Planets around evolved stellar systems. Tom Marsh, Department of Physics, University of Warwick
|
|
- Frank Griffin
- 5 years ago
- Views:
Transcription
1 Planets around evolved stellar systems Tom Marsh Department of Physics, University of Warwick Tom Marsh, Department of Physics, University of Warwick Slide 1 / 35
2 Tom Marsh, Department of Physics, University of Warwick Slide 2 / 35 Outline 1. White dwarfs 2. White dwarf binary stars 3. ULTRACAM 4. Eclipsing white dwarfs 5. Timing measurements 6. A role for variable star observers? 7. Conclusions
3 Tom Marsh, Department of Physics, University of Warwick Slide 3 / 35 White Dwarfs The most common end-point of stellar evolution; 95% of all stars > 1 M become white dwarfs. A typical white dwarf is comparable in size to Earth, but with a mass similar to the Sun, they have mean densities ρ 1 tonne per cc. There are around 1000 million white dwarfs in our Galaxy. NGC 6543 (Cat s Eye), with nascent white dwarf (HST)
4 Tom Marsh, Department of Physics, University of Warwick Slide 4 / 35 White dwarfs & Type Ia Supernovae Exploding white dwarfs are thought to make the Type Ia supernovae (2011 Physics Nobel Prize dark energy ): 1. Add mass to a white dwarf 2. As mass nears 1.4 M, the white dwarf shrinks and compresses. 3. Carbon/Oxygen material undergoes runaway fusion... Khoklov et al (1997)
5 Tom Marsh, Department of Physics, University of Warwick Slide 4 / 35 White dwarfs & Type Ia Supernovae Exploding white dwarfs are thought to make the Type Ia supernovae (2011 Physics Nobel Prize dark energy ): 1. Add mass to a white dwarf 2. As mass nears 1.4 M, the white dwarf shrinks and compresses. 3. Carbon/Oxygen material undergoes runaway fusion... Khoklov et al (1997)
6 Tom Marsh, Department of Physics, University of Warwick Slide 5 / 35 Tycho s supernova was a Type Ia Remnant of an exploded white dwarf in X-rays (Tycho s SN of 1572, now about 30 light-years across). Light-echo from Tycho s SN shows that it was a Type Ia
7 Tom Marsh, Department of Physics, University of Warwick Slide 6 / 35 White Dwarfs in Binary Stars Modern astronomical surveys are producing large numbers of white dwarfs in binary systems. So many, that even the exclusive class of eclipsing systems is growing rapidly Number of eclipsers known vs time
8 Tom Marsh, Department of Physics, University of Warwick Slide 7 / 35 CVs accreting white dwarfs Cataclysmic variables are a long-lived phase of evolution in which mass transfer is driven by weak angular momentum loss. They give us the chance to measure the build-up or otherwise of mass on white dwarfs.
9 Tom Marsh, Department of Physics, University of Warwick Slide 8 / 35 Detached WD+MS systems Simple systems with spectra which are a combination of white dwarfs and low-mass main-sequence stars. Can be detected through simultaneous flux excess in ultraviolet and red filters. Around 2000 now known, mostly from the Sloan Digital Sky Survey. Pyrzas et al (2009), spectra of 4 eclipsing WD/dM systems.
