INDEX OF SUBJECTS 6, 14, 23, 50, 95, 191 4, 191, 234

Size: px
Start display at page:

Download "INDEX OF SUBJECTS 6, 14, 23, 50, 95, 191 4, 191, 234"

Transcription

1 INDEX OF SUBJECTS Abundances, elemental Abundances, ionic AGB stars (see Stars, AGB) Age, nebulae Asymptotic Giant Branch (AGB) Be stars (see Stars, Be) Bipolar structure, nebulae Carbon stars Carbon stars, IR photometry Catalogue, Galactic Planetary Nebulae Catalogue, IRAS LRS spectra Catalogue, IRAS Point Source (PSC) Catalogue, IRAS Small Structure (SSC) Catalogue, Strasbourg-ESO Catalogue, symbiotic stars (Allen,1984) Central star, H-R diagram Central star, Wolf-Rayet Central star, binaries Central star, evolution Central star, light curve Central star, luminosity Central star, luminosity function Central star, absolute magnitude Central star, magnitude Central star, mass Central star, radius Central star, rotation Central star, spectra Central star, superwind Central star, temperature Central star, wind Chemical evolution, galactic Circumstellar disk Circumstellar Circumstellar Circumstellar Cirrus Core mass Crossing time dust nebulae shell 6, 14, 23, 50, 95, 191 4, 191, 234, 121, 131, , 69, 121, , 107, 130, , , 39, 46, 221, , , 79, 84, 89, 131 7, 23, 91 87, 126,, 171, ,, 113, 131, 138, 143, , 79, 118, 131, , 143, , 272 3, , 74 5, 80, 83, 135, 191, , 56, 102, , 71, , , , 67, 114, Distance scales Distance to nebulae Dust to gas ratio , , 147, 195 6, 10, , 250, 276

2 2R2 INDEX OF SUBJECTS Dust, IR luminosity Dust, evolution Dust, heating Dust, mass Dust, optical depth Dust, size Dust, temperature Dust, temperature distribution Dust/gas envelope stars (DES) Emission line intensities, infrared Emission line intensities, optical Energy balance method Envelope mass Escape velocity Excitation, nebulae Expanding envelope Expansion velocity, nebulae Expansion velocity, stellar envelope Extinction, Balmer decrement Filling factor Galactic centre planetary nebulae Grains, cross-section Grains, graphite Grains, iron Grains, silicate Grains, silicon carbide Grains, size distribution H II regions H II regions, compact H-R diagram Helium flash Helium-burning phase Horizontal branch stars Hydrogen envelope mass Hydrogen-burning phase Infrared emission Infrared emission, dust Infrared emission, line Infrared emission, spatial extent Infrared energy distribution Infrared excess Infrared photometry Infrared photometry, Be stars Infrared photometry, Mira stars Infrared photometry, OH/IR stars Infrared spectroscopy , 241 6, 184, , 250 2, 62, 193, , 243, , 188, 214, , 178, 190 3, , , 56, 63, 86, 123, 146, , 126 9, 49, , 242, 246, , 276 7, 48, 186, 243, 258 7, , 250 7, 28, 92, 99, , 30 83, 131, , , , 113, 124, , 46, 239, ,, 190, 197, 235, 276 5, 234 2, 229 4, , 221, , 76, 1, 204, 255

3 INDEX OF SUBJECTS 2R3 Infrared two-colour diagram Interacting stellar winds model International Ultraviolet Explorer (IUE) Interplanetary dust Interstellar reddening Interstellar medium I R A S - Additional Observations (AO) I R A S - Chopped Photo Channel (CPC) I R A S - LRS spectra I R A S - Survey fluxes Infrared Space Obsevatory (ISO) ISO - Camera ISO - Long WI Spectrometer ISO - Photopolarimeter ISO - Short WI Spectrometer Main sequence mass, initial Maps, far infrared Maser emission, H20 Maser emission, OH Maser emission, SiO Mass loss Mass loss rate Mass loss, AGB stars Mass loss, Miras Mass loss, OH masers Mass loss, OH/IR stars Mass loss, reg giants Massive stars Metal abundances Mira stars (see Stars, Miras) Misclassified planetary nebulae Model atmosphere Models, nebula Molecular lines, CO Molecular lines, H2 Nebulae, UV spectrum Nebulae, abundances Nebulae, evolution Nebulae, evolutionary age Nebulae, expansion age Nebulae, far-ir luminosity Nebulae, halos Nebulae, ionization structure Nebulae, mass Nebulae, optical images Nebulae, optical spectrum Nebulae, optically thick Nebulae, optically thin 12, 71, 77, 227, 228, , 101, , 11, 46, 187, 234, , 189, 199, 233, , , , 78, 57, 61, 58, 62, 55, 67, , 122, , , 113, , 23, 56, 58, 71, 122, , 115, 122, , , , 25, , 242 5, 57, 271, , , 191 2, 61, 121, 125, 132, 121 3, , 153, ,, , 154, 159, , 104, 153, , , ,

