The Core-Degenerate (CD) Scenario Noam Soker Department of Physics, Technion
|
|
- Beverley Golden
- 5 years ago
- Views:
Transcription
1 The Core-Degenerate (CD) Scenario am Soker Department of Physics, Technion The Core-Degenerate (CD) scenario: The exploding object is formed at the termination of the common envelope phase from a merger of a WD companion with the hot core of a massive asymptotic giant branch star. The remnant can explode immediately, or after spinning-down. (Ilkov & Soker 2012, 2013)
2 Property (e.g., 2002ic: 1.3Mo; Livio & Riess 2003: core-wd merger) CD Scenario fits the best; Soker et al. (2013) (Poster by Danny Tsebrenko) When the can be calculated >0.1Mo close to center. M M CSM CSM size AU (Soker et al. 2013) M CSM 1 3/2 M giant left! (Wolfgang Kerzendorf) t seen progenitor/remnant H in some SNe Ia
3 Property When the can be calculated >0.1Mo close to center. (Soker et al. 2013) time -1 Delay Time t for t >1Gyr. Only stars with M MS > 2M [M > 2.3 M ; Ilkov & Soker 2013] M CSM M 3/2 x 0.8 M 1000AU CSM 1M MS t seen progenitor/remnant H in some SNe Ia
4 Delay-Time Figure from Graur, O., & Maoz, D. (2013) Slope if stars with M<2Mo [MWD=0.62Mo] contribute to SN Ia (Greggio, L., Renzini, A., & Daddi, E. 2008)
5 Property Elliptical remnants When the can be calculated >0.1Mo close to center. M M CSM CSM 1 x AU M 3/2 M (Soker et al. 2013) -1 t for t>1gyr. Only stars with M MS > 2M t seen progenitor/remnant H in some SNe Ia
6 JETS!? : ~1Mo CSM Simulations of jets Poster by Danny Tsebrenko (arxiv: last week) G SNR
7 Planetary nebulae Jets might be common in pre - SN Ia, (Tsebrenko & Soker 2013, accepted by astro-ph), although their energy is very small, unlike core collapse supernovae (CCSNe), where we think that jets explode all of them. see poster by Oded Papish see poster by Avishai Gilkis
8 Property (SN 2011fe) Single-Degenerate scenario But...OK according to Mazzali et al. (yesterday on astro-ph; arxiv : ) Thus we qualitatively favour the hydrogen-accretion scenario. Progenitor/Remnant not seen H in CSM of some SNe Ia
9 Property (SN 2011fe) Chomiuk, Laura; Soderberg, Alicia M.;..Moe, M., Chevalier, Roger A.; Rupen, M. P.; Badenes, Carles; Margutti, Raffaella; Fransson, Claes;... (2012) Practically ruled out all SD cases,..leaving..exotic single degenerate.. Single-Degenerate scenario But...OK according to Mazzali et al. (yesterday on astro-ph; arxiv : ) Thus we qualitatively favour the hydrogen-accretion scenario. Progenitor/Remnant not seen H in CSM of some SNe Ia
10 Property (SN 2011fe) Chomiuk, Laura; Soderberg, Alicia M.;..Moe, M., Chevalier, Roger A.; Rupen, M. P.; Badenes, Carles; Margutti, Raffaella; Fransson, Claes;... (2012) Practically ruled out all SD cases,..leaving..exotic single degenerate.. (Exotic? Maybe an Uranium star with cadmium where alpha particle are accreted *) Single-Degenerate scenario But...OK according to Mazzali et al. (yesterday on astro-ph; arxiv : ) Thus we qualitatively favour the hydrogen-accretion scenario. * The cadmium is needed to prevent fission chain reaction in the star Progenitor/Remnant not seen H in CSM of some SNe Ia
11 Property (SN 2011fe) Progenitor/Remnant not seen H in CSM of some SNe Ia Single-Degenerate scenario
12 Property Single-Degenerate (SN 2002ic) (SN 2011fe) Progenitor/Remnant not seen H in CSM of some SNe Ia (strong ) (strong ) Maybe OK? (Dean Townsley)
13 My view: t even one SN Ia since the big bang came from the single-degenerate route. This is strongly supported by my wife and three kids This comes from Occam s Razor Principle:
14 My view: t even one SN Ia since the big bang came from the single-degenerate route. This is strongly supported by my wife and three kids This comes from Occam s Razor Principle: The Iron in the Razor does not come from explosion of a SD scenario.