10 Tom Marsh, Department of Physics, University of Warwick Slide 9 / 35 ULTRACAM White dwarfs are small, with orbital speeds at their surfaces of 4000 km s 1. They must be observed fast to resolve variations, typically 1 to 30 sec. In May 2002 we commissioned a new high-speed camera to facilitate observations of white dwarf binary stars. ULTRACAM mounted on the 4.2m WHT in La Palma
11 Tom Marsh, Department of Physics, University of Warwick Slide 10 / 35 ULTRACAM To reduce light-losses due to filters, in ULTRACAM we split the light up into three bands, UV, green and red, before imaging. The detectors used are frame transfer CCDs in which one exposure is taken while the previous one is being read out. Can take 100s of frames/second with high efficiency. Timestamps are taken from the GPS. ULTRACAM design
12 Tom Marsh, Department of Physics, University of Warwick Slide 11 / 35 ULTRACAM ULTRACAM and two astronomers ULTRACAM at the 8.2 m VLT, Cerro Paranal, Chile
13 Tom Marsh, Department of Physics, University of Warwick Slide 12 / 35 White dwarf / main-sequence eclipsers Exquisite measurements are possible on large telescopes (the VLT in this case). [Magnitude: V = 17.0, eclipse length: 10 mins, exposure time: 1.5 sec.] Parsons et al (2010a), GK Vir, a hot WD M M-dwarf eclipser.
14 Tom Marsh, Department of Physics, University of Warwick Slide 13 / 35 White dwarf + very low mass star Very dim companions are outshone by the white dwarf at all wavelengths. Rise in between eclipses caused by heating of cool star by the white dwarf. The dip at the top of the lightcurve occurs as the white dwarf transits the heated face. T W = 35, 300 K, M W = 0.51 M, M C = 0.09 M. Parsons et al (2011), CSS 03170, P = 94 mins
15 NN Serpentis In the best cases, complete solution of M W, R W, M R, R R and i is possible. e.g NN Ser M W = ± M R W = ± R M R = ± M R R = ± R i = 89.6 ± 0.2. Parsons et al (2010b), NN Ser. Tom Marsh, Department of Physics, University of Warwick Slide 14 / 35
16 Tom Marsh, Department of Physics, University of Warwick Slide 15 / 35 Testing Equations of State These are good enough to test models of both white dwarfs and very low mass stars (and, potentially, brown dwarfs), themselves dependent upon the behaviour of high density matter. Parsons et al (2010b)
17 Tom Marsh, Department of Physics, University of Warwick Slide 16 / 35 One motivation for high-speed work is to study the angular momentum loss that drives binary evolution. A steady rate of period change Ṗ alters the times of eclipse by a quadratic function of time t = 1 Ṗ 2 P t2. Timing studies In practice, rather erratic variations always seem to be the rule. Period changes in WD/dM system QS Vir, O Donoghue et al (2003)
18 Tom Marsh, Department of Physics, University of Warwick Slide 17 / 35 Applegate s Mechanism Applegate (1992) suggested that such variations are driven by variations in the shape of the MS star driven by solar type cycles. No angular momentum is lost in the process; Applegate s mechanism is not a driver of evolution. Applegate s mechanism does require energy however. Variations in shape alter the gravitational attraction between the stars
19 Tom Marsh, Department of Physics, University of Warwick Slide 18 / 35 Violating Applegate We have found that some systems show too large a period change for the MS star to have supplied the energy needed. Here the eclipses in QS Vir are seen to arrive 200 sec earlier than expected from O Donoghue et al. s data. It seems certain that there is a third body orbiting the binary, probably a brown dwarf ULTRACAM Last 3 O Donoghue times ULTRACAM QS Vir, Parsons et al (2010)
20 Tom Marsh, Department of Physics, University of Warwick Slide 19 / 35 Third bodies from timing Unseen object Unseen object different time Eclipse arrival time delayed or advanced
21 Tom Marsh, Department of Physics, University of Warwick Slide 20 / 35 Planets! NN Ser is the best measured system to date. Its timing variation in NN Ser can be fit to within very small errors with two planets, M c sin i = 6.9 M J, M d sin i = 2.2 M J in 15.5 and 7.7 yr orbits. Two planet fit to NN Ser times, Beuermann et al (2010)
22 Tom Marsh, Department of Physics, University of Warwick Slide 21 / 35 Planets around a CV Here, M c sin i = 6.3 M J, M d sin i = 7.7 M J, with periods of 16 and 5.3 years. System here is accreting and so may be subject to variability-induced scatter. In optimum cases such as NN Ser, timing is sensitive to planets of a few Earth masses in long period orbits. Two planet fit to UZ For times, Potter et al (2011)
23 Tom Marsh, Department of Physics, University of Warwick Slide 22 / 35 Liverpool Telescope Project Even well-measured systems can be hard to pin down, and well-spaced sampling is needed. Start using robotic Liverpool Telescope data to extend coverage. Some possible orbits of NN Ser given the data in hand.