4 2K4 INDEX OF SUBJECTS Nebulae, radio continuum Nebulae, spatial distribution Nebulae, spectroscopic survey OH/IR stars (see Stars, OH/IR) OH/IR stars, non-variable OH/IR stars, radio emission OH/IR stars, space distribution Oxigen-rich planetaries P-Cygni profiles Polycyclic aromatic hydrocarbons (PAH) Progenitors of planetary nebulae Progenitors of planetary nebulae, mass Protoplanetary nebulae Radial velocity, nebulae Radio continuum emission Radio maps, VLA Radius of planetary nebulae Shock waves Shocked gas Stars, AGB Stars, Be Stars, Miras Stars, OH/IR Stars, post-agb Stars, red giant Stars, sub-dwarfs Stellar envelope, mass Stellar wind Superwind Symbiotic stars Symbiotic stars, IR excess Symbiotic stars, IR photometry Symbiotic stars, UV spectra Symbiotic stars, X-ray Symbiotic stars, catalogue Symbiotic stars, optical spectrum Symbiotic stars, radio Temperature, Energy-Balance method Temperature, Zanstra method Temperature, stellar continuum Thermal pulse Transition objects Very Low Excitation (VLE) objects White dwarfs Zanstra temperature 4, 272 8, , 67, 75, , 48, 193, , 91 17, 91, , 74, , 10, , 133, , , , 28, 70, 167 2, 8, 57, , 141, 143, , 139, , 122, , 56, 93, 102, 56, 60, 71, 116, 28, 130, , D, , 80, 201 3, , 121, 1 55, 62, , 122, 30 3D, 73, 113, 131, , 126, , 273

5 INDEX OF ASTRONOMICAL OBJECTS A) Planetary Nebulae PK Name HI SwStl NGC M MI Hb NGC VV NGC NGC A M NGC NGC Sa NGC NGC VVI M IC NGC M M K NGC NGC NGC NGC Ap NGC NGC NGC Cn K NGC , 9, 82, 276, , 46 82, 200, , 201, 8,, 95 5, 62, 88, , 62, , 48, 200, 201, , 199,, 276 2

6 286 INDEX OF ASTRONOMICAL OBJECTS PK Name Pag Vy NGe Hu A A Ie NGe NGe NGe NGe BD NGe NGe NGe NGe K Hul Ml NGe NGe Me NGe NGe Hb NGe Vy NGe Ie Ie NGe 650/ NGe Ie Ie NGe Ie NGe 2371/ J NGe A Ie , 46, 49, 63, 64, 67, , 52, 62 5, 41, 95, 200, , , 8, 49, , 20, 23,, 200, 201, 276 5, 47, 62, 81, 83,, , 200, 201, 41 20, 47, 105,, 199,, , 47, 83,, 200, 201, 8, 52, 8, 102, 162, 199, ,, 40, , 199, , 43 20, 199, 201

7 INDEX OF ASTRONOMICAL OBJECTS 287 PK Name Pag Ml NGC IC NGC M IC Aro Pb Ml NGC Ml M NGC Ml Ml Ml M NGC Sa NGC NGC Pb NGC He He Wra NGC He He Pb Wra Wra Pb NGC He ES SV Car IC NGC ES0 15, 41, 62, 95,, 178, 183, 275 8, 20, 48, 62,, 200, 201,, , 83, 49, 82, 83,, 95, 158, 199, , 83,, 20, 199, 201, , 83,, , 82, 82, 83,

8 288 INDEX OF ASTRONOMICAL OBJECTS PK Name Pag He Ph NGC He NGC He He Aro IC He He Wra He NGC Wra He He He He He He He He Wra Wra Pe He He He He He Wra He NGC He He He Cn Mz Wra , 83,, 154,, 242, , , 83,, 95,, 87, 8, 8, 48,

9 INDEX OF ASTRONOMICAL OBJECTS 2R9 PK Name Pag He He He He He Pel He He LT NGC H IC M NGC H ES Hl M M Ml NGC M Hl M , 62, 82, 87, 95, , B) Symbiotic Stars a Sco AG Dra AG Peg AR Pav CH Cyg CI Cyg EG And HM Sge MWC 349 PK , , , 168 R Aqr RR Tel V 1016 Cyg V 1329 Cyg 167, , , 168

10 290 INDEX OF ASTRONOMICAL OBJECTS c) Proto-Planetaries and OH/IR Stars AFGL 6815 CRL 618 CRL 2688 IRAS IRC IRC OH OH OH OH OH OHI , 63, , D) Other Objects Feige 66 Feige 110 lid LMC M 17 M 82 M 83 NGC 1566 NGC 2023 NGC 2359 NGC 6822 NGC 6888 Orion SB 939 SMC V 6 Man