15 Property DD1 DD2 DD3 CD ; Violent merger (Pakmor et al.) Double Detonation (from Ken Shen 2013) WD-WD Collisin (Kushnir et al. 2013) Can be Violent or d-detonation in prompt explosion (can explain 0 ± 1% of all SN Ia) (Hamers et for number al. 2013) Slope under construction (SN 2011fe) Some might have Progenitor/Remnant not seen?? H in some CSM (0.001Mo)? Merger rate of WD (Badenes Maoz 2012) Good for DD, but not for all ignition processes t relevant t relevant
16 Summary (my view): The Property DD2+CD DD1 DD2 DD3 CD Collision act together (Kushnir et al. 2013) Violent merger (Pakmor et al.) For these use Coredegenerate Double Detonation For these use Coredegenerate Can be Violent d-detonation in prompt explosion for number Slope? else: use DD (SN 2011fe) Some might have Progenitor/Remnant not seen??? H in some CSM use CD use CD? Merger rate of WD (Badenes Maoz 2012) Good for DD, but not for all ignition processes t relevant t relevant
Pleasantness Review*
Pleasantness Review* Department of Physics, Technion, Israel Nebulae powered by a central explosion Garching 2015 Noam Soker Essential collaborators (Technion): Muhammad Akashi, Danny Tsebrenko, Avishai
More informationPleasantness Review* Department of Physics, Technion, Israel. Noam Soker
Pleasantness Review* Department of Physics, Technion, Israel The role of jets: from common envelope to nebulae Nice 2015 Noam Soker Essential collaborators (Technion): Amit Kashi, Muhammad Akashi, Ealeal
More informationEvolution and Final Fates of Accreting White Dwarfs. Ken Nomoto (Kavli IPMU / U. Tokyo)
Evolution and Final Fates of Accreting White Dwarfs Ken Nomoto (Kavli IPMU / U. Tokyo) AD 1572 Korean & Chinese Record Guest Star as bright as Venus (Sonjo Sujong Sillok: Korea) AD 1572 Tycho Brahe s Supernova
More informationSN1987A before(right) and during the explosion. Supernova Explosion. Qingling Ni
SN1987A before(right) and during the explosion Supernova Explosion Qingling Ni Overview Core-Collapse supernova (including Type II supernova) -Mechanism: collapse+rebound Type Ia supernova -Mechanism:
More informationGuiding 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 informationThe 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 informationGuiding 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 informationStellar 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 informationFifty-One Ergs. An International Conference on the Physics and Observations of Supernovae and Supernova Remnants. Program
Fifty-One Ergs An International Conference on the Physics and Observations of Supernovae and Supernova Remnants Program Monday, May 13 th 8:30 Warwick Arden Welcome address by The Provost of NC State 8:45
More informationIntroductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
More informationProf. Kenney Class 8 June 6, 2018
Prof. Kenney Class 8 June 6, 2018 differences in textbook editions 10 th ed vs 8 th & 9 th ed all chapter assignments starting with ch 21 on are shifted by 1 in 10th edition relative to 8th, 9th editions
More informationStellar Explosions (ch. 21)
Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least
More informationarxiv: v1 [astro-ph.sr] 19 Sep 2010
Type Ia Supernovae and Accretion Induced Collapse A. J. Ruiter, K. Belczynski,, S. A. Sim, W. Hillebrandt, M. Fink and M. Kromer arxiv:1009.3661v1 [astro-ph.sr] 19 Sep 2010 Max Planck Institute for Astrophysics,
More informationWhite dwarf collisions: a new pathway to type Ia supernovae. Enrique García-Berro & Pablo Lorén-Aguilar
White dwarf collisions: a new pathway to type Ia supernovae Enrique García-Berro & Pablo Lorén-Aguilar Supernovae, hypernovae and binary driven hypernovae An Adriatic Workshop Pescara 2016 CONTENTS 1.
