Pulsars are Cool. Seriously. Scott Ransom National Radio Astronomy Observatory / University of Virginia
|
|
- Drusilla Cole
- 6 years ago
- Views:
Transcription
1 Pulsars are Cool. Seriously. Scott Ransom National Radio Astronomy Observatory / University of Virginia
2 Neutron Stars Spin rates up to 716 Hz Solar masses km radii Central densities several times nuclear Surface temp ~106 K Luminosity up to 10,000x the Sun's! Detailed emission mechanisms unknown Surface gravity ~1011 times Earth's Magnetic field (Gauss): Millisecond: Normal : Magnetar:
3 Neutron Stars Spin rates up to 716 Hz Solar masses km radii Central densities several times nuclear Detailed emission mechanisms unknown Surface gravity ~1011 times Earth's These are exotic objects Surface temp ~106 K Luminosity up to 10,000x the Sun's! Magnetic field (Gauss): Millisecond: Normal : Magnetar:
4 The Discovery of Pulsars PhD student Jocelyn Bell and Prof. Antony Hewish Initially Little Green Men Hewish won Nobel Prize in 1974
5 What are their radio properties? Continuum sources Typically somewhat to highly linearly polarized Steep radio spectra (index of -1 to -3, typical obs freqs GHz) Point sources Special ISM effects (freq dependent) Highly time variable Wide variety of timescales Very faint average flux density ~mjy
6 Confusion? None for pulsars! Pulsars separated via time (or spin frequency!) rather than spatially. Gain variations? Who cares?! Observations are continually on and off source. Large beam? Doesn't matter! Sub-arcsec positions come from pulsar timing. Timing solns for 33 Ter5 MSPs (VLA contours in green)
7 Fundamental Physics with Pulsars Gravitational wave detection (e.g. high precision timing) Physics at nuclear density (e.g. neutron star interiors) Strong-field gravity tests (e.g. binary pulsar dynamics) Also many others: Plasma physics (e.g. magnetospheres, pulsar eclipses) Astrophysics (e.g. stellar masses and evolution) Fluid dynamics (e.g. supernovae collapse) Magnetohydrodynamics (e.g. pulsar winds) Relativistic electrodynamics (e.g. pulsar magnetospheres) Atomic physics (e.g. NS atmospheres) Solid state physics (e.g. NS crust properties)
8 Basic Physical Information from Pulsars Rotating dipole magnet in a vacuum (I = 1045 g cm2): radiates energy and therefore spins-down (p-dot) Surface magnetic field strength (B) Spin-down luminosity (E-dot) Age (T) and Characteristic Age ( c) (braking index: n ~ 3)
9 P-Pdot Diagram Pulsar HertzsprungRussell Diagram HR Diagram: Temp (color) vs Luminosity P-Pdot Diagram Period vs Spindown rate
10 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Old Low B
11 Crab Nebula SN1054AD Pulsar rotates 30 times per second! Anasazi Indian cave pictogram, Chaco Canyon, NM
12 The Crab is visible at all energies! Red = Radio Green = Optical Blue = X-ray
13 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Pulsars move down and right across the diagram as they lose energy (assuming that the magnetic field doesn't change...) Old Low B
14 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Normal (average B, slow spin) Old Low B
15 Science with normal pulsars Used to: study the unknown pulsar emission mechanism probe the interstellar medium (scattering, scintillation, rotation measures, electron distribution) Scintillation Walker et al 2008 Measure PSR distances (HI absorption) Drifting Sub-pulses Bhattacharyya et al 2007
16 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Normal (average B, slow spin) Eventually they slow down so much that there is not enough spin to generate the electric fields which produce emission. Low B Their lifetimes are Myrs. Old
17 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Normal (average B, slow spin) Old Millisecond (low B, very fast, very old, very stable spin, best for basic physics tests) Low B
18 1982: Enigmatic bright, steep-spectrum, polarized, and scintillating radio source... Using Arecibo: 1.558ms pulsar (640 Hz)! (6 pulses) 21x faster than Crab! ~half an octave above Concert A! Courtesy Bob Rood
19 Millisecond Pulsars: via Recycling Supernova produces a neutron star Red Giant transfers matter to neutron star Alpar et al 1982 Radhakrishnan & Srinivasan 1984 Millisecond Pulsar emerges with a white dwarf companion Picture credits: Bill Saxton, NRAO/AUI/NSF
20 Pulsar Flavors Young High B Young (high B, fast spin, very energetic) Normal (average B, slow spin) ng! Old (low B, very fast, very old, very stable spin, best for basic physics tests) Re cy cli Millisecond Low B
21 The Primary Pulsar Telescopes Arecibo GBT Parkes Jodrell Bank
22 New All-Sky Pulsar Surveys All major radio telescopes are conducting all-sky pulsar surveys We know of only about 5% of the total pulsars in the Galaxy! Generate lots of data (~50MB/s!): 1000s of hrs, 1000s of channels, khz sampling: Green Bank Telescope gives more than a Petabyte! Requires huge amounts of high performance computing Processing 2 min of GBT data requires 2 days on a fast CPU! Millions of false positives
23 Dispersion Lower frequency radio waves are delayed with respect to higher frequency radio waves by the ionized interstellar medium t DM -2 High Freq Low Freq (DM = Dispersion Measure) Coherent Dedispersion exactly removes this effect, but is very computationally difficult
