Supermassive Black Hole Binaries and Transient Radio Events: Studies in Pulsar Astronomy

Total Page:16

File Type:pdf, Size:1020Kb

Supermassive Black Hole Binaries and Transient Radio Events: Studies in Pulsar Astronomy Supermassive Black Hole Binaries and Transient Radio Events: Studies in Pulsar Astronomy Sarah Burke Spolaor Presented in fulfillment of the requirements of the degree of Doctor of Philosophy 2011 Faculty of Information and Communication Technology Swinburne University i Abstract The field of pulsar astronomy encompasses a rich breadth of astrophysical topics. The research in this thesis contributes to two particular subjects of pulsar astronomy: gravitational wave science, and identifying celestial sources of pulsed radio emission. We first investigated the detection of supermassive black hole (SMBH) binaries, which are the brightest expected source of gravitational waves for pulsar timing. We consid- ered whether two electromagnetic SMBH tracers, velocity-resolved emission lines in active nuclei, and radio galactic nuclei with spatially-resolved, flat-spectrum cores, can reveal systems emitting gravitational waves in the pulsar timing band. We found that there are systems which may in principle be simultaneously detectable by both an electromagnetic signature and gravitational emission, however the probability of actually identifying such a system is low (they will represent 1% of a randomly selected galactic nucleus sample). ≪ This study accents the fact that electromagnetic indicators may be used to explore binary populations down to the “stalling radii” at which binary inspiral evolution may stall indef- initely at radii exceeding those which produce gravitational radiation in the pulsar timing band. We then performed a search for binary SMBH holes in archival Very Long Base- line Interferometry data for 3114 radio-luminous active galactic nuclei. One source was detected as a double nucleus. This result is interpreted in terms of post-merger timescales for SMBH centralisation, implications for “stalling”, and the relationship of radio activity in nuclei to mergers. Our analysis suggested that binary pair evolution of SMBHs (both 8 of masses >10 M⊙) spends less than 500 Myr in progression from the merging of galactic stellar cores to within the purported stalling radius for SMBH pairs, giving no evidence for an excess of stalled binary systems at small separations. Circumstantial evidence showed that the relative state of radio emission between paired SMBHs is correlated within orbital separations of 2.5 kpc. We then searched for transient radio events in two archival pulsar surveys, and in the new High Time Resolution Universe (HTRU) Survey. We present the methodology employed for these searches, noting the novel addition of methods for single-event recog- nition, automatic interference mitigation, and data inspection. 27 new neutron stars were discovered. We discuss the relationship between “rotating radio transient” (RRAT) and pulsar populations, finding that the Galactic z-distribution of RRATs closely resembles the distribution of pulsars, and where measurable, RRAT pulse widths are similar to in- dividual pulses from pulsars of similar period, implying a similar beaming fraction. We postulate that many RRATs may simply represent a tail of extreme-nulling pulsars that are “on” for less than a pulse period; this is supported by the fact that nulling pulsars and single-pulse discoveries exhibit a continuous distribution across null/activity timescales and nulling fractions. We found a drop-off in objects with emissivity cycles longer than ii 300 seconds at intermediate and low nulling fractions which is not readily explained by ∼ selection effects. The HTRU deep low-latitude survey (70- min. pointings at galactic lati- tudes b < 3.5◦ and longitudes 80◦ <l< 30◦) will be capable of exploring whether this | | − deficit is natural or an effect of selection. The intriguing object PSR J0941–39 may rep- resent an evolutionary link between nulling populations; discovered as an sparsely-pulsing RRAT, in follow-up observations it often appeared as a bright (10 mJy) pulsar with a low nulling fraction. It is therefore apparent that a neutron star can oscillate between nulling levels, much like mode-changing pulsars. Crucially, the RRAT and pulsar-mode emission sites are coincident, implying that the two emission mechanisms are linked. We estimate that the full HTRU survey will roughly quadruple the known deep-nulling pulsar popu- lation, allowing statistical studies to be made of extreme-nulling populations. HTRU’s low-latitude survey will explore the neutron star population with null lengths lasting up to several hours. We lastly reported the discovery of 16 pulses, the bulk of which exhibit a frequency sweep with a shape and magnitude resembling the “Lorimer