The Physics and Dynamics of Planetary Nebulae

The Physics and Dynamics of Planetary Nebulae Grigor A. Gurzadyan The Physics and Dynamics of Planetary Nebulae With 125 Figures, 14 Plates and 93 Tables Springer Contents 1. Global Concepts 1 1.1 The Shapes of Planetary Nebulae 1 1.2 The Structure

More information

The Physics of the Interstellar Medium

The Physics of the Interstellar Medium The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,

More information

Midterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10

Midterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10 Lecture 13 : The Interstellar Medium and Cosmic Recycling Midterm Results A2020 Prof. Tom Megeath The Milky Way in the Infrared View from the Earth: Edge On Infrared light penetrates the clouds and shows

More information

Post-AGB stars and Planetary Nebulae. Stellar evolution Expansion and evolution Molecules and dust 3He SKA

Post-AGB stars and Planetary Nebulae. Stellar evolution Expansion and evolution Molecules and dust 3He SKA Post-AGB stars and Planetary Nebulae Stellar evolution Expansion and evolution Molecules and dust 3He SKA GAIA HR diagram McDonald et al. 2017 Post-AGB evolution Molecular shell detaches and expands Heating

More information

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,

More information

The Deaths of Stars 1

The Deaths of Stars 1 The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,

More information

Lifespan on the main sequence. Lecture 9: Post-main sequence evolution of stars. Evolution on the main sequence. Evolution after the main sequence

Lifespan on the main sequence. Lecture 9: Post-main sequence evolution of stars. Evolution on the main sequence. Evolution after the main sequence Lecture 9: Post-main sequence evolution of stars Lifetime on the main sequence Shell burning and the red giant phase Helium burning - the horizontal branch and the asymptotic giant branch The death of

More information

Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two

Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two Stellar Evolution: The Deaths of Stars Chapter Twenty-Two Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come

More information

arxiv:astro-ph/ v1 23 Oct 2002

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

More information

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages The Deaths of Stars Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,

More information

The Ṁass- loss of Red Supergiants

The Ṁass- loss of Red Supergiants The Ṁass- loss of Red Supergiants Dr. Donald F. Figer Director, Center for Detectors Speaker: Yuanhao (Harry) Zhang RIT 9/12/13 1 9/12/13 2 Outline IntroducJon MoJvaJon Objects Method Need for SOFIA/FORCAST

More information

A NEW CATALOG OF AGB STARS BASED ON INFRARED TWO-COLOR DIAGRAMS

A NEW CATALOG OF AGB STARS BASED ON INFRARED TWO-COLOR DIAGRAMS Journal of the Korean Astronomical Society https://doi.org/.5/jkas.7.5.. 5: 8, 7 August pissn: 5-6 eissn: 88-89X c 7. The Korean Astronomical Society. All rights reserved. http://jkas.kas.org A NEW CATALOG

More information

Astr 2310 Thurs. March 23, 2017 Today s Topics

Astr 2310 Thurs. March 23, 2017 Today s Topics Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar

More information

5) What spectral type of star that is still around formed longest ago? 5) A) F B) A C) M D) K E) O

5) What spectral type of star that is still around formed longest ago? 5) A) F B) A C) M D) K E) O HW2 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) The polarization of light passing though the dust grains shows that: 1) A) the dust grains

More information

Mass loss from stars

Mass loss from stars Mass loss from stars Can significantly affect a star s evolution, since the mass is such a critical parameter (e.g., L ~ M 4 ) Material ejected into interstellar medium (ISM) may be nuclear-processed:

More information

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand

More information

Paul Broberg Ast 4001 Dec. 10, 2007

Paul Broberg Ast 4001 Dec. 10, 2007 Paul Broberg Ast 4001 Dec. 10, 2007 What are W-R stars? How do we characterize them? What is the life of these stars like? Early stages Evolution Death What can we learn from them? Spectra Dust 1867: Charles

More information

Symbiotic Stars: an ISO overview. R. Angeloni 1,2, M. Contini 2,1, S. Ciroi 1, P. Rafanelli 1 AJ, , 205. Rodolfo Angeloni May SNA

Symbiotic Stars: an ISO overview. R. Angeloni 1,2, M. Contini 2,1, S. Ciroi 1, P. Rafanelli 1 AJ, , 205. Rodolfo Angeloni May SNA Silicate Dust in D-type Symbiotic Stars: an ISO overview R. Angeloni 1,2, M. Contini 2,1, S. Ciroi 1, P. Rafanelli 1 AJ, 2007-134, 205 1 Dept. of Astronomy, University of Padova, Italy 2 School of Physics

More information

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. 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