24 Scattering and Pulse Broadening -4.4 Multipath propagation causes frequency dependent pulse broadening.
25 Searching for New Pulsars Pulsars are: Very weak radio sources Binary pulsars show Doppler effects Often distant (therefore weaker and high DM) Predominantly found in the Galactic Plane (ISM effects) Sensitivity (A /Ttot) (tint BW)1/2 Computations Fspin3 tint2 Solutions: Use large telescopes and sensitive receivers Use longer integration times Use advanced algorithms to adaptively remove interference Use advanced algorithms to optimize sensitivity to weak binary MSPs (the hardest PSRs to detect)
26 Basic Radio Pulsar Search Recipe Step (% of CPU Time) 1. Interference identification and removal (1%) 2. De-dispersion of the raw data (5%) 3. Normal FFT search (slow pulsars) (15%) 4. Acceleration search (binary MSPs) (60%) 5. Single-pulse search (15%) 6. Sifting of candidates (<1%) 7. Folding of candidates (3%) Processing a single ~2-min pointing takes ~2 days! Big surveys have ~105 pointings, therefore 5+ CPU centuries!
27 Ter5 A (4th harm) Ter5 N (3rd harm)
28 Single Pulse Searches Some pulsars have highly variable pulse amplitudes or shut off completely (i.e. nulling) RRATs Look for dispersed individual pulses (e.g. McLaughlin & Cordes, 2003, ApJ, 596, 982) New PALFA Pulsar J
29 New Millisecond Pulsars Numbers have: quadrupled in last 10 yrs doubled in last ~3 years Why? Rise in computing capability, sensitive new radio surveys, Fermi! Year
30 Currently ~70 new Radio/gamma-ray MSPs because of Fermi! ~10% of them look like they will be good timers Courtesy: Paul Ray
31 Millisecond Pulsars are Very Precise Clocks PSR J At 12:40PM PST February : P = ms +/ ms The last digit changes by 1 every 2 minutes! This digit changes by 1 every ~4000 years! This extreme precision is what allows us to use pulsars as tools to do unique physics!
32 Pulsar Timing: Unambiguously account for every rotation of a pulsar over years Pulse Measurements (TOAs: Times of Arrival) Observation 1 Obs 2 Pulses Model (prediction) Obs 3 Time Measurement - Model = Timing Residuals Single day at telescope Time in days Predict each pulse to ~200 ns over 2 yrs!
33 Does it work? PSR J ~3yrs of Fermi gamma-ray data ~3000 photons (~3/day) ~560 binary orbits ~24 billion rotations of MSP Perfectly lined up from radio pulsar timing 2 Pulse Rotations
34
35 Demorest et al. 2010, Nature
36 Ask the right question... Highly circular orbit has a radius of ~3.4 million km (~5 x Solar radius or ~9 x Earth-Moon distance)...get a spectacular answer! The measured difference between the semi-major and semi-minor axes is: 2.8 +/- 0.2 mm! Demorest et al. 2010, Nature
37 The Binary Pulsar: B First binary pulsar discovered at Arecibo Observatory by Hulse and Taylor in 1974 NS-NS Binary Ppsr = ms Porb = hrs a sin(i)/c = lt-s e = ω = 4.2 deg/yr Mc = (7) M Mp = (7) M
38 Post-Keplerian Orbital Parameters Besides the normal 5 Keplerian parameters (Porb, e, asin(i)/c, T0, ω), General Relativity gives: (Orbital Precession) (Grav redshift + time dilation) (Shapiro delay: range and shape ) where: T GM /c3 = μs, These are only functions of: M = m1 + m2, and s sin(i) - the (precisely!) known Keplerian orbital parameters Pb, e, asin(i) - the mass of the pulsar m1 and the mass of the companion m2
39 Post-Keplerian Orbital Parameters Besides the normal 5 Keplerian parameters (Porb, e, asin(i)/c, T0, ω), General Relativity gives: Need eccentric orbit and time for precession (Orbital Precession) (Grav redshift + time dilation) Need compact orbit and a lot of patience Need high precision, Inclination, and m2 (Shapiro delay: range and shape ) where: T GM /c3 = μs, These are only functions of: M = m1 + m2, and s sin(i) - the (precisely!) known Keplerian orbital parameters Pb, e, asin(i) - the mass of the pulsar m1 and the mass of the companion m2