More informationWhite dwarf dynamical interactions. Enrique García-Berro. Jornades de Recerca, Departament de Física
White dwarf dynamical interactions Enrique García-Berro Jornades de Recerca, Departament de Física CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
More informationarxiv: v3 [astro-ph.sr] 21 Sep 2012
THE NUMBER OF PROGENITORS IN THE CORE - DEGENERATE SCENARIO FOR TYPE IA SUPERNOVAE Marjan Ilkov 1 and Noam Soker 1 ABSTRACT arxiv:1208.0953v3 [astro-ph.sr] 21 Sep 2012 We calculate the expected number
More informationChapter 12: The Life Cycle of Stars (contʼd) How are stars born, and how do they die? 4/9/09 Habbal Astro Lecture 25 1
Chapter 12: The Life Cycle of Stars (contʼd) How are stars born, and how do they die? 4/9/09 Habbal Astro 110-01 Lecture 25 1 12.3 Life as a High-Mass Star Learning Goals What are the life stages of a
More informationStars 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 informationCore-collapse supernovae are thermonuclear explosions
Core-collapse supernovae are thermonuclear explosions Doron Kushnir Collaborators: Boaz Katz (WIS), Kfir Blum (WIS), Roni Waldman (HUJI) 17.9.2017 The progenitors are massive stars SN2008bk - Red Super
More informationRemnants of Type Ia Supernovae
Remnants of Type Ia Supernovae Brian J. Williams NPP Fellow NASA GSFC Collaborators: Steve Reynolds, Kazik Borkowski, John Blondin (NCSU), Rob Petre, Jack Hewitt (GSFC), Frank Winkler (Middlebury), Knox
More informationChapter 15. Supernovae Classification of Supernovae
Chapter 15 Supernovae Supernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe, typically producing about 10 53 erg, with a large fraction of
More informationBrian P. Schmidt Wolfgang Kerzendorf, Anna Frebel, Martin Asplund, Ken Nomoto, Philipp Podsiadlowski
Brian P. Schmidt Wolfgang Kerzendorf, Anna Frebel, Martin Asplund, Ken Nomoto, Philipp Podsiadlowski The Research School of Astronomy & Astrophysics Mount Stromlo and Siding Spring Observatories 1 2 SkyMapper
More informationThe Progenitors of Type Ia Supernovae
The Progenitors of Type Ia Supernovae Philipp Podsiadlowski, Richard Booth, Mark Sullivan (Oxford), Shazrene Mohamed (Bonn), Paolo Mazzali (MPA/Padova), Zhanwen Han (Kunming), Stephen Justham (Beijing),
More informationPost Activity/ Homework Questions: 1. Before a star forms A. Where do you think the gas and dust originally came from?
Critical Thinking Questions: (work on these with a partner) 1. During the formation of a Red Giant Star, the core of a star pushes the outer shell back only enough to make the star larger. However, during
More informationWhat Are Type Ia Supernovae?
What Are Type Ia Supernovae? Max-Planck-Institut für Astrophysik Based on collaborations with: W. Hillebrandt (MPA Garching) S.E. Woosley (UC Santa Cruz) M. Reinecke (MPA Garching) B. Leibundgut (ESO Garching)
More information17.3 Life as a High-Mass Star
17.3 Life as a High-Mass Star Our goals for learning: What are the life stages of a high-mass star? How do high-mass stars make the elements necessary for life? How does a high-mass star die? What are
More informationLecture 26. High Mass Post Main Sequence Stages
Lecture 26 Fate of Massive Stars Heavy Element Fusion Core Collapse Supernova Neutrinoes Gaseous Remnants Neutron Stars Mar 27, 2006 Astro 100 Lecture 26 1 High Mass Post Main Sequence Stages For M(main
More informationToday. Stars. Evolution of High Mass Stars. Nucleosynthesis. Supernovae - the explosive deaths of massive stars
Today Stars Evolution of High Mass Stars Nucleosynthesis Supernovae - the explosive deaths of massive stars 1 Another good job on exam! Class average was 71% Given the difficulty of the exam, this was
More informationPhysics 5K Lecture 5 - Friday May 4, Atoms. Joel Primack Physics Department UCSC. Friday, May 4, 12
Physics 5K Lecture 5 - Friday May 4, 2012 Atoms Joel Primack Physics Department UCSC Giancoli The Electromagnetic Spectrum Brief History of Atomic Theory 1904 Joseph J. Thomson s "Plum Pudding" model
More informationThis class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)
This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)!1 Cas$A$ All$Image$&$video$credits:$Chandra$X7ray$ Observatory$
More informationLecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4
Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Key Ideas HR Diagrams of Star Clusters Ages from the Main Sequence Turn-off Open Clusters Young clusters of ~1000 stars Blue Main-Sequence
More informationNuclear Physics and Astrophysics of Exploding Stars
Nuclear Physics and Astrophysics of Exploding Stars Lars Bildsten Kavli Institute for Theoretical Physics Department of Physics University of California, Santa Barbara Dan Kasen (UCSC), Kevin Moore (UCSB),
More informationAstronomy. Astrophysics. The birth rate of supernovae from double-degenerate and core-degenerate systems. X. Meng 1,2 and W. Yang 1,3. 1.
