Program 38 b. Telescope Improvement 40 C. Telescope Operations and User Support 41 1. Sacramento Peak 41 2. NSO/KittPeak 42 V. THE SCIENTIFIC STAFF 42 VI. EDUCATIONAL OUTREACH 45 A. Educational Program 45 1. Direct Classroom Involvement 46 2. Development of Instructional Materials 46 3. WWW Distribution of Science Resources 47 4. Outreach Advisory Board 47 5. Undergraduate Education 47 6. Graduate Education 47 7. Educational Partnership Programs 47 B. Public Information 48 1. Press Releases and Other Interactions With the Media 48 2. Images 48 3 Visitor Center 48 C.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Ioptron CEM40 Center-Balanced Equatorial Mount
    iOptron®CEM40 Center-Balanced Equatorial Mount Instruction Manual Product CEM40 (#7400A series) and CEM40EC (#7400ECA series, as shown) Please read the included CEM40 Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper operation will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while using a telescope. 2 Table of Contents Table of Contents ........................................................................................................................................ 3 1. CEM40 Introduction ............................................................................................................................... 5 2. CEM40 Overview ................................................................................................................................... 6 2.1. Parts List .........................................................................................................................................
    [Show full text]
  • Anousheh Ansari
    : Fort Worth Astronomical Society (Est. 1949) August 2010 Astronomical League Member At the August Meeting: Special Guest Anousheh Ansari Club Calendar – 2 – 3 Skyportunities Star Party & Club Reports – 5 House Calls by Ophiuchus – 6 Hubble’s Amazing Rescue – 8 Your Most Important Optics -- 9 Stargazers’ Diary – 11 1 Milky Way Over Colorado by Jim Murray August 2010 Sunday Monday Tuesday Wednesday Thursday Friday Saturday 1 2 3 4 5 6 7 Third Qtr Moon Challenge binary star for August: Make use of the New Viking 1 Orbiter 11:59 pm Moon Weekend for Alvan Clark 11 (ADS 11324) (Serpens Cauda) ceases operation better viewing at the 30 years ago Notable carbon star for August: Dark Sky Site Mars : Saturn O V Aquilae 1.9 Conjunction Mercury at greatest Challenge deep-sky object for August: eastern elongation Venus, Mars and Abell 53 (Aquila) Saturn all within a this evening binocular field of First in-flight New Moon view for the first 12 New Moon shuttle repair Neal Armstrong Weekend Weekend days of August. 15 years ago born 80 years ago 8 9 10 11 12 13 14 New Moon Moon at Perigee Double shadow (224,386 miles) transit on Jupiter 3RF Star Party 10:08 pm 1 pm 5:12am High in SSW Museum Star (A.T. @ 5:21 am) Party Venus : Saturn O . 3 of separation Perseid Meteor Watch Party @ 3RF New Moon Magellan enters Fairly consistent show Weekend orbit around Venus of about 60 per hour 20 years ago 15 16 17 18 19 20 21 Algol at Minima 2:45 am - In NE First Qtr Moon Total Solar 1:14 pm Eclipse in 7 years Nearest arc of totality takes in FWAS Grand Island NE St Joseph MO Meeting With Neptune @ Columbia MO Venus at greatest Opposition Anousheh Algol at Minima eastern elongation N of Nashville TN 11:34pm Low In NE 5 am N of Charleston SC Ansari this evening 22 23 24 25 26 27 28 Full Moon Moon at Apogee 2:05 pm (252,518.miles) GATE CODES Smallest of 2010 1 am to the (within 11 hrs of apogee) DARK SKY SITE will be changed st September 1 BE SURE YOU ARE CURRENT WITH DUES to Astroboy’s Day Job Venus : Mars receive new codes O 2 Conjunction 29 31 30 Anousheh Ansari’s Mission Patch at right.