40 The Binary Pulsar: B Three Relativistic Observables: ω, γ, Porb Indirect detection of Gravitational Radiation In 1993, Russell Hulse and Joseph Taylor were awarded the Nobel Prize for their work on PSR B ! From Weisberg & Taylor, 2003
41 The Double Pulsar: J Faster spin, more compact orbit, edge on system, 6 relativistic observables, 2 pulsars! Overall, much better than HulseTaylor binary PSR. Currently GR tests to ~0.01%! Measured vs Predicted Relativistic Shapiro Delay Kramer et al., 2006, Science, 314, 97
42 Shapiro Delay NRAO / Bill Saxton Irwin Shapiro 1964 Shapiro et al. 1968, 1971
43 J : Incredible Shapiro Delay Signal Full Shapiro Signal No General Relativity Mwd = 0.500(6) M Mpsr = 1.97(4) M! Inclination = 89.17(2) deg! Full Relativistic Solution Demorest et al. 2010, Nature, 467, 1081D see Ozel et al. 2010, ApJL, 724, 1990
44 An MSP in a Triple Stellar System Recently with GBT: a stellar triple system!
45
46 Direct Gravitational Wave Detection (Pulsar Timing Array) Looking for nhz freq gravitational waves from super massive black hole binaries Need good MSPs: Significance scales with the number of MSPs being timed Must time 20+ pulsars for 10+ years at precision of ~100 nanosec! Bill Saxton (NRAO/AUI) For more information, see nanograv.org Australia Europe North America
47 Where do these GWs come from? Coalescing Super-Massive Black Holes Basically all galaxies have them Masses of Solar Masses Galaxy mergers lead to black hole mergers When BHs within 1pc, GWs are main energy loss For nearby very massive binaries, we can get 10s of nano-second timing residuals Potentially measurable with a single MSP, but much better using an array of MSPs.
48 What about the future? We only know of about 2,000 out of ~50,000+ pulsars in the Galaxy! Many of them will be Holy Grails Sub-MSP, PSR-Black Hole systems, MSP-MSP binary Several new huge telescopes... We need them because we are sensitivity limited! MeerKAT (64 dishes, SA) FAST (500m, China))
49
50 Summary Pulsars are Cool. Seriously.
Pulsars and Radio Transients. Scott Ransom National Radio Astronomy Observatory / University of Virginia
Pulsars and Radio Transients Scott Ransom National Radio Astronomy Observatory / University of Virginia TIARA Summer School on Radio Astronomy 2016 Radio Transients Non-thermal emission Emission types
More informationDetecting Gravitational Waves. (and doing other cool physics) with Millisecond Pulsars. NANOGrav. Scott Ransom
Detecting Gravitational Waves (and doing other cool physics) with Millisecond Pulsars NANOGrav Scott Ransom What s a Pulsar? Rotating Neutron Star! Size of city: R ~ 10-20 km Mass greater than Sun: M ~
More informationRecent Results in Pulsars: A Pulsar Renaissance. Scott Ransom
Recent Results in Pulsars: A Pulsar Renaissance Scott Ransom NRAO Charlottesville NAIC/NRAO Single-Dish Summer School 2005 What s a Pulsar? Discovered in 1967 by Jocelyn Bell and Antony Hewish at Cambridge
More informationPulsar Overview. Kevin Stovall NRAO
Pulsar Overview Kevin Stovall NRAO IPTA 2018 Student Workshop, 11 June, 2018 Pulsars Pulsars ~2,700 pulsars known Act as clocks, therefore provide a means for studying a variety of physical phenomena Strongly
More informationNS masses from radio timing: Past, present and future. Paul Demorest (NRAO) Symposium on Neutron Stars, Ohio U., May 2016
NS masses from radio timing: Past, present and future Paul Demorest (NRAO) Symposium on Neutron Stars, Ohio U., May 2016 Overview Review of how to measure neutron star masses via radio pulsar timing. Summary
More informationBut wait! There's More! A wealth of science from millisecond pulsars. Scott Ransom National Radio Astronomy Observatory / University of Virginia
But wait! There's More! A wealth of science from millisecond pulsars Scott Ransom National Radio Astronomy Observatory / University of Virginia What s a Millisecond Pulsar? Rapidly Rotating Neutron Star!
