A Pulsar Discovery - Moments of Discovery
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Exploring Pulsars
High-energy astrophysics Explore the PUL SAR menagerie Astronomers are discovering many strange properties of compact stellar objects called pulsars. Here’s how they fit together. by Victoria M. Kaspi f you browse through an astronomy book published 25 years ago, you’d likely assume that astronomers understood extremely dense objects called neutron stars fairly well. The spectacular Crab Nebula’s central body has been a “poster child” for these objects for years. This specific neutron star is a pulsar that I rotates roughly 30 times per second, emitting regular appar- ent pulsations in Earth’s direction through a sort of “light- house” effect as the star rotates. While these textbook descriptions aren’t incorrect, research over roughly the past decade has shown that the picture they portray is fundamentally incomplete. Astrono- mers know that the simple scenario where neutron stars are all born “Crab-like” is not true. Experts in the field could not have imagined the variety of neutron stars they’ve recently observed. We’ve found that bizarre objects repre- sent a significant fraction of the neutron star population. With names like magnetars, anomalous X-ray pulsars, soft gamma repeaters, rotating radio transients, and compact Long the pulsar poster child, central objects, these bodies bear properties radically differ- the Crab Nebula’s central object is a fast-spinning neutron star ent from those of the Crab pulsar. Just how large a fraction that emits jets of radiation at its they represent is still hotly debated, but it’s at least 10 per- magnetic axis. Astronomers cent and maybe even the majority. -
Brochure Pulsar Multifunction Spectroscopy Service Complete Cased Hole Formation Evaluation and Reservoir Saturation Monitoring from A
Pulsar Multifunction spectroscopy service Introducing environment-independent, stand-alone cased hole formation evaluation and saturation monitoring 1 APPLICATIONS FEATURES AND BENEFITS ■ Stand-alone formation evaluation for diagnosis of bypassed ■ Environment-independent reservoir saturation monitoring ■ High-performance pulsed neutron generator (PNG) hydrocarbons, depleted reservoirs, and gas zones in any formation water salinity ● Optimized pulsing scheme with multiple square and short ● Differentiation of gas-filled porosity from very low porosity ● Production fluid profile determination for any well pulses for clean separation in measuring both inelastic and formations by using neutron porosity and fast neutron cross inclination: horizontal, deviated, and vertical capture gamma rays 8 section (FNXS) measurements ● Detection of water entry and flow behind casing ● High neutron output of 3.5 × 10 neutron/s for greater ■ measurement precision Petrophysical evaluation with greater accuracy by accounting ● Gravel-pack quality determination by using for grain density and mineral properties in neutron porosity elemental spectroscopy ■ State-of-the-art detectors ■ Total organic carbon (TOC) quantified as the difference ■ Metals for mining exploration ● Near and far detectors: cerium-doped lanthanum bromide between the measured total carbon and inorganic carbon ■ High-resolution determination of reservoir quality (RQ) (LaBr3:Ce) ■ Oil volume from TOC and completion quality (CQ) for formation evaluation ● Deep detector: yttrium aluminum perovskite -
Determination of the Night Sky Background Around the Crab Pulsar Using Its Optical Pulsation
28th International Cosmic Ray Conference 2449 Determination of the Night Sky Background around the Crab Pulsar Using its Optical Pulsation E. O˜na-Wilhelmi1,2, J. Cortina3, O.C. de Jager1, V. Fonseca2 for the MAGIC collaboration (1) Unit for Space Physics, Potchefstroom University for CHE, Potchefstroom 2520, South Africa (2) Dept. de f´isica At´omica, Nuclear y Molecular, UCM, Ciudad Universitaria s/n, Madrid, Spain (3) Institut de Fisica de l’Altes Energies, UAB, Barcelona, Spain Abstract The poor angular resolution of imaging γ-ray telescopes is offset by the large collection area of the next generation telescopes such as MAGIC (17 m diameter) which makes the study of optical emission associated with some γ-ray sources feasible. In particular the optical photon flux causes an increase in the photomultiplier DC currents. Furthermore, the extremely fast response of PMs make them ideal detectors for fast (subsecond) optical transients and periodic sources like pulsars. The HEGRA CT1 telescope (1.8 m radius) is the smallest Cerenkovˆ telescope which has seen the Crab optical pulsations. 