More information

From AGB Stars to Planetary Nebula. Cats Eye Planetary Nebula: HST

From AGB Stars to Planetary Nebula. Cats Eye Planetary Nebula: HST From AGB Stars to Planetary Nebula Cats Eye Planetary Nebula: HST AGB Stars NOAO H -> He in convective region Dredge Up Prialnik AGB stars pulsing Schwarzchild & Harm (1967) The 9th Cycle Schwarzchild

More information

Chemical Enrichment of the ISM by Stellar Ejecta

Chemical Enrichment of the ISM by Stellar Ejecta Chemical Enrichment of the ISM by Stellar Ejecta Sun Kwok The University of Hong Kong IAU GA Beijing, Special Session 12, August 31, 2012 Molecular synthesis in the late stages of stellar evolution It

More information

Visiting Assistant Professor at Space Science Institute, Macau University of Science and Technology, December 2015 October 2016

Visiting Assistant Professor at Space Science Institute, Macau University of Science and Technology, December 2015 October 2016 Academic Staff Resume Name: Chih-Hao Hsia Title: Research Fellow Space Science Institute Office:A 505 Tel.:+853-8897 3350 E-mail:chhsia@must.edu.mo Photo Academic Qualification: Ph.D. in Astronomy, Graduate

More information

Interstellar Medium and Star Birth

Interstellar Medium and Star Birth Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread

More information

Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical

Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Trigonometry p. 9 The Earth p. 12 The Celestial Sphere p. 14 The

More information

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)?

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)? How Long do Stars Live (as Main Sequence Stars)? A star on Main Sequence has fusion of H to He in its core. How fast depends on mass of H available and rate of fusion. Mass of H in core depends on mass

More information

Near infrared photometry of IRAS sources with colours like planetary nebulae. III.,

Near infrared photometry of IRAS sources with colours like planetary nebulae. III., ASTRONOMY & ASTROPHYSICS DECEMBER II 1997, PAGE 479 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 126, 479-502 (1997) Near infrared photometry of IRAS sources with colours like planetary nebulae. III.,

More information

Astrophysics of Gaseous Nebulae and Active Galactic Nuclei

Astrophysics of Gaseous Nebulae and Active Galactic Nuclei SECOND EDITION Astrophysics of Gaseous Nebulae and Active Galactic Nuclei Donald E. Osterbrock Lick Observatory, University of California, Santa Cruz Gary J. Ferland Department of Physics and Astronomy,

More information

Universe Now. 9. Interstellar matter and star clusters

Universe Now. 9. Interstellar matter and star clusters Universe Now 9. Interstellar matter and star clusters About interstellar matter Interstellar space is not completely empty: gas (atoms + molecules) and small dust particles. Over 10% of the mass of the

More information

Stellar Populations: Resolved vs. unresolved

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

More information

Physics and Chemistry of the Interstellar Medium

Physics and Chemistry of the Interstellar Medium Physics and Chemistry of the Interstellar Medium Sun Kwok The University of Hong Kong UNIVERSITY SCIENCE BOOKS Sausalito, California * Preface xi The Interstellar Medium.1.1 States of Matter in the ISM

More information

Stars + Galaxies: Back of the Envelope Properties. David Spergel

Stars + Galaxies: Back of the Envelope Properties. David Spergel Stars + Galaxies: Back of the Envelope Properties David Spergel Free-fall time (1) r = GM r 2 (2) r t = GM 2 r 2 (3) t free fall r3 GM 1 Gρ Free-fall time for neutron star is milliseconds (characteristic

More information

Stellar Evolution Stars spend most of their lives on the main sequence. Evidence: 90% of observable stars are main-sequence stars.

Stellar Evolution Stars spend most of their lives on the main sequence. Evidence: 90% of observable stars are main-sequence stars. Stellar Evolution Stars spend most of their lives on the main sequence. Evidence: 90% of observable stars are main-sequence stars. Stellar evolution during the main-sequence life-time, and during the post-main-sequence

More information

I. Introduction. First suspicion of existence of continuous stellar winds: Optical spectrum of Wolf-Rayet stars: widths of lines

I. Introduction. First suspicion of existence of continuous stellar winds: Optical spectrum of Wolf-Rayet stars: widths of lines 8. Stellar Winds History of Stellar Winds Spectroscopic Signatures of Stellar Winds Stellar Winds in Astronomy: Extragalactic supergiants, Mass loss, Galaxy evolution 1 I. Introduction First suspicion

More information

Evolution of Intermediate-Mass Stars

Evolution of Intermediate-Mass Stars Evolution of Intermediate-Mass Stars General properties: mass range: 2.5 < M/M < 8 early evolution differs from M/M < 1.3 stars; for 1.3 < M/M < 2.5 properties of both mass ranges MS: convective core and

More information

Guiding Questions. Stellar Evolution. Stars Evolve. Interstellar Medium and Nebulae

Guiding Questions. Stellar Evolution. Stars Evolve. Interstellar Medium and Nebulae Guiding Questions Stellar Evolution 1. Why do astronomers think that stars evolve? 2. What kind of matter exists in the spaces between the stars? 3. What steps are involved in forming a star like the Sun?