A&A 543, A137 (2012) DOI: 10.1051/0004-6361/201218810 c ESO 2012 Astronomy & Astrophysics The birth rate of supernovae from double-degenerate and core-degenerate systems X. Meng 1,2 and W. Yang 1,3 1 School
More informationThe structure and evolution of stars. Learning Outcomes
The structure and evolution of stars Lecture14: Type Ia Supernovae The Extravagant Universe By R. Kirshner 1 Learning Outcomes In these final two lectures the student will learn about the following issues:
More informationarxiv: v2 [astro-ph.sr] 16 Feb 2015
The response of a helium white dwarf to an exploding type Ia supernova Oded Papish 1, Noam Soker 1, Enrique García Berro 2,3, and Gabriela Aznar Siguán 2,3 ABSTRACT arxiv:1410.1153v2 [astro-ph.sr] 16 Feb
More informationThe electrons then interact with the surrounding medium, heat it up, and power the light curve. 56 Ni 56 Co + e (1.72 MeV) half life 6.
Supernovae The spectra of supernovae fall into many categories (see below), but beginning in about 1985, astronomers recognized that there were physically, only two basic types of supernovae: Type Ia and
More informationFriday, March 21, 2014 Reading for Exam 3: End of Section 6.6 (Type Ia binary evolution), 6.7 (radioactive decay), Chapter 7 (SN 1987A), NOT Chapter
Friday, March 21, 2014 Reading for Exam 3: End of Section 6.6 (Type Ia binary evolution), 6.7 (radioactive decay), Chapter 7 (SN 1987A), NOT Chapter 8 (Neutron Stars), keep for Exam 4. Background: Sections
More informationThe Evolution of Close Binaries
The Evolution of Close Binaries Philipp Podsiadlowski (Oxford) The case of RS Ophiuchi as a test of binary stellar evolution as a potential Type Ia supernova (SN Ia) progenitor I. Testing Binary Evolution:
More informationSupernova Explosions. Novae
Supernova Explosions Novae Novae occur in close binary-star systems in which one member is a white dwarf. First, mass is transferred from the normal star to the surface of its white dwarf companion. 1
More informationAstronomy II (ASTR1020) Exam 3 Test No. 3D
Astronomy II (ASTR1020) Exam 3 Test No. 3D 23 October 2001 The answers of this multiple choice exam are to be indicated on the Scantron with a No. 2 pencil. Don t forget to write your name and the Test
More informationReading and Announcements. Read Chapter 14.1, 14.2 Homework #6 due Tuesday, March 26 Exam #2, Thursday, March 28
Reading and Announcements Read Chapter 14.1, 14.2 Homework #6 due Tuesday, March 26 Exam #2, Thursday, March 28 The life of the Sun The Sun started as a cloud of gas. Gravity caused the cloud to collapse.
More informationThe Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.
The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. Once the giant phase of a mediummass star ends, it exhales its outer
More informationarxiv: v1 [astro-ph] 31 Jul 2007
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 10 May 2008 (MN LATEX style file v2.2) On the fraction of intermediate-mass close binaries that explode as type-ia supernovae arxiv:0707.4598v1 [astro-ph]
More informationSupernovae Through the Ages
Supernovae Through the Ages We ourselves are stardust. -Carl Sagan Jason Kezwer September 11, 2013 Outline - What are supernovae? Why are they important? - An observational history - How supernovae affect
More informationStellar Astronomy Sample Questions for Exam 4
Stellar Astronomy Sample Questions for Exam 4 Chapter 15 1. Emission nebulas emit light because a) they absorb high energy radiation (mostly UV) from nearby bright hot stars and re-emit it in visible wavelengths.
More informationDiverse Energy Sources for Stellar Explosions. Lars Bildsten Kavli Institute for Theoretical Physics University of California Santa Barbara
Diverse Energy Sources for Stellar Explosions Lars Bildsten Kavli Institute for Theoretical Physics University of California Santa Barbara Traditional Energy Sources Core collapse to NS or BH depositing
More informationType Ia supernovae observable nuclear astrophysics
Astrophysics and Nuclear Structure Hirschegg, January 27, 2013 Type Ia supernovae observable nuclear astrophysics Julius-Maximilians-Universität Würzburg, Germany W. Hillebrandt, S. Woosley, S. Sim, I.
More informationChapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc.
Chapter 14: The Bizarre Stellar Graveyard Assignments 2 nd Mid-term to be held Friday Nov. 3 same basic format as MT1 40 mult. choice= 80 pts. 4 short answer = 20 pts. Sample problems on web page Origin
More informationScience Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017
Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017 Team Name: Team Number: Directions: ~Answer all questions on the answer sheet provided. ~Please do NOT access the
More informationSupernova Explosions. Novae
Supernova Explosions Novae Novae occur in close binary-star systems in which one member is a white dwarf. First, mass is transferred from the normal star to the surface of its white dwarf companion. 1
More informationProtostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium
Protostars on the HR Diagram Once a protostar is hot enough to start, it can blow away the surrounding gas Then it is visible: crosses the on the HR diagram The more the cloud, the it will form stars Lifetimes
More informationObservable constraints on nucleosynthesis conditions in Type Ia supernovae
Observable constraints on nucleosynthesis conditions in Type Ia supernovae MPE Eurogenesis Garching, March 26, 2013 Ivo Rolf Seitenzahl Institut für Theoretische Physik und Astrophysik Julius-Maximilians-Universität
More informationSupernovae, Neutron Stars, Pulsars, and Black Holes
Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Stellar Deaths/Endpoints 13-2 Low Mass Stars ³ Like the Sun (< 2 M ) ² Live about 10 billion years (sun is middle aged) ² Create elements through Carbon, Nitrogen,
More informationCh. 29 The Stars Stellar Evolution
Ch. 29 The Stars 29.3 Stellar Evolution Basic Structure of Stars Mass effects The more massive a star is, the greater the gravity pressing inward, and the hotter and more dense the star must be inside
More informationThe Evolution of Low Mass Stars
The Evolution of Low Mass Stars Key Ideas: Low Mass = M < 4 M sun Stages of Evolution of a Low Mass star: Main Sequence star star star Asymptotic Giant Branch star Planetary Nebula phase White Dwarf star
More informationOutline - March 18, H-R Diagram Review. Protostar to Main Sequence Star. Midterm Exam #2 Tuesday, March 23
Midterm Exam #2 Tuesday, March 23 Outline - March 18, 2010 Closed book Will cover Lecture 8 (Special Relativity) through Lecture 14 (Star Formation) only If a topic is in the book, but was not covered
More informationAstronomy 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 informationLecture 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
More informationModels of Type Ia supernova explosions
Fifty-one erg workshop Raleigh, May 14, 2013 Models of Type Ia supernova explosions Julius-Maximilians-Universität Würzburg, Germany I. Seitenzahl, M. Fink, R. Pakmor, S. Sim, M. Kromer, A. Summa, F. CiaraldiSchoolmann,
More informationTHE 82ND ARTHUR H. COMPTON LECTURE SERIES
THE 82ND ARTHUR H. COMPTON LECTURE SERIES by Dr. Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow FLASH Center for Computational Science Department of Astronomy & Astrophysics University of Chicago
More informationPHYS 1401: Descriptive Astronomy Notes: Chapter 12
CHAPTER 12: STELLAR EVOLUTION 12.1: LEAVING THE MAIN SEQUENCE Stars and the Scientific Method You cannot observe a single star from birth to death You can observe a lot of stars in a very short period
More informationSupernovae and cosmology
Supernovae and cosmology On the Death of Stars and Standard Candles Gijs Hijmans Supernovae Types of Supernovae Type I Ia (no hydrogen but strong silicon lines in spectrum) Ib (non ionized helium lines)
More informationarxiv: v1 [astro-ph.he] 1 Aug 2013
SUBMITTED FOR PUBLICATION IN THE ASTROPHYSICAL JOURNAL Preprint typeset using LATEX style emulateapj v. 5/2/11 RECONCILING 56 NI PRODUCTION IN TYPE IA SUPERNOVAE WITH DOUBLE DEGENERATE SCENARIOS ANTHONY
More informationBoris Gänsicke. Type Ia supernovae and their progenitors
Boris Gänsicke Type Ia supernovae and their progenitors November 1572, in Cassiopeia: a nova a new star V~-4 Tycho Brahe: De nova et nullius aevi memoria prius visa stella (1602) October 9, 1604, in Ophiuchus
More informationOutline. Stellar Explosions. Novae. Death of a High-Mass Star. Binding Energy per nucleon. Nova V838Mon with Hubble, May Dec 2002
Outline Novae (detonations on the surface of a star) Supernovae (detonations of a star) The Mystery of Gamma Ray Bursts (GRBs) Sifting through afterglows for clues! Stellar Explosions Novae Nova V838Mon
More informationR-process in Low Entropy Neutrino Driven Winds
R-process in Low Entropy Neutrino Driven Winds E. Baron John J. Cowan, Tamara Rogers, 1 and Kris Gutierrez 2 Dept. of Physics and Astronomy, University of Oklahoma, 440 W. Brooks, Rm 131, Norman, OK 73019-0225
More informationEvolution of Low-Mass stars M < 4 M sun No C Burning!