24 Tom Marsh, Department of Physics, University of Warwick Slide 23 / 35 First LT results (started Feb 2011) Upper panel: an eclipse of NN Ser; lower panel: QS Vir times. More than 30 eclipses of different systems measured.
25 Tom Marsh, Department of Physics, University of Warwick Slide 24 / 35 All systems show timing anomalies... RR Caelum RXJ
26 Tom Marsh, Department of Physics, University of Warwick Slide 25 / 35 Are the planets really there? Orbital stability can place strong constraints upon multiple-planet systems. In NN Ser, the planets seems to be close to a 2:1 resonance. New data has significantly shrunk the allowable parameter space, but is still consistent with the 2:1 resonance.
27 Perhaps not always... Tom Marsh, Department of Physics, University of Warwick Slide 26 / 35
28 Tom Marsh, Department of Physics, University of Warwick Slide 27 / 35 Test with double eclipsing white dwarfs Pairs of eclipsing of white dwarfs should be much less vulnerable to stellar-induced timing noise than white dwarf/main-sequence binaries. Although the chances are low, the first such system, NLTT 11748, was discovered last year. 0.2 M M pair of white dwarfs in a 5.6-hour, at 0.1 from being exactly edge-on. The eclipses are total but only 6% and 3% deep.
29 Tom Marsh, Department of Physics, University of Warwick Slide 28 / 35 A second eclipsing DWD This year we discovered a second with 40% and 10% deep eclipses using Liverpool Telescope and Gemini data. Remarkably 4 are now known. If these systems show planets, it will be a firm indication of their reality. Watch this space!
30 Tom Marsh, Department of Physics, University of Warwick Slide 29 / 35 Origin of the circum-binary planets Systems like NN Ser are only a solar radius or so apart, with orbital periods of 10 hours or less. However prior to the formation of the white dwarf they were 1.5 AU apart, raising problems with stability of the planets. Two possibilities: 1. The planets predated the white dwarf and spiralled in as the white dwarf lost its envelope 2. The planets formed out of the material lost by the white dwarf.
31 Tom Marsh, Department of Physics, University of Warwick Slide 30 / 35 Calling Variable Star Observers In several cases we are limited by coverage with large gaps. Some systems have variations of order a minute or more. There are a few systems V471 Tau, QS Vir, DE CVn, RXJ and (for Australians) RR Cae within reach of small telescopes. Please contact me at tom.marsh@warwick.ac.uk if you are interested.
32 Tom Marsh, Department of Physics, University of Warwick Slide 31 / and a couple of longshots... White dwarfs could be totally eclipsed by any planets they host. Two interesting possibilities: G24-9 aka V1412 Aql: V = white dwarf with two reports of 2 mag. eclipses. Arno Landolt requested an AAVSO campaign in Feb No reports of success, but very interesting to continue this. EG 131: V = 12.3, a white dwarf but reported as varying by ±0.35 mag.
33 Tom Marsh, Department of Physics, University of Warwick Slide 32 / 35 V471 Tau with ULTRACAM V471 Tau (V = 9.8) is bright, but lacks nearby comparison stars (ULTRACAM FOV = 5 to 6 ).
34 Tom Marsh, Department of Physics, University of Warwick Slide 33 / 35 V471 Tau with ULTRACAM V471 Tau (V = 9.8) is bright, but lacks nearby comparison stars (ULTRACAM FOV = 5 to 6 ). The eclipse is much stronger in the UV than in red light, so with ULTRACAM we can use V471 Tau as its own comparison!