More information

Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused

More information

Energy. mosquito lands on your arm = 1 erg. Firecracker = 5 x 10 9 ergs. 1 stick of dynamite = 2 x ergs. 1 ton of TNT = 4 x ergs

Energy. mosquito lands on your arm = 1 erg. Firecracker = 5 x 10 9 ergs. 1 stick of dynamite = 2 x ergs. 1 ton of TNT = 4 x ergs Energy mosquito lands on your arm = 1 erg Firecracker = 5 x 10 9 ergs 1 stick of dynamite = 2 x 10 13 ergs 1 ton of TNT = 4 x 10 16 ergs 1 atomic bomb = 1 x 10 21 ergs Magnitude 8 earthquake = 1 x 10 26

More information

Carbon stars and dust production as a function of metallicity

Carbon stars and dust production as a function of metallicity Carbon stars and dust production as a function of metallicity G.C. Sloan and many others SOFIA Tele-Talk 2-26-2014 NGC 1978 in the LMC observed by the HST 1 Conclusions The amount of dust produced by carbon

More information

Astrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC HST

Astrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC HST Astrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC 7023 - HST Julien Montillaud 8th February 2013 Outline I. From Unidentified to Aromatic Infrared Bands (7 p.) I.1 Historical background I.2 Observational

More information

Einführung in die Astronomie II

Einführung in die Astronomie II Einführung in die Astronomie II Teil 10 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 15. Juni 2017 1 / 47 Overview part 10 Death of stars AGB stars PNe SNe

More information

Citation for published version (APA): Bernard Salas, J. (2003). Physics and chemistry of gas in planetary nebulae Groningen: s.n.

Citation for published version (APA): Bernard Salas, J. (2003). Physics and chemistry of gas in planetary nebulae Groningen: s.n. University of Groningen Physics and chemistry of gas in planetary nebulae Bernard Salas, Jeronimo IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite

More information

AGB stars and their environment. Michel Guélin (Presenter: Ka Tat Wong) Institut de Radioastronomie Millimétrique (IRAM) Grenoble, France

AGB stars and their environment. Michel Guélin (Presenter: Ka Tat Wong) Institut de Radioastronomie Millimétrique (IRAM) Grenoble, France AGB stars and their environment Michel Guélin (Presenter: Ka Tat Wong) Institut de Radioastronomie Millimétrique (IRAM) Grenoble, France 1. AGB stars and their winds: why, how? 2. New interferometric observations

More information

A NEW DISTANCE INDICATOR TO GALACTIC PLANETARY NEBULAE BASED UPON IRAS FLUXES

A NEW DISTANCE INDICATOR TO GALACTIC PLANETARY NEBULAE BASED UPON IRAS FLUXES THE ASTRONOMICAL JOURNAL, 115:1989È2008, 1998 May ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. A NEW DISTANCE INDICATOR TO GALACTIC PLANETARY NEBULAE BASED UPON IRAS

More information

Chapter 17: Stellar Evolution

Chapter 17: Stellar Evolution Astr 2310 Thurs. Mar. 30, 2017 Today s Topics Chapter 17: Stellar Evolution Birth of Stars and Pre Main Sequence Evolution Evolution on and off the Main Sequence Solar Mass Stars Massive Stars Low Mass

More information

8: Composition and Physical state of Interstellar Dust

8: Composition and Physical state of Interstellar Dust 8: Composition and Physical state of Interstellar Dust James Graham UC, Berkeley 1 Reading Tielens, Interstellar Medium, Ch. 5 Mathis, J. S. 1990, AARA, 28, 37 Draine, B. T., 2003, AARA, 41, 241 2 Nature

More information

Stars and their properties: (Chapters 11 and 12)

Stars and their properties: (Chapters 11 and 12) Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using

More information

Scale height and Luminosity

Scale height and Luminosity The Milky Way I suggest to consult the excellent lectures held at Saas-Fee by Gilmore, King and van der Kruit in the Book The Milky Way as a Galaxy edited by Buser & King and published by the University

More information

Physics Homework Set 2 Sp 2015

Physics Homework Set 2 Sp 2015 1) A large gas cloud in the interstellar medium that contains several type O and B stars would appear to us as 1) A) a reflection nebula. B) a dark patch against a bright background. C) a dark nebula.

More information

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Choose the answer that best completes the question. Read each problem carefully and read through all the answers.