Evolution of Low-Mass stars M < 4 M sun No C Burning! C-O Core Envelope Ejection 0.1Myr Luminosity (L sun ) 10 6 10 4 10 2 1 10-2 10-4 C-O White Dwarf (forever) Asymptotic Giant Branch C-O core contraction,
More informationChapter 12 Review. 2) About 90% of the star's total life is spent on the main sequence. 2)
Chapter 12 Review TRUE/FALSE. Write 'T' if the statement is true and 'F' if the statement is false. 1) As a main-sequence star, the Sun's hydrogen supply should last about 10 billion years from the zero-age
More informationFollow the Angular Momentum! Pleasantness Review
Follow the Angular Momentum! Summary talk of the April 8-12, 2013, ESO Meeting The deaths of stars and the lives of galaxies Noam Soker Department of Physics, Technion ** Biased and personal summary. When
More informationThe 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
More informationarxiv: v1 [astro-ph.he] 17 Jan 2016
September 16, 2018 10:53 WSPC Proceedings - 9.75in x 6.5in main page 1 1 Quark-Noave in binaries: Observational signatures and implications to astrophysics Rachid Ouyed, Denis Leahy, Nico Koning Department
More informationChapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.
Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect
More informationChapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5
Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5 20.4 Evolution of Stars More Massive than the Sun It can be seen from this H-R diagram that stars more massive than the Sun follow very different paths
More informationProtostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium
Protostars on the HR Diagram Once a protostar is hot enough to start, it can blow away the surrounding gas Then it is visible: crosses the on the HR diagram The more the cloud, the it will form stars Lifetimes
More informationSearching for the Progenitors of Subluminous Type Ia Supernovae with SN 2013bc
Hubble Space Telescope Cycle 11 General Observer Proposal Searching for the Progenitors of Subluminous Type Ia Supernovae with SN 2013bc Principal Investigator: Institution: Electronic mail: Maximilian
More informationAstronomy in the news? Patriots goal-line interception
Monday, February 2, 2015 First exam Friday. First Sky Watch Due. Review sheet posted Today. Review session Thursday, 5 6 PM, RLM 6.104 Reading: Chapter 6 Supernovae, Sections 6.1, 6.2, 6.3 Chapter 1 Introduction,
More informationThe SWARMS Survey: Unveiling the Galactic population of Compact White Dwarf Binaries
The SWARMS Survey: Unveiling the Galactic population of Compact White Dwarf Binaries Weizmann Institute of Science / Tel-Aviv University Type Ia SN Progenitors Workshop Leiden, September 22 2010 Steve
More informationAstronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
More informationAstronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
More informationImpact of Type Ia Supernova Ejecta on Binary Companions
Impact of Type Ia Supernova Ejecta on Binary Companions Speaker: Kuo-Chuan Pan (ASTR) Charm++ Workshop, April 18, 2011 1 [Dept. of Astronomy] Advisor: Prof. Paul Ricker Collaborator: Prof. Ronald Taam
More informationThe dying sun/ creation of elements
The dying sun/ creation of elements Homework 6 is due Thurs, 2 April at 6:00am OBAFGKM extra credit Angel: Lessons>Extra Credit Due 11:55pm, 31 March Final exam (new, later time) 6 May, 3:00-5:00, BPS
More information10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure
10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds
More informationChapter 6: Stellar Evolution (part 2): Stellar end-products
Chapter 6: Stellar Evolution (part 2): Stellar end-products Final evolution stages of high-mass stars Stellar end-products White dwarfs Neutron stars and black holes Supernovae Core-collapsed SNe Pair-Instability
More informationPlanetary Nebulae White dwarfs
Life of a Low-Mass Star AST 101 Introduction to Astronomy: Stars & Galaxies Planetary Nebulae White dwarfs REVIEW END STATE: PLANETARY NEBULA + WHITE DWARF WHAS IS A WHITE DWARF? Exposed core of a low-mass