35 Tom Marsh, Department of Physics, University of Warwick Slide 34 / 35 V471 Tau with ULTRACAM V471 Tau (V = 9.8) is bright, but lacks nearby comparison stars (ULTRACAM FOV = 5 to 6 ). The eclipse is much stronger in the UV than in red light, so with ULTRACAM we can use V471 Tau as its own comparison!
36 Tom Marsh, Department of Physics, University of Warwick Slide 35 / 35 Conclusions Large surveys are hugely increasing the number of eclipsing white dwarf binaries enabling precision parameter studies. These require high time resolution and large apertures to exploit fully. The same studies give precise eclipse times. Almost all eclipsing detached systems show timing anomalies that can be interpreted in terms of planets. It remains to be seen whether this will stand the test of time.
White Dwarfs in Binary Systems
Tom Marsh, Department of Physics, University of Warwick Slide 1 / 39 White Dwarfs in Binary Systems Tom Marsh Department of Physics, University of Warwick Collaborators: Steven Parsons, Madelon Bours,
More informationMonitoring orbital period variations in eclipsing white dwarf binaries
Monitoring orbital period variations in eclipsing white dwarf binaries Madelon Bours Tom Marsh, Steven Parsons Astronomy & Astrophysics Group - University of Warwick - UK RAS Meeting London, January 11,
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 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 informationBoris Gänsicke. Eclipsing binaries, something different. York 2014 To commemorate the 250th anniversary of the birth of John Goodricke
Boris Gänsicke Eclipsing binaries, something different York 2014 To commemorate the 250th anniversary of the birth of John Goodricke John Goodricke White dwarfs Cosmology Eclipsing binaries Masses and
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 informationHelium white dwarfs in binaries
Tom Marsh, Department of Physics, University of Warwick Slide 1 / 20 Helium white dwarfs in binaries Tom Marsh Department of Physics, University of Warwick WD0957-666 Outline Tom Marsh, Department of Physics,
More informationThe Hertzprung-Russell Diagram. The Hertzprung-Russell Diagram. Question
Key Concepts: Lecture 21: Measuring the properties of stars (cont.) The Hertzsprung-Russell (HR) Diagram (L versus T) The Hertzprung-Russell Diagram The Stefan-Boltzmann Law: flux emitted by a black body
More informationPlanetary Nebulae evolve to White Dwarf Stars
Planetary Nebulae evolve to White Dwarf Stars Planetary Nebulae When Red Giant exhausts its He fuel the C core contracts Low & medium-mass stars don t have enough gravitational energy to heat to core 6
More informationPoS(SSC2015)051. Multi-tomography of polars from SALT spectroscopy
from SALT spectroscopy Stephen B. Potter 1 South African Astronomical Observatory Cape Town, South Africa E-mail: sbp@saao.ac.za Enrico J. Kotze South African Astronomical Observatory and Astrophysics,
More informationHR Diagram, Star Clusters, and Stellar Evolution
Ay 1 Lecture 9 M7 ESO HR Diagram, Star Clusters, and Stellar Evolution 9.1 The HR Diagram Stellar Spectral Types Temperature L T Y The Hertzsprung-Russel (HR) Diagram It is a plot of stellar luminosity
More informationAstronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes
Astronomy Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes are hot, compact stars whose mass is comparable to the Sun's and size to the Earth's. A. White dwarfs B. Neutron stars
More informationSupernova events and neutron stars
Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly
More informationDetermining the Orbital Period of the Cataclysmic Variable CSS1204 Using Data from the Vatican Advanced Technology Telescope
Determining the Orbital Period of the Cataclysmic Variable CSS1204 Using Data from the Vatican Advanced Technology Telescope Amy Applegate 2012 NSF/REU Program Physics Department, University of Notre Dame