More information

1. The AGB dust budget in nearby galaxies

1. The AGB dust budget in nearby galaxies **Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific Identifying the chemistry of the dust around AGB stars in nearby galaxies

More information

Dust. The four letter word in astrophysics. Interstellar Emission

Dust. The four letter word in astrophysics. Interstellar Emission Dust The four letter word in astrophysics Interstellar Emission Why Dust Dust attenuates and scatters UV/optical/NIR Amount of attenuation and spectral shape depends on dust properties (grain size/type)

More information

THE INTERSTELLAR MEDIUM

THE INTERSTELLAR MEDIUM THE INTERSTELLAR MEDIUM An IR view of dust clouds In particular, light from polycyclic aromatic hydrocarbons (PAH s) Little bit of carbon out there, forms hydrocarbons like car exhaust Associated with

More information

Guiding Questions. The Birth of Stars

Guiding Questions. The Birth of Stars Guiding Questions The Birth of Stars 1 1. Why do astronomers think that stars evolve (bad use of term this is about the birth, life and death of stars and that is NOT evolution)? 2. What kind of matter

More information

Nucleosynthesis and stellar lifecycles. A. Ruzicka

Nucleosynthesis and stellar lifecycles. A. Ruzicka Nucleosynthesis and stellar lifecycles A. Ruzicka Stellar lifecycles A. Ruzicka Outline: 1. What nucleosynthesis is, and where it occurs 2. Molecular clouds 3. YSO & protoplanetary disk phase 4. Main Sequence

More information

Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae

Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae Graziela R. Keller 1 Colaborators: Luciana Bianchi 2 and Walter J. Maciel 1 1 IAG/Universidade de São Paulo 2 The

More information

The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered?

The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered? The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered? Sumner Starrfield School of Earth and Space Exploration Arizona State University WHY DO WE CARE? RS Oph may

More information

Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83

Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83 Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83 J. Bernard Salas, J. R. Houck, P. W. Morris, G. C. Sloan, S. R. Pottasch, & D. J. Barry ApJS, 154, 271

More information

Gas 1: Molecular clouds

Gas 1: Molecular clouds Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,

More information

Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars

Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars Lecture 11 Stellar Evolution Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars A Spiral Galaxy (Milky Way Type) 120,000 ly A few hundred billion stars

More information

University of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16

University of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16 University of Naples Federico II, Academic Year 2011-2012 Istituzioni di Astrofisica, read by prof. Massimo Capaccioli Lecture 16 Stellar populations Walter Baade (1893-1960) Learning outcomes The student

More information

arxiv:astro-ph/ v1 10 Sep 2004

arxiv:astro-ph/ v1 10 Sep 2004 The scientific promise of the SKA SKA Workshop Oxford, 2003 Kramer & Rawlings Late stages of stellar evolution with the Square Kilometer Array arxiv:astro-ph/0409242v1 10 Sep 2004 Albert A. Zijlstra UMIST,

More information

Comparing the Period-Luminosity relationships in variable stars

Comparing the Period-Luminosity relationships in variable stars Comparing the Period-Luminosity relationships in variable stars Daniela Romero Uppsala Universitet daniela.romero1230@gmail.com June 201 Abstract There are four Period Luminosity relations from three sources,

More information

Evolution, Mass Loss and Variability of Low and Intermediate-Mass Stars

Evolution, Mass Loss and Variability of Low and Intermediate-Mass Stars Evolution, Mass Loss and Variability of Low and Intermediate-Mass Stars Mass Loss from Low and Intermediate Mass Stars Significant mass loss occurs in two phases 1. In red giants before large amplitude

More information

The Interstellar Medium

The Interstellar Medium http://www.strw.leidenuniv.nl/~pvdwerf/teaching/ The Interstellar Medium Lecturer: Dr. Paul van der Werf Fall 2014 Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium

More information

The Local Group of Galaxies

The Local Group of Galaxies The Local Group of Galaxies Two large spiral galaxies Milky Way & Andromeda (Messier 31 or M31) Distance between them: D = 700 kpc = 2.3 x 10 6 light yrs Each large spiral galaxy has several smaller satellite

More information

Late-type Stars with Perspective of Radio Observations. Youngjoo Yun 2018 Radio Winter of Ulsan

Late-type Stars with Perspective of Radio Observations. Youngjoo Yun 2018 Radio Winter of Ulsan Late-type Stars with Perspective of Radio Observations Youngjoo Yun 2018 Radio Winter School @University of Ulsan Outline l l l l Introduction to late-type stars with an example Brief description of stellar

More information

NIR Silicate features and Statistics from IRAS data

NIR Silicate features and Statistics from IRAS data NIR Silicate features and Statistics from IRAS data Ranjan Gupta Inter University Center for Astronomy and Astrophysics Pune-411007, India NIR Silicate features and Statistics from IRAS data p.1/46 Abstract

More information

Fundamental Astronomy

Fundamental Astronomy H. Karttunen P. Kroger H. Oja M.Poutanen K.J. Donner (Eds.) Fundamental Astronomy Fifth Edition With 449 Illustrations Including 34 Colour Plates and 75 Exercises with Solutions < J Springer VII 1. Introduction