More informationThe Evolution of Stellar Triples
The Evolution of Stellar Triples Silvia Toonen toonen@uva.nl Simon Portegies Zwart, Tjarda Boekholt, Adrian Hamers, Hagai Perets, Fabio Antonini Triple evolution Isolated Hierarchical Stellar triples:
More informationA search for supernova type Ia progenitors in the Magellanic Clouds. Kelly Lepo
A search for supernova type Ia progenitors in the Magellanic Clouds by Kelly Lepo A thesis submitted in conformity with the requirements for the degree of Doctor of Philosophy Graduate Department of Astronomy
More informationSTELLAR DEATH, AND OTHER THINGS THAT GO BOOM IN THE NIGHT. Kevin Moore - UCSB
STELLAR DEATH, AND OTHER THINGS THAT GO BOOM IN THE NIGHT Kevin Moore - UCSB Overview Stellar evolution basics! Fates of stars related to their mass! Mass transfer adds many possibilities Historical supernovae
More informationAstronomy 110: SURVEY OF ASTRONOMY. 11. Dead Stars. 1. White Dwarfs and Supernovae. 2. Neutron Stars & Black Holes
Astronomy 110: SURVEY OF ASTRONOMY 11. Dead Stars 1. White Dwarfs and Supernovae 2. Neutron Stars & Black Holes Low-mass stars fight gravity to a standstill by becoming white dwarfs degenerate spheres
More informationThe Theory of Supernovae in Massive Binaries
The Theory of Supernovae in Massive Binaries Philipp Podsiadlowski (Oxford) the majority of massive stars are in interacting binaries the large diversity of observed supernova types and (sub-)types is
More informationThe Algol Mystery. Binary Evolution Novae, Supernovae, and X-ray Sources. Algol. Mass Transfer in Binaries
The Algol Mystery Binary Evolution Novae, Supernovae, and X-ray Sources http://apod.nasa.gov/apod/ Algol is a double-lined eclipsing binary system with a period of about 3 days (very short). The two stars
More informationCHAPTER 14 II Stellar Evolution
14-5. Supernova CHAPTER 14 II Stellar Evolution Exactly which stars become supernovae is not yet clear, but more than likely they are massive stars that become highly evolved. A star that develops an iron
More informationLecture 24. Reprise: Evolution Timescale
Lecture 24 Life as a Low Mass Giant Dating the Stars Shell vs Core Fusion Helium Fusion Planetary Nebulae Mar 22, 2006 Astro 100 Lecture 24 1 Reprise: Evolution Timescale To estimate the duration of any
More informationObservational summary
Observational summary Andy Howell Las Cumbres Observatory Global Telescope Network University of California Santa Barbara Entertainment value Scientific quality Rene Magritte: The Treachery of Images
More informationChapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.
Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect nuclear
More informationoptical / IR: photon counting flux density or magnitude corresponds to number of electrons per second (mean rate)
optical / IR: photon counting flux density or magnitude corresponds to number of electrons per second (mean rate) N electrons/sec = ɛ F λ λa hc/λ 0 efficiency factor flux density x bandpass x collecting
More informationLecture 8: Stellar evolution II: Massive stars
Lecture 8: Stellar evolution II: Massive stars Senior Astrophysics 2018-03-27 Senior Astrophysics Lecture 8: Stellar evolution II: Massive stars 2018-03-27 1 / 29 Outline 1 Stellar models 2 Convection
More informationRelativistic Astrophysics Neutron Stars, Black Holes & Grav. W. ... A brief description of the course
Relativistic Astrophysics Neutron Stars, Black Holes & Grav. Waves... A brief description of the course May 2, 2009 Structure of the Course Introduction to General Theory of Relativity (2-3 weeks) Gravitational
More informationEinführung 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 informationWednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM
Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM RLM 15.216B (Backup RLM 15.202A) Reading: Chapter 6
More information