More informationLecture 21 Formation of Stars November 15, 2017
Lecture 21 Formation of Stars November 15, 2017 1 2 Birth of Stars Stars originally condense out of a COLD, interstellar cloud composed of H and He + trace elements. cloud breaks into clumps (gravity)
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 informationThe Stellar Graveyard Neutron Stars & White Dwarfs
The Stellar Graveyard Neutron Stars & White Dwarfs White Dwarfs White dwarfs are the remaining cores of low-mass (M < 8M sun ) stars Electron degeneracy pressure supports them against gravity Density ~
More informationDr G. I. Ogilvie Lent Term 2005 INTRODUCTION
Accretion Discs Mathematical Tripos, Part III Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION 0.1. Accretion If a particle of mass m falls from infinity and comes to rest on the surface of a star of mass
More informationThe Bizarre Stellar Graveyard
The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White dwarfs
More informationObserved Properties of Stars - 2 ASTR 2120 Sarazin
Observed Properties of Stars - 2 ASTR 2120 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Hipparchus 1) Classified stars by brightness,
More informationCredit: NASA/Kepler Mission/Dana Berry. Exoplanets
Credit: NASA/Kepler Mission/Dana Berry Exoplanets Outline What is an exoplanet? Why are they interesting? How can we find them? Exolife?? The future... Jon Thaler Exoplanets 2 What is an Exoplanet? Most
More informationStar Formation. Stellar Birth
Star Formation Lecture 12 Stellar Birth Since stars don t live forever, then they must be born somewhere and at some time in the past. How does this happen? And when stars are born, so are planets! 1 Molecular
More informationWhite Dwarf Stars as Probes of Physical and Astrophysical Processes
White Dwarf Stars as Probes of Physical and Astrophysical Processes M I K E M O N T G O M E R Y D E P A R T M E N T O F A S T R O N O M Y, M C D O N A L D O B S E R V A T O R Y A N D T H E T E X A S C
More informationSearching for Other Worlds
Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats
More informationFORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
More informationObserved Properties of Stars - 2 ASTR 2110 Sarazin
Observed Properties of Stars - 2 ASTR 2110 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Stellar Colors Stellar Colors Stellar Colors Stars
More informationChapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
More informationAstro 1050 Fri. Apr. 10, 2015
Astro 1050 Fri. Apr. 10, 2015 Today: Continue Ch. 13: Star Stuff Reading in Bennett: For Monday: Finish Chapter 13 Star Stuff Reminders: Ch. 12 HW now on Mastering Astronomy, due Monday. Ch. 13 will be
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 informationKyle Lackey PHYS
Kyle Lackey PHYS 730 9-23-15 Galaxies Large systems of gas, dust, stars, and dark matter orbiting around a common center of mass. We estimate that roughly 185 billion galaxies exist within the observable
More informationHubble Science Briefing: 25 Years of Seeing Stars with the Hubble Space Telescope. March 5, 2015 Dr. Rachel Osten Dr. Alex Fullerton Dr.
Hubble Science Briefing: 25 Years of Seeing Stars with the Hubble Space Telescope March 5, 2015 Dr. Rachel Osten Dr. Alex Fullerton Dr. Jay Anderson Hubble s Insight into the Lives of Stars Comes From:
More informationNames: Team: Team Number:
Astronomy C Michigan Region 8 March 11, 2017 Names: Team: Team Number: Directions 1. There is a separate answer sheet. Answers written elsewhere (e.g. on the test) will not be considered. 2. You may take
More informationHD Transits HST/STIS First Transiting Exo-Planet. Exoplanet Discovery Methods. Paper Due Tue, Feb 23. (4) Transits. Transits.