    [Show full text]
  • The Perek-Kohoutek Catalogue of Planetary Nebulae
    Perek- Right Catalog Other Declination Kohoutek ascension The Perek-Kohoutek number designation (2000.0) number (2000.0) Catalogue of 1 119+06.1 A 1 0h12.9m 69°11' 2 120+09.1 NGC 40 0h13.0m 72°32' Planetary Nebulae 3 118–08.1 Vy 1–1 0h18.7m 53°53' 4 119+00.1 BV 1 0h19.9m 62°59' Data is from Catalogue of Galactic Planetary 5 119–06.1 Hu 1–1 0h28.3m 55°58' Nebulae, updated version 2000, by L. Kohoutek, 6 120–05.1 Sh 2–176 0h31.8m 57°23' Hamburg-Berfedorf, 2001. 7 108–76.1 BOBN 1 0h37.2m –13°43' 8 121+03.1 We 1–1 0h38.9m 66°23' 9 121+00.1 BV 2 0h40.3m 62°51' 10 122–04.1 A 2 0h45.6m 57°57' 11 118–74.1 NGC 246 0h47.0m –11°53' 12 125–47.1 PHL 932 0h59.9m 15°44' 13 124–07.1 WeSb 1 1h00.9m 55°04' 14 124+02.1 KLSS 2–7 1h02.4m 65°46' 15 124+10.1 EL 0103+73 1h07.1m 73°33' 16 126+03.1 K 3–90 1h24.9m 65°39' 17 128–04.1 S 22 1h30.5m 58°24' 18 130–11.1 M 1–1 1h37.3m 50°28' 19 129–05.1 KLSS 2–8 1h40.1m 56°35' 20 130–10.1 NGC 650–1 1h42.4m 51°34' 21 129–02.1 We 2–5 1h42.6m 60°10' 22 131–05.1 BV 3 1h53.0m 56°25' 23 130+01.1 IC 1747 1h57.6m 63°20' 24 129+04.1 K 3–91 1h58.6m 66°34' 25 148–48.1 GR 0155+10 1h58.0m 10°57' 26 133–08.1 M 1–2 1h58.8m 52°54' 27 130+03.1 K 3–92 2h03.7m 64°57' 28 131+02.1 A 3 2h12.1m 64°09' 29 132+04.1 K 3–93 2h26.5m 65°47' 30 144–15.1 A 4 2h45.4m 42°34' 31 141–07.1 A 5 2h52.3m 50°36' 32 136+04.1 A 6 2h58.7m 64°30' 33 255–59.1 Lo 1 2h57.0m –44°10' 34 136+05.1 HEFE 1 3h03.8m 64°54' 35 138+02.1 IC 289 3h10.3m 61°19' 36 138+04.1 HtDe 2 3h11.0m 62°48' 37 147–09.1 HtWe 3 3h16.6m 46°54' 38 149–09.1 HtDe 3 3h27.2m 45°24' 39 220–53.1 NGC
    [Show full text]
  • MUSE Commissioning
    Telescopes and Instrumentation MUSE Commissioning Roland Bacon1 The Multi Unit Spectroscopic Explorer reach MUSE from the star’s surface, but Joel Vernet2 (MUSE) is now in Paranal and was it is also the duration of the project, which Elena Borisiva3 installed on the VLT’s Unit Telescope 4 started in 2001 when the consortium Nicolas Bouché4 in January 2014. MUSE enters science answered the ESO call for ideas for sec- Jarle Brinchmann5 operations in October. A short summary ond generation VLT instrumentation. Marcella Carollo3 of the commissioning activities and Sci- David Carton5 ence Verification are presented. Some Joseph Caruana7 examples of the first results achieved Commissioning Susana Cerda2 during the two commissioning runs are Thierry Contini4 highlighted. After some technical half nights to finalise Marijn Franx5 the instrument’s alignment on the tele- Marianne Girard4 scope, the first commissioning period Adrien Guerou4,2 The Multi Unit Spectroscopic Explorer started. During 15 nights, from 7 to Nicolas Haddad2 (MUSE) is a second generation Very 21 February 2014, functional tests and George Hau2 Large Telescope (VLT) instrument for performance assessments were per- Christian Herenz7 integral field spectroscopy in the optical formed. From the first minute, MUSE Juan Carlos Herrera2 range (460–940 nm). It has two modes worked as expected and the whole run Bernd Husemann2 with different fields of view: 1 by 1 arc- went very smoothly, with no down time. Tim-Oliver Husser6 minutes at a spatial sampling of 0.2 arc- Aurélien Jarno1 seconds; and, when coupled to the The performance, as anticipated by the Sebastian Kamann6 Adaptive Optics Facility, a laser tomogra- laboratory measurements, is excellent Davor Krajnovic7 phy adaptive optics assisted mode with a and in general, much better than the Simon Lilly3 field of 7.5 by 7.5 arcseconds (with original specifications.