More information

Interstellar Dust and Extinction

Interstellar Dust and Extinction University of Oxford, Astrophysics November 12, 2007 Outline Extinction Spectral Features Emission Scattering Polarization Grain Models & Evolution Conclusions What and Why? Dust covers a range of compound

More information

PLANETARY NEBULAE AND ALMA. Patrick Huggins, New York University

PLANETARY NEBULAE AND ALMA. Patrick Huggins, New York University PLANETARY NEBULAE AND ALMA Patrick Huggins, New York University Abell 39 PNe: Overview Reminders evolution: AGB stars proto-pne PNe white dwarfs properties Problems and challenges current observational

More information

The Later Evolution of Low Mass Stars (< 8 solar masses)

The Later Evolution of Low Mass Stars (< 8 solar masses) The Later Evolution of Low Mass Stars (< 8 solar masses) http://apod.nasa.gov/apod/astropix.html The sun - past and future central density also rises though average density decreases During 10 billion

More information

ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium:

ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium: ASTR2050 Spring 2005 Lecture 10am 29 March 2005 Please turn in your homework now! In this class we will discuss the Interstellar Medium: Introduction: Dust and Gas Extinction and Reddening Physics of Dust

More information

The Dusty Universe. Joe Weingartner George Mason University Dept of Physics and Astronomy

The Dusty Universe. Joe Weingartner George Mason University Dept of Physics and Astronomy The Dusty Universe Joe Weingartner George Mason University Dept of Physics and Astronomy To astronomers, dust means: sub micron solid grains (1 micron = 1 m = 10 6 m = one millionth of a meter) Typical

More information

The Interstellar Medium. Papillon Nebula. Neutral Hydrogen Clouds. Interstellar Gas. The remaining 1% exists as interstellar grains or

The Interstellar Medium. Papillon Nebula. Neutral Hydrogen Clouds. Interstellar Gas. The remaining 1% exists as interstellar grains or The Interstellar Medium About 99% of the material between the stars is in the form of a gas The remaining 1% exists as interstellar grains or interstellar dust If all the interstellar gas were spread evenly,

More information

Exploring ISM dust with IRSIS. Emmanuel DARTOIS IAS-CNRS

Exploring ISM dust with IRSIS. Emmanuel DARTOIS IAS-CNRS Exploring ISM dust with IRSIS Emmanuel DARTOIS IAS-CNRS IRSIS meeting 05-12-2007 Overview Intestellar ice mantles Hydrocarbons in the galaxy and outside Polycyclic Aromatic Hydrocarbons (PAHs) Interstellar

More information

Late Stages of Stellar Evolution. Late Stages of Stellar Evolution

Late Stages of Stellar Evolution. Late Stages of Stellar Evolution Late Stages of Stellar Evolution The star enters the Asymptotic Giant Branch with an active helium shell burning and an almost dormant hydrogen shell Again the stars size and luminosity increase, leading

More information

Raman Spectroscopy in Symbiotic Stars. Jeong-Eun Heo Sejong University, Korea Gemini Observatory, Chile

Raman Spectroscopy in Symbiotic Stars. Jeong-Eun Heo Sejong University, Korea Gemini Observatory, Chile Raman Spectroscopy in Symbiotic Stars Jeong-Eun Heo Sejong University, Korea Gemini Observatory, Chile Jeong-Eun, Heo Ph.D Student Dept. of Astronomy, Sejong University, Seoul, Korea The astrophysical

More information

Chapter 12 Stellar Evolution

Chapter 12 Stellar Evolution Chapter 12 Stellar Evolution Guidepost Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main

More information

The Mira variable S Ori: SiO maser shells related to the photosphere and dust shell at 3 epochs

The Mira variable S Ori: SiO maser shells related to the photosphere and dust shell at 3 epochs The Mira variable S Ori: SiO maser shells related to the photosphere and dust shell at 3 epochs Program of coordinated interferometry of oxygen-rich evolved stars at near-infrared, mid-infrared, and radio

More information

Formation and Evolution of Planetary Systems

Formation and Evolution of Planetary Systems Formation and Evolution of Planetary Systems Meyer, Hillenbrand et al., Formation and Evolution of Planetary Systems (FEPS): First Results from a Spitzer Legacy Science Program ApJ S 154: 422 427 (2004).

More information

This document is provided by JAXA.