Paper Due Tue, Feb 23 Exoplanet Discovery Methods (1) Direct imaging (2) Astrometry position (3) Radial velocity velocity Seager & Mallen-Ornelas 2003 ApJ 585, 1038. "A Unique Solution of Planet and Star
More informationChapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves
Chapter 23: Dark Matter, Dark Energy & Future of the Universe Galactic rotation curves Orbital speed as a function of distance from the center: rotation_of_spiral_galaxy.htm Use Kepler s Third Law to get
More information18. 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 informationThe Nature of Pulsars! Agenda for Ast 309N, Nov. 1. To See or Not to See (a Pulsar) The Slowing & Fading of Pulsars!
Agenda for Ast 309N, Nov. 1 Quiz 7 Card 10/30 feedback More on pulsars and other neutron stars Begin: the saga of interacting binary systems Card: questions for review Reading: - Kaler, ch. 7 Wheeler,
More informationASTR Midterm 1 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 1 Phil Armitage, Bruce Ferguson FIRST MID-TERM EXAM FEBRUARY 16 th 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More informationthe nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes
the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes The spectral lines of stars tell us their approximate composition Remember last year in Physics?
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 informationAstr 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 informationAccording to the currents models of stellar life cycle, our sun will eventually become a. Chapter 34: Cosmology. Cosmology: How the Universe Works
Chapter 34: Cosmology According to the currents models of stellar life cycle, our sun will eventually become a a) Cloud of hydrogen gas b) Protostar c) Neutron star d) Black hole e) White dwarf id you
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Final Exam
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Physics 8.282J EAPS 12.402J May 20, 2005 Final Exam Name Last First (please print) 1. Do any
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 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 informationBasic Properties of the Stars
Basic Properties of the Stars The Sun-centered model of the solar system laid out by Copernicus in De Revolutionibus (1543) made a very specific prediction: that the nearby stars should exhibit parallax
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 informationNeutron Stars. But what happens to the super-dense core? It faces two possible fates:
Neutron Stars When a massive star runs out of fuel, its core collapses from the size of the Earth to a compact ball of neutrons just ten miles or so across. Material just outside the core falls onto this
More information10/16/ Detecting Planets Around Other Stars. Chapter 10: Other Planetary Systems The New Science of Distant Worlds
10/16/17 Lecture Outline 10.1 Detecting Planets Around Other Stars Chapter 10: Other Planetary Systems The New Science of Distant Worlds Our goals for learning: How do we detect planets around other stars?
More information27.1: Characteristics of Stars
27.1: Characteristics of Stars STAR NOTES: Part 1 What is a Star? A body of gases that gives off energy in the form of light and heat. 27.1: Characteristics of Stars Are all stars the same? No 1. Stars
More informationBinary Evolution Novae, Supernovae, and X-ray Sources
Binary Evolution Novae, Supernovae, and X-ray Sources The Algol Mystery Algol is a double-lined eclipsing binary system with a period of about 3 days (very short). The two stars are: Star A: B8, 3.4M o
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 informationPage # Astronomical Distances. Lecture 2. Astronomical Distances. Cosmic Distance Ladder. Distance Methods. Size of Earth
Size of Astronomical istances ecture 2 Astronomical istances istance to the Moon (1 sec) istance to the Sun (8 min) istance to other stars (years) istance to centre of our Galaxy ( 30,000 yr to centre)
More informationOne of a kind: A radio pulsing white dwarf binary star
One of a kind: A radio pulsing white dwarf binary star Dr. F.-J. (Josch) Hambsch VVS, BAV, AAVSO, GEOS Introduction White dwarfs are compact stars, similar in size to Earth but 200000 times more massive
More informationActive Galaxies & Quasars
Active Galaxies & Quasars Normal Galaxy Active Galaxy Galactic Nuclei Bright Active Galaxy NGC 5548 Galaxy Nucleus: Exact center of a galaxy and its immediate surroundings. If a spiral galaxy, it is the
More information1. (15.1) What are the approximate mass and radius of a white dwarf compared with those of the Sun?