    [Show full text]
  • Emission Lines in Planetary Nebulae
    The Astrophysical Journal, 840:80 (8pp), 2017 May 10 https://doi.org/10.3847/1538-4357/aa6c28 © 2017. The American Astronomical Society. All rights reserved. ∗ Identification of Near-infrared [Se III] and [Kr VI] Emission Lines in Planetary Nebulae N. C. Sterling1, S. Madonna2,3, K. Butler4, J. García-Rojas2,3, A. L. Mashburn1, C. Morisset5, V. Luridiana2,3, and I. U. Roederer6,7 1 Department of Physics, University of West Georgia, 1601 Maple Street, Carrollton, GA 30118, USA; [email protected], [email protected] 2 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; [email protected], [email protected], [email protected] 3 Universidad de La Laguna, Dpto. Astrofísica, E-38206 La Laguna, Tenerife, Spain 4 Institut für Astronomie und Astrophysik, Scheinerstr. 1, D-81679 München, Germany; [email protected] 5 Instituto de Astronomía, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20164, 04510, Mexico; [email protected] 6 Department of Astronomy, University of Michigan, 1085 South University Avenue, Ann Arbor, MI 48109, USA; [email protected] 7 Joint Institute for Nuclear Astrophysics and Center for the Evolution of the Elements (JINA-CEE), USA Received 2017 January 19; accepted 2017 April 4; published 2017 May 9 Abstract We identify [Se III]1.0994 μm in the planetary nebula (PN) NGC5315 and [Kr VI]1.2330 μm in three PNe from spectra obtained with the Folded-Port InfraRed Echellette (FIRE) spectrometer on the 6.5 m Baade Telescope. Se and Kr are the two most widely detected neutron-capture elements in astrophysical nebulae, and can be enriched by s-process nucleosynthesis in PN progenitor stars.
    [Show full text]
  • Lecture 3 Evolution of X-Ray Binaries.Pptx
    Evolution of X-ray binaries Rudy Wijnands Anton Pannekoek Institute for Astronomy University of Amsterdam 30 May 2017 Bologna, Italy Evolution of a binary • Many stars are in binary systems • Stellar evolution can be significantly altered due to mass loss and mass transfer • Binary orbit can expand or shrink considerably during the evolution – Conservative or non-conservative mass transfer Conservative mass transfer • Total mass is conserved – Mtotal = m1 + m2 = constant • Total angular moment is conserved – Consider only Jorbit as Jspin<< Jorbit • Then one can proof that • If more massive star transfers mass – dm1/dt < 0 and m1 > m2 – Then P and a decreases until masses become equal for minimum P and a à runaway Roche-lobe mass transfer! – If mass transfer continues, then orbit expands again Non-conservative mass transfer • General case • What happens if either mass or angular moment are not conserved? – Mass is not conserved when • Mass transfer and loss through stellar wind • Very rapid Roche-lobe overflow – Receiving star cannot accrete all mass and mass is loss through L2 point – Angular moment is not conserved when • Magnetic braking through stellar wind – Wind is forced to co-rotate at large distance with the rotation of the star • Gravitational radiation for close compact binaries • E.g., wind from primary escapes system § dm1/dt < 0, and dm2/dt = 0, • General case for mass transfer in circular orbits § With KJ the change in angular moment § Conservative mass transfer: § Stellar wind loss case: Evolution of a binary • Many stars
    [Show full text]
  • Near Infrared Photometry of IRAS Sources with Colours Like Planetary Nebulae
    University of Groningen Near infrared photometry of IRAS sources with colours like planetary nebulae. III. Garcia-Lario, P.; Manchado, A.; Pych, W.; Pottasch, S. R. Published in: Astronomy & astrophysics supplement series DOI: 10.1051/aas:1997277 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 1997 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Garcia-Lario, P., Manchado, A., Pych, W., & Pottasch, S. R. (1997). Near infrared photometry of IRAS sources with colours like planetary nebulae. III. Astronomy & astrophysics supplement series, 126(3), 479- 502. https://doi.org/10.1051/aas:1997277 Copyright Other than for strictly personal use, 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), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal.
    [Show full text]