This document is provided by JAXA. The Institute of Space and Astronautical Science Report SP No.14, December 2000 Far-Infrared Emission of Intracluster Dust (ICD) By Nobuo Arimoto Λ, Toshinobu Takagi y, and Hitoshi Hanami z (November 1,

More information

Dust & Gas around Stars Young & Old, Near & Far

Dust & Gas around Stars Young & Old, Near & Far Dust & Gas around Stars Young & Old, Near & Far Kathleen Kraemer ISR Scientific Collaborators Steve Price (BC) Greg Sloan (Cornell (formerly BC)) Don Mizuno (BC) Tom Kuchar (BC) Charles Engelke (BC) Bev

More information

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 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]

More information

Mass Loss from Red Giants

Mass Loss from Red Giants Mass Loss from Red Giants D. Reimers, R. Baade, H.-J. Hagen Hamburger Sternwarte, Universität Hamburg D. Reimers, May 30, 2007 Mass Loss from Red Giants 1/33 Halo stars - Pop II Only indirect evidence:

More information

Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization

Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others

More information

Stellar Structure and Evolution

Stellar Structure and Evolution Stellar Structure and Evolution Achim Weiss Max-Planck-Institut für Astrophysik 01/2014 Stellar Structure p.1 Stellar evolution overview 01/2014 Stellar Structure p.2 Mass ranges Evolution of stars with

More information

Life of stars, formation of elements

Life of stars, formation of elements Life of stars, formation of elements Recap life of sun Life of massive stars Creation of elements Formation of stars Profs. Jack Baldwin & Horace Smith will teach course for the remainder of the term to

More information

20. Stellar Death. Interior of Old Low-Mass AGB Stars

20. Stellar Death. Interior of Old Low-Mass AGB Stars 20. Stellar Death Low-mass stars undergo three red-giant stages Dredge-ups bring material to the surface Low -mass stars die gently as planetary nebulae Low -mass stars end up as white dwarfs High-mass

More information

VY Canis Majoris: The Astrophysical Basis of Its Luminosity

VY Canis Majoris: The Astrophysical Basis of Its Luminosity VY Canis Majoris: The Astrophysical Basis of Its Luminosity Roberta M. Humphreys School of Physics and Astronomy, University of Minnesota, 55455 ABSTRACT arxiv:astro-ph/0610433v1 13 Oct 2006 The luminosity

More information

Asteroseismology in Action: Probing the interiors of EHB stars

Asteroseismology in Action: Probing the interiors of EHB stars Asteroseismology in Action: Probing the interiors of EHB stars Suzanna Randall, ESO Garching Betsy Green, University of Arizona Gilles Fontaine, Université de Montréal Stéphane Charpinet, Observatoire

More information

Lecture 18 - Photon Dominated Regions

Lecture 18 - Photon Dominated Regions Lecture 18 - Photon Dominated Regions 1. What is a PDR? 2. Physical and Chemical Concepts 3. Molecules in Diffuse Clouds 4. Galactic and Extragalactic PDRs References Tielens, Ch. 9 Hollenbach & Tielens,

More information

Stellar Winds and Hydrodynamic Atmospheres of Stars. Rolf Kudritzki Spring Semester 2010

Stellar Winds and Hydrodynamic Atmospheres of Stars. Rolf Kudritzki Spring Semester 2010 Stellar Winds and Hydrodynamic Atmospheres of Stars Rolf Kudritzki Spring Semester 2010 I. Introduction First suspicion of existence of continuous stellar winds: Optical spectrum of P Cygni B2 hypergiant

More information

A World of Dust. Bare-Eye Nebula: Orion. Interstellar Medium

A World of Dust. Bare-Eye Nebula: Orion. Interstellar Medium Interstellar Medium Physics 113 Goderya Chapter(s): 10 Learning Outcomes: A World of Dust The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of

More information

Stellar Evolution. Eta Carinae

Stellar Evolution. Eta Carinae Stellar Evolution Eta Carinae Evolution of Main Sequence Stars solar mass star: from: Markus Bottcher lecture notes, Ohio University Evolution off the Main Sequence: Expansion into a Red Giant Inner core

More information

INTRODUCTION TO SPACE

INTRODUCTION TO SPACE INTRODUCTION TO SPACE 25.3.2019 The Galaxy II: Stars: Classification and evolution Various types of stars Interstellar matter: dust, gas Dark matter ELEC-E4530 Radio astronomy: the Sun, pulsars, microquasars,

More information

18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy

18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy 18. Stellar Birth Star observations & theories aid understanding Interstellar gas & dust in our galaxy Protostars form in cold, dark nebulae Protostars evolve into main-sequence stars Protostars both gain

More information

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines! Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities

More information

Radio Nebulae around Luminous Blue Variable Stars

Radio Nebulae around Luminous Blue Variable Stars Radio Nebulae around Luminous Blue Variable Stars Claudia Agliozzo 1 G. Umana 2 C. Trigilio 2 C. Buemi 2 P. Leto 2 A. Ingallinera 1 A. Noriega-Crespo 3 J. Hora 4 1 University of Catania, Italy 2 INAF-Astrophysical

More information

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!

More information

Chapter 19: The Evolution of Stars

Chapter 19: The Evolution of Stars Chapter 19: The Evolution of Stars Why do stars evolve? (change from one state to another) Energy Generation fusion requires fuel, fuel is depleted [fig 19.2] at higher temperatures, other nuclear process

More information