1. Method Imaging Atmospheric Cerenkovˆ Detectors (IACT) can be used to detect the optical emission of an astronomical object through the increase it generates in the currents of the camera pixels [7,3]. Since the Crab pulsar shows pulsed emission in the optical wavelengths with the same frequency as in radio and most probably of VHE γ-rays, we use the central pixel of CT1 [5] and MAGIC [1] to monitor the optical Crab pulsation. Before the Crab observations were performed, the expected rate of the Crab pulsar and background were estimated theoretically. -
PDF (Thesis020605.Pdf)
Optical Pulse-Phased Observations of Faint Pulsars with a Phase-Binning CCD Camera Thesis by Brian Kern In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy ITUTE O ST F N T I E C A I H N N R 1891 O O L F O I G L Y A C California Institute of Technology Pasadena, California 2002 (Submitted May 29, 2002) ii c 2002 Brian Kern All Rights Reserved iii Abstract We have constructed a phase-binning CCD camera optimized for optical observations of faint pulsars. The phase-binning CCD camera combines the high quantum efficiency of a CCD with a pulse-phased time resolution capable of observing pulsars as fast as 10 ms, with no read noise penalty. The phase- binning CCD can also operate as a two-channel imaging polarimeter, obtaining pulse-phased linear photopolarimetric observations. We have used this phase-binning CCD to make the first measurements of optical pulsations from an anomalous X-ray pulsar. We measured the optical pulse profile of 4U 0142+61, finding a pulsed fraction of 27%, many times larger than the pulsed fraction in X-rays. From this observation, we concluded that 4U 0142+61 must be a magnetar, an ultramagnetized neutron star (B>1014 G). The optical pulse is double-peaked, similar to the soft X-ray pulse profile. We also used the phase-binning CCD to obtain the photometric and polarimetric pulse profiles of PSR B0656+14, a middle-aged isolated rotation-powered pulsar. The optical pulse profile we measured significantly disagrees with the low signal-to-noise profile previously published for this pulsar. -
Optical Observations of Pulsars: the ESO Contribution R.P
Figure 3: The normalised spectral energy distribution of 3 galaxies. From left to right we show a regular Ly-break galaxy (Fig. 2c), the “spiral” galaxy (Fig. 2d), and the very red galaxy from Figure 2e. The red continuum feature of the last two galaxies can be due to the Balmer/4000 Angstrom break or due to dust. Only one of these would be selected by the regular Ly-break selection technique, as the others are too faint in the optical (rest-frame UV). Acknowledgement References van Dokkum, P. G., Franx, M., Fabricant, D., Kelson, D., Illingworth, G. D., 2000, sub- Dickinson, M., et al, 1999, preprint, as- It is a pleasure to thank the staff at mitted to ApJ. troph/9908083. Steidel, C. C., Giavalisco, M., Pettini, M., ESO who contributed to the construc- Gioia, I., and Luppino, G. A., 1994, ApJS, tion and operation of the VLT and Dickinson, M., Adelberger, K. L., 1996, 94, 583. ApJL, 462, L17. ISAAC. This project has only been van Dokkum, P. G., Franx, M., Fabricant, D., Williams, R. E., et al, 2000, in prepara- possible because of their enormous ef- Kelson, D., Illingworth, G. D., 1999, ApJL, tion. forts. 520, L95. Optical Observations of Pulsars: the ESO Contribution R.P. MIGNANI1, P.A. CARAVEO 2 and G.F. BIGNAMI3 1ST-ECF, [email protected]; 2IFC-CNR, [email protected]; 3ASI [email protected] Introduction matic gamma-rays source Geminga, and ESO telescopes gave to the not yet recognised as an X/gamma-ray European astronomers the chance to Our knowledge of the optical emis- pulsar, was proposed. -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
EVOLUTION of the CRAB NEBULA in a LOW ENERGY SUPERNOVA Haifeng Yang and Roger A