More informationPulsars. in this talk. Pulsar timing. Pulsar timing. Pulsar timing. Pulsar timing. How to listen to what exotic. are telling us! Paulo César C.
How to listen to what exotic Pulsars are telling us! in this talk 1. 2. 3. Test of gravitational theories using binary pulsars 4. Probing the equation of state of super-dense matter Paulo César C. Freire
More informationimin...
Pulsar Timing For a detailed look at pulsar timing and other pulsar observing techniques, see the Handbook of Pulsar Astronomy by Duncan Lorimer and Michael Kramer. Pulsars are intrinsically interesting
More informationThe (obscene) Challenges of Next-Generation Pulsar Surveys
The (obscene) Challenges of Next-Generation Pulsar Surveys Scott Ransom NRAO / Univ. of Virginia Charlottesville, VA Haslam 408MHz Survey Summary: The Pulsar Search Problem Pulsars are faint we are sensitivity
More informationGravity with the SKA
Gravity with the SKA Strong-field tests of gravity using Pulsars and Black Holes Michael Kramer Jodrell Bank Observatory University of Manchester With Don Backer, Jim Cordes, Simon Johnston, Joe Lazio
More informationA Pulsar Timing Array for Gravitational Wave Detection. Paul Demorest, NRAO
A Pulsar Timing Array for Gravitational Wave Detection Paul Demorest, NRAO About 10% of known radio pulsars are recycled millisecond pulsars (MSPs). These are spun up by accreting matter from a companion
More informationProbing Relativistic Gravity with the Double Pulsar
Probing Relativistic Gravity with the Double Pulsar Marta Burgay INAF Osservatorio Astronomico di Cagliari The spin period of the original millisecond pulsar PSR B1937+21: P = 0.0015578064924327 ± 0.0000000000000004
More informationObservations radio de pulsars binaires relativistes a Nancay
Observations radio de pulsars binaires relativistes a Nancay Ismael Cognard icognard@cnrs-orleans.fr LPC2E, CNRS - Universite d'orleans, France Nancay Radio Telescope I.Cognard - Pulsars binaires relativistes
More informationMeasurements of Neutron Star Masses with a strong emphasis on millisecond binary radio pulsar timing
Measurements of Neutron Star Masses with a strong emphasis on millisecond binary radio pulsar timing David Nice, Lafayette College Physics of Neutron Stars 2014, Saint Petersburg 1. Motivation 2. How to
More informationTesting physics with millisecond pulsars. Paul Demorest, NRAO
Testing physics with millisecond pulsars Paul Demorest, NRAO Talk outline: 1. Intro: Neutron stars, millisecond pulsars 2. Digital instrumentation for radio pulsar observations 3. Mass of PSR J1614-2230
More informationRecent Radio Observations of Pulsars
Recent Radio Observations of Pulsars R. N. Manchester Australia Telescope National Facility, CSIRO Sydney Australia Summary A pulsar census Recent pulsar surveys Pulse modulation and drifting subpulses
More informationPulsars. Table of Contents. Introduction
Pulsars Table of Contents Introduction... 1 Discovery...2 Observation...2 Binary Pulsars...3 Pulsar Classes... 3 The Significance of Pulsars... 3 Sources...4 Introduction Pulsars are neutron stars which
More informationTesting Gravity and Extreme Physics with Pulsars
Testing Gravity and Extreme Physics with Pulsars John Rowe Animation Australia Telescope National Facility, CSIRO René Breton School of Physics & Astronomy The University of Manchester Liverpool Physics
More informationPulsar Surveys Present and Future: The Arecibo-PALFA Survey and Projected SKA Survey
Pulsar Surveys Present and Future: The Arecibo-PALFA Survey and Projected SKA Survey Arecibo Telescope SKA concept design Julia Deneva,, Cornell University, USA 15 May 2006 363 rd Heraeus Seminar, Bad
More informationRadio Aspects of the Transient Universe
Radio Aspects of the Transient Universe Time domain science: the transient sky = frontier for all λλ Less so at high energies BATSE, RXTE/ASM, Beppo/Sax, SWIFT, etc. More so for optical, radio LSST = Large
More informationNeutron Stars. Neutron Stars Mass ~ 2.0 M sun! Radius ~ R sun! isolated neutron stars first seen only recently (1997)
Neutron Stars 1 2 M core > 1.4 M - collapse past WD! sun nuclei packed tightly together! protons absorb electrons; only neutrons left! collapse halted by neutron degeneracy pressure How do you find something
More informationThe Neutron Star Zoo. Stephen C.-Y. Ng ( 吳志勇 ) HKU
The Neutron Star Zoo Stephen C.-Y. Ng ( 吳志勇 ) HKU Overview Introduction to neutron stars Different classes of neutron stars: Radio Pulsars MSPs Magnetars DINS CCOs Unification 6/12/2017 NAOC Stephen Ng
More informationPulsars ASTR2110 Sarazin. Crab Pulsar in X-rays
Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other
More informationPaul Demorest (NRAO) for NANOGrav collaboration, CHIME pulsar team John Galt Symposium, DRAO, Sept 23, 2014
Pulsars and CHIME: Gravitational Waves, the ISM and More! Paul Demorest (NRAO) for NANOGrav collaboration, CHIME pulsar team John Galt Symposium, DRAO, Sept 23, 2014 Outline Pulsar stuff: Pulsar timing
More informationMILLISECOND PULSAR POPULATION
MILLISECOND PULSAR POPULATION on Formation and Evolution Of Neutron Stars 11/12/2017 COMPANY NAME Outline 1. Millisecond Pulsars 2.Current Population 3.Applications 4.Future Prospects 4.1.Potential Science
More informationUniversity of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 19.