SUMMARY White dwarfs, neutron stars, and black holes are the remnants of dead stars. A white dwarf forms when a low mass star expels its outer layers to form a planetary nebula shell and leaves its hot
More informationFate of Stars. relative to Sun s mass
INITIAL MASS relative to Sun s mass M < 0.01 Fate of Stars Final State planet.01 < M
More informationCenters of Galaxies. = Black Holes and Quasars
Centers of Galaxies = Black Holes and Quasars Models of Nature: Kepler Newton Einstein (Special Relativity) Einstein (General Relativity) Motions under influence of gravity [23] Kepler The planets move
More informationChapter 9. Stars. The Hertzsprung-Russell Diagram. Topics for Today s Class. Phys1411 Introductory Astronomy Instructor: Dr.
Foundations of Astronomy 13e Seeds Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 9 Stars Cengage Learning 2016 Topics for Today s Class HR Diagram Variable Stars Intrinsic Variables Cepheids
More informationThe Gravitational Microlensing Planet Search Technique from Space
The Gravitational Microlensing Planet Search Technique from Space David Bennett & Sun Hong Rhie (University of Notre Dame) Abstract: Gravitational microlensing is the only known extra-solar planet search
More informationIntroduction to SDSS -instruments, survey strategy, etc
Introduction to SDSS -instruments, survey strategy, etc (materials from http://www.sdss.org/) Shan Huang 17 February 2010 Survey type Status Imaging and Spectroscopy Basic Facts SDSS-II completed, SDSS-III
More informationChapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc.
Chapter 16 Lecture The Cosmic Perspective Seventh Edition Star Birth 2014 Pearson Education, Inc. Star Birth The dust and gas between the star in our galaxy is referred to as the Interstellar medium (ISM).
More informationChapter 14: The Bizarre Stellar Graveyard
Lecture Outline Chapter 14: The Bizarre Stellar Graveyard 14.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf?
More informationSubaru telescope observes echo of the exploding star first seen in 1572, and reveals its nature
Institute for the Physics and Mathematics of the Universe IPMU Press Release 2008 12 04 Subaru telescope observes echo of the exploding star first seen in 1572, and reveals its nature Kashiwa, Japan A
More informationEvolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
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 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 informationThe 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 informationCompton Lecture #4: Massive Stars and. Supernovae. Welcome! On the back table:
Compton Lecture #4: Massive Stars and Welcome! On the back table: Supernovae Lecture notes for today s s lecture Extra copies of last week s s are on the back table Sign-up sheets please fill one out only
More informationOur Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.
Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.
More informationNeutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is
More information21. Neutron Stars. The Crab Pulsar: On & Off. Intensity Variations of a Pulsar
21. Neutron Stars Neutron stars were proposed in the 1930 s Pulsars were discovered in the 1960 s Pulsars are rapidly rotating neutron stars Pulsars slow down as they age Neutron stars are superfluid &
More informationChapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard 18.1 White Dwarfs What is a white dwarf? What can happen to a white dwarf in a close binary system? What supports
More informationPart 3: The Dark Energy
Part 3: The Dark Energy What is the fate of the Universe? What is the fate of the Universe? Copyright 2004 Pearson Education, published as Addison Weasley. 1 Fate of the Universe can be determined from
More informationObjectives. HR Diagram
Objectives HR Diagram Questions from Yesterday Centripetal Force perpendicular to the rotation axis Acts to slow down collapse Strongest 90 deg from rotation axis Particles with an angle < 90 feel the
More informationThe Family of Stars. Chapter 13. Triangulation. Trigonometric Parallax. Calculating Distance Using Parallax. Calculating Distance Using Parallax
The Family of Stars Chapter 13 Measuring the Properties of Stars 1 Those tiny glints of light in the night sky are in reality huge, dazzling balls of gas, many of which are vastly larger and brighter than
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 informationChapter 21 Galaxy Evolution. How do we observe the life histories of galaxies?