Draft version August 23, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 EVOLUTION OF THE CRAB NEBULA IN A LOW ENERGY SUPERNOVA Haifeng Yang and Roger A. Chevalier Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904; [email protected], [email protected] Draft version August 23, 2018 ABSTRACT The nature of the supernova leading to the Crab Nebula has long been controversial because of the low energy that is present in the observed nebula. One possibility is that there is significant energy in extended fast material around the Crab but searches for such material have not led to detections. An electron capture supernova model can plausibly account for the low energy and the observed abundances in the Crab. Here, we examine the evolution of the Crab pulsar wind nebula inside a freely expanding supernova and find that the observed properties are most consistent with a low energy event. Both the velocity and radius of the shell material, and the amount of gas swept up by the pulsar wind point to a low explosion energy ( 1050 ergs). We do not favor a model in which circumstellar interaction powers the supernova luminosity∼ near maximum light because the required mass would limit the freely expanding ejecta. Subject headings: ISM: individual objects (Crab Nebula) | supernovae: general | supernovae: indi- vidual (SN 1054) 1. INTRODUCTION energy of 1050 ergs (Chugai & Utrobin 2000). However, SN 1997D had a peak absolute magnitude of 14, con- The identification of the supernova type of SN 1054, − the event leading to the Crab Nebula, has been an en- siderably fainter than SN 1054 at maximum. -
Central Engines and Environment of Superluminous Supernovae
Central Engines and Environment of Superluminous Supernovae Blinnikov S.I.1;2;3 1 NIC Kurchatov Inst. ITEP, Moscow 2 SAI, MSU, Moscow 3 Kavli IPMU, Kashiwa with E.Sorokina, K.Nomoto, P. Baklanov, A.Tolstov, E.Kozyreva, M.Potashov, et al. Schloss Ringberg, 26 July 2017 First Superluminous Supernova (SLSN) is discovered in 2006 -21 1994I 1997ef 1998bw -21 -20 56 2002ap Co to 2003jd 56 2007bg -19 Fe 2007bi -20 -18 -19 -17 -16 -18 Absolute magnitude -15 -17 -14 -13 -16 0 50 100 150 200 250 300 350 -20 0 20 40 60 Epoch (days) Superluminous SN of type II Superluminous SN of type I SN2006gy used to be the most luminous SN in 2006, but not now. Now many SNe are discovered even more luminous. The number of Superluminous Supernovae (SLSNe) discovered is growing. The models explaining those events with the minimum energy budget involve multiple ejections of mass in presupernova stars. Mass loss and build-up of envelopes around massive stars are generic features of stellar evolution. Normally, those envelopes are rather diluted, and they do not change significantly the light produced in the majority of supernovae. 2 SLSNe are not equal to Hypernovae Hypernovae are not extremely luminous, but they have high kinetic energy of explosion. Afterglow of GRB130702A with bumps interpreted as a hypernova. Alina Volnova, et al. 2017. Multicolour modelling of SN 2013dx associated with GRB130702A. MNRAS 467, 3500. 3 Our models of LC with STELLA E ≈ 35 foe. First year light ∼ 0:03 foe while for SLSNe it is an order of magnitude larger. -
Pulsars and Supernova Remnants
1604–2004: SUPERNOVAE AS COSMOLOGICAL LIGHTHOUSES ASP Conference Series, Vol. 342, 2005 M. Turatto, S. Benetti, L. Zampieri, and W. Shea Pulsars and Supernova Remnants Roger A. Chevalier Dept. of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903, USA Abstract. Massive star supernovae can be divided into four categories de- pending on the amount of mass loss from the progenitor star and the star’s ra- dius. Various aspects of the immediate aftermath of the supernova are expected to develop in different ways depending on the supernova category: mixing in the supernova, fallback on the central compact object, expansion of any pul- sar wind nebula, interaction with circumstellar matter, and photoionization by shock breakout radiation. Models for observed young pulsar wind nebulae ex- panding into supernova ejecta indicate initial pulsar periods of 10 − 100 ms and approximate equipartition between particle and magnetic energies. Considering both pulsar nebulae and circumstellar interaction, the observed properties of young supernova remnants allow many of them to be placed in one of the super- nova categories; the major categories are represented. The pulsar properties do not appear to be related to the supernova category. 1. Introduction The association of SN 1054 with the Crab Nebula and its central pulsar can be understood in the context of the formation of the neutron star in the core collapse and the production of a bubble of relativistic particles and magnetic fields at the center of an expanding supernova. Although the finding of more young pulsars and their wind nebulae initially proceeded slowly, there has recently been a rapid set of discoveries of more such pulsars and nebulae (Camilo 2004). -