University of Naples Federico II, Academic Year 2011-2012 Istituzioni di Astrofisica, read by prof. Massimo Capaccioli Lecture 19 Neutron stars Learning outcomes The student will see: xxx Discovery of
More informationIn Search of New MSPs for Pulsar Timing Arrays. Kevin Stovall, NRAO Socorro NANOGrav Collaboration
In Search of New MSPs for Pulsar Timing Arrays Kevin Stovall, NRAO Socorro NANOGrav Collaboration NRAO Postdoc Symposium, March 27, 2017 NANOGrav = US/Canada-based collaboration working to detect nhz GW
More informationThe Eight-meter-wavelength Transient Array
The Eight-meter-wavelength Transient Array Steve Ellingson Cameron Patterson John Simonetti Dept. of Electrical & Computer Engineering Dept. of Electrical & Computer Engineering Dept. of Physics Virginia
More informationBinary Pulsars and Evidence for Gravitational Radiation
Binary Pulsars and Evidence for Gravitational Radiation Matthew S. Paoletti Physics 798G March 29, 2007 http://www.rowes.com.au/csiro.htm Motivation Three classical tests of GR Bending of light as it passes
More informationBinary Pulsars and Evidence for Gravitational Radiation
Binary Pulsars and Evidence for Gravitational Radiation Matthew S. Paoletti Institute for Research in Electronics and Applied Physics Energy Research Facility, Bldg. #3 University of Maryland College Park,
More informationNew Radio Millisecond Pulsars in Fermi (formerly) Unassociated Sources
New Radio Millisecond Pulsars in Fermi (formerly) Unassociated Sources Scott Ransom (NRAO) For the Fermi Pulsar Search Consortium (PSC) Fermi Pulsars Currently 24 blind search pulsars (16 in Sci) Currently
More informationAstronomy 421. Lecture 23: End states of stars - Neutron stars
Astronomy 421 Lecture 23: End states of stars - Neutron stars 1 Outline Neutron stars Pulsars properties distribution emission mechanism evolution 2 Neutron stars Typical values: M ~ 1.4M R ~ 10 km ρ ~
More informationGravity Tests with Radio Pulsars
Gravity Tests with Radio Pulsars Norbert Wex Paris, June 21 st, 2010 Regimes of Gravity Tests (1) Quasi-stationary weak-field regime Solar system experiments (2) Quasi-stationary strong-field regime (3)
More informationETA Observations of Crab Pulsar Giant Pulses
ETA Observations of Crab Pulsar Giant Pulses John Simonetti,, Dept of Physics, Virginia Tech October 7, 2005 Pulsars Crab Pulsar Crab Giant Pulses Observing Pulses --- Propagation Effects Summary Pulsars
More informationTesting General Relativity using the Square Kilometre Array
Testing General Relativity using the Square Kilometre Array Willem van Straten Institute for Radio Astronomy & Space Research Auckland University of Technology Self-consistent but incomplete Baryon asymmetry
More informationRadio Searches for Pulsars in the Galactic Center
Radio Searches for Pulsars in the Galactic Center J.Deneva (GMU, resident at NRL), P.Ray (NRL), S.Hyman (SBC), D.Frail (NRAO), N.Kassim (NRL), M. Kerr (NRL), J.Lazio (JPL) Outline Motivation. Types of
More informationPulsars - a new tool for astronomy and physics
1 Reading: Chapter 24, Sect. 24.5-24.6; Chap. 20, Chap. 25, Sec. 25.1 Exam 2: Thursday, March 22; essay question given on Tuesday, March 20 Last time:death of massive stars - supernovae & neutron stars
More informationTeV Emission from Millisecond Pulsars in Compact Binaries? Mallory Roberts Eureka Scientific/NRL
TeV Emission from Millisecond Pulsars in Compact Binaries? Mallory Roberts Eureka Scientific/NRL Binary Period in Days Millisecond Pulsars Spun up by a low mass companion such that their spin period P
More informationInvestigating Emission Mechanisms by Mapping Pulsar Magnetospheres in 3D
Investigating Emission Mechanisms by Mapping Pulsar Magnetospheres in 3D Candidacy Presentation, 22 Aug 2016 Sam McSweeney Supervisors: Ramesh Bhat Steven Tremblay Avinash Deshpande Trying to figure out
More informationTesting General Relativity with Relativistic Binary Pulsars
Testing General Relativity with Relativistic Binary Pulsars Ingrid Stairs UBC GWPAW Milwaukee Jan. 29, 2011 Green Bank Telescope Jodrell Bank Parkes Arecibo Outline Intro to pulsar timing Equivalence principle
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 informationAstronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 22 Neutron Stars and Black Holes MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) In a neutron star, the core
More informationNext Texas Meeting December It s warm in December! In Melbourne. See kangaroos & koalas Swim at Barrier Reef Exciting science