Chapter 21 Galaxy Evolution How do we observe the life histories of galaxies? Deep observations show us very distant galaxies as they were much earlier in time (old light from young galaxies). 1 Observing
More informationLecture 25: Cosmology: The end of the Universe, Dark Matter, and Dark Energy. Astronomy 111 Wednesday November 29, 2017
Lecture 25: Cosmology: The end of the Universe, Dark Matter, and Dark Energy Astronomy 111 Wednesday November 29, 2017 Reminders Online homework #11 due Monday at 3pm One more lecture after today Monday
More informationFundamental (Sub)stellar Parameters: Masses and Radii. PHY 688, Lecture 10
Fundamental (Sub)stellar Parameters: Masses and Radii PHY 688, Lecture 10 Outline Review of previous lecture brown dwarf effective temperatures finding cool brown dwarfs current problem: what are the coolest
More informationMeasuring Radial & Tangential Velocity. Radial velocity measurement. Tangential velocity measurement. Measure the star s Doppler shift
17. The Nature of the Stars Parallax reveals stellar distance Stellar distance reveals luminosity Luminosity reveals total energy production The stellar magnitude scale Surface temperature determines stellar
More informationSpecial Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers.
Black Holes Special Relativity Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. 2. The speed of light is the same for all inertial observers regardless
More informationPosition 1 Position 2 6 after position 1 Distance between positions 1 and 2 is the Bigger = bigger parallax (Ɵ)
STARS CHAPTER 10.1 the solar neighborhood The distances to the nearest stars can be measured using Parallax => the shift of an object relative to some distant background as the observer s point of view
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 information8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars
Classifying Stars In the early 1900s, Ejnar Hertzsprung and Henry Russell made some important observations. They noticed that, in general, stars with higher temperatures also have brighter absolute magnitudes.
More informationBinary Evolution Novae, Supernovae, and X-ray Sources
Binary Evolution Novae, Supernovae, and X-ray Sources http://apod.nasa.gov/apod/ http://www.space.com/32150-farthest-galaxy-smashes-cosmic-distance-record.html The Algol Mystery Algol is a double-lined
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 information7. BINARY STARS (ZG: 12; CO: 7, 17)
7. BINARY STARS (ZG: 12; CO: 7, 17) most stars are members of binary systems or multiple systems (triples, quadruples, quintuplets,...) orbital period distribution: P orb = 11 min to 10 6 yr the majority
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 informationAy 1 Midterm. Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA
Ay 1 Midterm Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA You have THREE HOURS to complete the exam, but it is about two hours long. The
More informationSpectroscopy, the Doppler Shift and Masses of Binary Stars
Doppler Shift At each point the emitter is at the center of a circular wavefront extending out from its present location. Spectroscopy, the Doppler Shift and Masses of Binary Stars http://apod.nasa.gov/apod/astropix.html
More informationAST 2010: Descriptive Astronomy EXAM 2 March 3, 2014
AST 2010: Descriptive Astronomy EXAM 2 March 3, 2014 DO NOT open the exam until instructed to. Please read through the instructions below and fill out your details on the Scantron form. Instructions 1.
More informationThe Milky Way & Galaxies
The Milky Way & Galaxies The Milky Way Appears as a milky band of light across the sky A small telescope reveals that it is composed of many stars (Galileo again!) Our knowledge of the Milky Way comes
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 informationOur 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 informationBasics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances
Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers
More informationObserving the Night Sky. Observing the Night Sky. Observing the Night Sky. Observing the Night Sky. Observing the Night Sky. Chapter 29 THE UNIVERSE
Hewitt/Lyons/Suchocki/Yeh Conceptual Integrated Science Constellations are groups of stars named over antiquity. A familiar constellation is Ursa Major, the Great Bear. Chapter 29 THE UNIVERSE The monthly
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 informationWhite dwarf populations. Gijs Nelemans Radboud University Nijmegen
White dwarf populations Gijs Nelemans Radboud University Nijmegen Outline Introduction: Population synthesis Basic ingredients Observational inputs White dwarf populations Different types and mergers WD
More information