Astrophysics VLT/UVES Spectroscopy of Wray 977, the Hypergiant
UvA-DARE (Digital Academic Repository) VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301-2 Kaper, L.; van der Meer, A.; Najarro, F. DOI 10.1051/0004-6361:20065393 Publication date 2006 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Kaper, L., van der Meer, A., & Najarro, F. (2006). VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301-2. Astronomy & Astrophysics, 457(2), 595- 610. https://doi.org/10.1051/0004-6361:20065393 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:02 Oct 2021 A&A 457, 595–610 (2006) Astronomy DOI: 10.1051/0004-6361:20065393 & c ESO 2006 Astrophysics VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301−2 L. -
Stsci Newsletter: 1991 Volume 008 Issue 03
SPACE 'fEIFSCOPE SOENCE ...______._.INSTITUIE Operated for NASA by AURA November 1991 Vol. 8No. 3 HIGHLIGHTS OF THIS ISSUE: HSTSCIENCE HIGHLIGHTS WF/PC OBSERVATIONS OF THE STELLAR O NEW SCIENCE RESULTS ON M87, CRAB PULSAR CUSP IN M87 O COSTAR PROGRESSING WELL The photograph on the left shows one of a set of images of the central regions of the giant ellipti O ANSWERS TO YOUR QUESTIONS ABOUT HST DATA cal galaxy M87, obtained in June 1991 withHSI's Wide Field and Planetary Camera {WF/PC). 0 CYCLE 2 PEER REVIEW UNDERWAY Analysis of these images has revealed a stellar cusp in the core of M87, consistent with the pres ence of a massive black hole in its nucleus. A combined approach of image deconvolution and modelling has made it possible to investigate the starlight distribution in M87 down to a limiting radius of about 0'.'04 from the nucleus (or about 3 pc from the nucleus if the Virgo cluster is at 16 Mpc). The results show that the central struc ture of M87 can be described by three compo nents: a power-law starlight profile with an r·114 slope which continues unabated into the center, an unresolved central point source, and optical coun terparts of the jet knots identified by VLBI obser vations. In both the V- and /-band Planetary Camera images, the stellar cusp is consistent with the black-hole model proposed for M87 by Young et al. in 1978; in this model, there is a central mas sive object of about 3 x 109 Me. -
Gravitational Waves from Neutron & Strange-Quark Stars
Gravitational Waves From Neutron & Strange-quark Stars • A billion tons per teaspoon: the history of neutron stars. • The discovery of pulsars and identification with NS. • Are NS really strange- quark stars? Supported by the National Science Foundation http://www.ligo.caltech.edu • GWs from NS and SQS. Gregory Mendell • What will we learn? LIGO Hanford Observatory LIGO-G050005-00-W The Neutron Star Idea • Chandrasekhar Supernova 1987A 1931: white dwarf stars will collapse if M > 1.4 solar masses. Then what? • Baade & Zwicky 1934: suggest SN form NS. • Oppenheimer & Volkoff 1939: work http://www.aao.gov.au/images/captions/aat050.html out NS models. Anglo-Australian Observatory, photo by David Malin. (http://www.jb.man.ac.uk/~pul sar/tutorial/tut/tut.html; LIGO-G050005-00-W Jodrell Bank Tutorial) Discovery of Pulsars • Bell notes “scruff” on chart in 1967. • Close up reveals the first pulsar (pulsating radio source) with P = 1.337 s. • Rises & sets with the stars: source is extraterrestrial. • LGM? • More pulsars discovered indicating pulsars are natural phenomena. www.jb.man.ac.uk/~pulsar/tutorial/LIGO-G050005tut/node3.html#SECTION00012000000000000000-00-W A. G. Lyne and F. G. Smith. Pulsar Astronomy. Cambridge University Press, 1990. Pulsars = Neutron Stars • Gold 1968: pulsars are rotating neutron stars. •orbital motion •oscillation •rotation • From the Sung-shih (Chinese Astronomical Treatise): "On the 1st year of the Chi-ho reign period, 5th month, chi-chou (day) [1054 AD], a guest star appeared…south-east of Tian-kuan [Aldebaran].(http://super.colorado.edu/~a str1020/sung.html) http://antwrp.gsfc.nasa.gov/apod/ap991122.html Crab Nebula: FORS Team, 8.2-meter VLT, ESO LIGO-G050005-00-W Pulsars Seen and Heard Play Me (Vela Pulsar) http://www.jb.m an.ac.uk/~pulsa r/Education/Sou nds/sounds.html (Crab Pulsar) Jodrell Bank Observatory, Dept.