Next Texas Meeting December 2006 In Melbourne It s warm in December! See kangaroos & koalas Swim at Barrier Reef Exciting science Millisecond Pulsars and Gravity R. N. Manchester Australia Telescope National
More informationLecture Outlines. Chapter 22. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 22 Astronomy Today 8th Edition Chaisson/McMillan Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 Neutron-Star Binaries 22.4 Gamma-Ray
More informationNeutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star.
Neutron Stars Neutron Stars The emission from the supernova that produced the crab nebula was observed in 1054 AD by Chinese, Japanese, Native Americans, and Persian/Arab astronomers as being bright enough
More informationPulsars. 1967, Cambridge. S. Jocelyn Bell Burnell
Pulsars 1967, Cambridge S. Jocelyn Bell Burnell Nature 217, 709-713 (24 February 1968) Observation of a Rapidly Pulsating Radio Source A. HEWISH, S. J. BELL, J. D. H. PILKINGTON, P. F. SCOTT & R. A. COLLINS
More informationFinal States of a Star
Pulsars Final States of a Star 1. White Dwarf If initial star mass < 8 MSun or so. (and remember: Maximum WD mass is 1.4 MSun, radius is about that of the Earth) 2. Neutron Star If initial mass > 8 MSun
More informationPulsar Observation and Data Analysis Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science
Credit: John Sarkissian Pulsar Observation and Data Analysis Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science Outline What are pulsars? What are the requirements for instrumentation/observing
More informationMass 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 informationNeutron Stars. Melissa Louie
Neutron Stars Melissa Louie 11-08-10 Outline History, Formation, Properties Detection Pulsars Crab Nebula Pulsar Pulsar Timing Pulsars in Binary Systems Isolated Neutron Stars J185635-3754 Summary 2 The
More informationCompact Binaries - 3 ASTR2110 Sarazin
Compact Binaries - 3 ASTR2110 Sarazin Zoology of Binary Stars X-ray Binary Pulsar Spin-Up Accreted material has high angular momentum Spins up neutron star (true of ~all X-ray binary pulsars) Millisecond
More informationSKADS Virtual Telescope: Pulsar Survey IV: Globular Cluster Pulsars
SKADS Virtual Telescope: Pulsar Survey IV: Globular Cluster Pulsars PI: S. Ransom Co-I: M. Kramer We propose to use the SKADS Virtual Telescope (SVT) to search Globular clusters for fast rotating pulsars
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 informationStellar remnants II. Neutron Stars 10/18/2010. (progenitor star 1.4 < M< 3 Msun) Stars, Galaxies & the Universe Announcements
Stars, Galaxies & the Universe Announcements Exam #2 on Wednesday Review sheet and study guide posted by Thursday Use office hours and Astronomy Tutorial hours Covers material since Exam #1 (plus background
More informationMillisecond X-ray pulsars: 10 years of progress. Maurizio Falanga
Millisecond X-ray pulsars: 10 years of progress Maurizio Falanga History I Radio Astronomy in the 30 s-60 s Karl Jansky 1933 3C273 Discovery (1961-63) Quasi-Stellar Radio Sources as the most energetic
More informationPulsar Astronomy with GLAST Steve Thorsett UC Santa Cruz GLAST
Pulsar Astronomy with Steve Thorsett UC Santa Cruz Discovery of Neutron Stars: Pulsars In 1967, Jocelyn Bell discovered a strange, pulsating radio source (dubbed LGM 1) http://www.ggw.org/asras/ snimages/
More informationThe Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar
The Mystery of Fast Radio Bursts and its possible resolution Outline Pawan Kumar FRBs: summary of relevant observations Radiation mechanism and polarization FRB cosmology Wenbin Lu Niels Bohr Institute,
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 informationPulsars. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Pulsars 1/43
Pulsars D.Maino Physics Dept., University of Milano Radio Astronomy II D.Maino Pulsars 1/43 Pulsar Properties Pulsars are magnetized neutron stars emitting periodic, short pulses at radio wavelenghts with
More informationFermi Large Area Telescope:
Fermi Large Area Telescope: Early Results on Pulsars Kent Wood Naval Research Lab kent.wood@nrl.navy.mil for the Fermi LAT Collaboration Tokyo Institute of Technology 7 March 2009 K. Wood (NRL) 1/30 Fermi
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 The Bizarre Stellar Graveyard
Chapter 18 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
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 informationarxiv:astro-ph/ v1 10 Nov 1999
Pulsar Astronomy 2000 and Beyond ASP Conference Series, Vol. e iπ + 1, 2000 M. Kramer, N. Wex, and R. Wielebinski, eds. The Parkes Multibeam Pulsar Survey arxiv:astro-ph/9911185v1 10 Nov 1999 F. Camilo
More informationDetecting Gravitational Waves with Pulsars
Detecting Gravitational Waves with Pulsars R. N. Manchester Australia Telescope National Facility, CSIRO, Sydney Australia Summary Pulsars and pulsar timing Parkes pulsar surveys the double pulsar The
More informationASTR 200 : Lecture 20. Neutron stars
ASTR 200 : Lecture 20 Neutron stars 1 Equation of state: Degenerate matter We saw that electrons exert a `quantum mechanical' pressure. This is because they are 'fermions' and are not allowed to occupy
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 informationProbing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era
Utah State University DigitalCommons@USU Colloquia and Seminars Astrophysics 9-7-2011 Probing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era Shane L. Larson Utah
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 informationASTR Midterm 2 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 2 Phil Armitage, Bruce Ferguson SECOND MID-TERM EXAM MARCH 21 st 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More informationChapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter
13.1 Neutron Stars Lecture Outline Chapter 13 Neutron Stars and After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is
More informationChapter 33 The History of a Star. Introduction. Radio telescopes allow us to look into the center of the galaxy. The milky way
Chapter 33 The History of a Star Introduction Did you read chapter 33 before coming to class? A. Yes B. No You can see about 10,000 stars with the naked eye. The milky way Radio telescopes allow us to
More informationThe Double Pulsar:! A Decade of Discovery! (and what you can do over the next decade with FAST!)
The Double Pulsar:! A Decade of Discovery! (and what you can do over the next decade with FAST!) Maura McLaughlin West Virginia University 20 May 2014 : Double neutron star systems" The pulsar catalog
More informationThe Hunt for New Pulsars with the Green Bank Telescope
The Hunt for New Pulsars with the Green Bank Telescope Ryan Lynch Postdoctoral Fellow McGill University What we'll talk about... Two most recent large-area GBT pulsar surveys the 350 MHz Drift Scan Survey
More informationScience with Radio Pulsar Astrometry
Science with Radio Pulsar Astrometry Shami Chatterjee Cornell University August 2012 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrometry is
More informationMILLISECOND PULSARS. Merve Çolak
MILLISECOND PULSARS Merve Çolak OUTLINE Corbet Diagram (again) P-P(dot) Diagram MSPs and Their History Properties of MSPs Spin-up of Neutron Stars Spin-down of MSPs MSP Evolution Recent MSP Evolution Model
More informationDetection of Gravitational Waves with Pulsar Timing
Detection of Gravitational Waves with Pulsar Timing R. N. Manchester Australia Telescope National Facility, CSIRO Sydney Australia Summary Detection of gravitational waves Pulsar Timing Array (PTA) projects
More informationGeneral Relativity Tests with Pulsars
General Relativity Tests with Pulsars Ingrid Stairs UBC Rencontres de Moriond La Thuile March 25, 2011 Green Bank Telescope Jodrell Bank Parkes Arecibo Outline Intro to pulsar timing Equivalence principle
More informationNeutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
More informationPulsar Key Science with the SKA
Pulsar Key Science with the SKA Strong-field tests of gravity using Pulsars and Black Holes Michael Kramer Krabi, April 2007 Pulsar Key Science with the SKA Strong-field tests of gravity using Pulsars
More informationOur View of the Milky Way. 23. The Milky Way Galaxy
23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral
More informationPulsar timing and the IISM: dispersion, scattering,
Pulsar timing and the IISM: dispersion, scattering, Jean-Mathias Grießmeier Station de Radioastronomie de Nançay, LPC2E, Université Orléans jean-mathias.griessmeier@cnrs-orleans.fr Pulsar timing Dispersion
More informationAstronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review
Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review 16-1 Fusion in the Sun The solar corona has temperatures roughly the same as temperatures in the Sun's core, where nuclear fusion takes place.
More informationAccretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
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 informationStellar-Mass Black Holes and Pulsars
Stellar-Mass Black Holes and Pulsars Anthony Rushton Work group 2 leader (ESO ALMA fellow) 2010-06-24 Overview of Work Group 2 Stellar-mass black holes and pulsars Two work group leaders: Anthony Rushton
More informationDiscovery of a transitional Redback millisecond pulsar J !
Discovery of a transitional Redback millisecond pulsar J1227-4853! By Jayanta Roy!! JBCA, University of Manchester!! and!! National Centre for Radio Astrophysics (NCRA-TIFR) Neutron stars at the crossroads,
More informationREAD: Chapter 11.1, 11.2 (11.2.1, only), 11.3(
HW READ: Chapter 11.1, 11.2 (11.2.1,11.2.2 only), 11.3( 11.3.1,11.3.2 only), 11.4,11.5 Question 11.2(HW#15) Problems 1(HW#16) (part a: recall: basic KE=1/2mv 2,Part tb: recall momentum conservation M f
More informationChapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs
Chapter 18 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
More informationASTRONOMY II Spring 1995 FINAL EXAM. Monday May 8th 2:00pm
ASTRONOMY II - 79202 Spring 1995 FINAL EXAM Monday May 8th 2:00pm Name: You have three hours to complete this exam. I suggest you read through the entire exam before you spend too much time on any one
More informationHigh Energy Astrophysics
High Energy Astrophysics Gamma-ray Bursts Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk May 2011 Gamma-ray Bursts - Observations - Long-duration
More informationPulsars. The maximum angular frequency of a spinning star can be found by equating the centripetal and gravitational acceleration M R 2 R 3 G M
Pulsars Pulsating stars were discovered in 1967 via radio dipole antennae by Jocelyn Bell and Anthony Hewish Pulse period of PSR 1919+21 is 1.337 s Most pulsars have periods between 0.25 s and 2 s The
More informationCompact Binaries as Gravitational-Wave Sources
Compact Binaries as Gravitational-Wave Sources Chunglee Kim Lund Observatory Extreme Astrophysics for All 10 February, 2009 Outline Introduction Double-neutron-star systems = NS-NS binaries Neutron star
More informationLIGO Detection of Gravitational Waves. Dr. Stephen Ng
LIGO Detection of Gravitational Waves Dr. Stephen Ng Gravitational Waves Predicted by Einstein s general relativity in 1916 Indirect confirmation with binary pulsar PSR B1913+16 (1993 Nobel prize in physics)
More informationRadiative Processes in Astrophysics
Radiative Processes in Astrophysics 9. Synchrotron Radiation Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Useful reminders relativistic terms, and simplifications for very high velocities
More informationRotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/0608311 Introduction 11 Rotating RAdio Transients (RRATs) (Mclaughlin et al 2006) Repeated, irregular radio bursts
More informationThe double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity. Maxim Lyutikov (Purdue U.)
The double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity Maxim Lyutikov (Purdue U.) The Double Pulsar: sixth most important scientific discovery of 2004 (Science)
More informationThe Dynamic Radio Sky
The Dynamic Radio Sky Exoplanet Bursts, Lunar Neutrinos, and other Exotica Joseph Lazio (Naval Research Laboratory SKA Program Development Office) Who Cares? Radio transients are like butterfly collecting.
More informationGeneral Relativity Tests with Pulsars
General Relativity Tests with Pulsars Ingrid Stairs UBC SLAC Summer Institute July 27, 2005 Much of this material is in Living Reviews in Relativity 2003 5. Pulsars: rotating, magnetized neutron stars.
More informationNeutron Star Astrophysics
Pulsars I. The Why and How of Searching for Exotic Pulsars Jim Cordes, Cornell University Why would you want to know about pulsars and why would you like to discover more? Science, the big questions How
More information