Burst” (Lorimer et al. 2007), which three years ago was reported as a solitary radio burst that was thought to be the first discovery of a rare, impulsive event of unknown extragalactic origin. However, the new events were of clearly terrestrial origin, with properties unlike any known sources of terrestrial broad-band radio emission. The new detections cast doubt on the extragalactic interpretation of the original burst, and call for further sophistication in radio-pulse sur- vey techniques to identify the origin of the anomalous terrestrial signals and definitively distinguish future extragalactic pulse detections from local signals. The ambiguous origin of these seemingly dispersed, swept-frequency signals suggest that radio-pulse searches us- ing multiple detectors will be the only experiments able to provide definitive information about the origin of new swept-frequency radio burst detections. Finally, we summarise our major findings and suggest future work which would expand on the work in this thesis. iii Acknowledgements Many good people have contributed to the completion of this thesis and to the unique period of personal and professional growth that the past few years have represented. I owe a big round of thanks to four great supervisors, Matthew Bailes, Dick Manchester, Simon Johnston, and David Barnes, who each in their way has constantly conveyed an excitement for science and the scientific process that I strive to replicate. I appreciate the scientific and personal support offered by all of them at various times, as well as the space and encouragement they gave to explore my own ideas (and patient support through those “bold claims,” as Matthew would say, that came from left-field ideas!). All of these elements were essential in navigating successfully through this period, and my closer supervisors, Dick, Simon, and Matthew, all made crucial contributions to my education and to developing the scientific ideas explored by this thesis. I would like to particularly thank my primary supervisor, Matthew, for being an important role model for balancing the importance of family with a strong astronomical career. I have a great respect for the leadership he has shown over the course of my PhD. I am tremendously grateful to have had the chance to interact closely with both Ron Ekers and George Hobbs. Ron first introduced me to the Australian scientific community and has always been a valuable sounding board for new ideas, a like-minded brainstorm companion, a constant source of encouragement and way-out-of-the-box thinking, a men- tor, and a good friend. George has likewise been an indespensable part of my candidature, often providing a house filled with good music, food, films, and strange board games, and always providing insightful discussions on pulsar and extragalactic astronomy. I must ex- press appreciation for those who laid the seeds of my scientific career early on through dedicated and creative teaching. This includes Doc Stoneback, Steve Boughn, Walter Smith, and the person who first introduced me to the world of scientific research and to the Universe through cosmology, Prof. Bruce Partridge. A very general thanks go to the staff and scientists at Swinburne Ctr. for Astrophysics, ATNF Marsfield, and Parkes Telescope: rest assured all of you helped make each of these places welcoming, engaging institutions. I hold special thanks for a few: the post-docs at Swinburne who let me wander into their offices to either chat idly, snatch books off their shelves, nag them about code bugs, or deliberate about a range of topics—Willem, Ramesh, Andrew, and Jonathon, thanks for all that. It has been a pleasure to learn from such knowledgeable scientists, and in many cases, have sources of light relief in S. Amy, B. Koribalski, J. Reynolds, G. Carrad, T. Tzioumis, R. Hollow, C. Cliff, J. Caswell, T. Cornwell, R. Smits, R. Jenet, Shirley and Janette, J. Khoo, DJ Champion, E. Sadler, A. Graham, T. Murphy, M. Kesteven, M. Keith, P. Weltevrede, and D. Schnitzeler. Big thanks are owed to John Sarkissian for the countless late-night chats about everything in iv the world, and the tireless help with observing. My fellow students and friends have been necessary stress relievers along the way, particularly my “not-really-band-mates” Joris, Carlos, Chris, and Max, as well as many others in and out of work like Lina, Stefan, Evelyn, Adam, Juan, Adrian, Francesco, Caterina, Andy, Ben, Amanda and Jonathon, Marc, Glenn, Nigel, Nick Jones, Minnie, Katherine Newton-McGee, Peter and Sofie. I hope to see you all again many times in the coming years of our careers. Last and anything but least, I acknowledge the invaluable and ongoing support of my family. From my beginning, my parents have taught and encouraged me to pursue every interest in and out of this world; they, my siblings Hannah and Ryan, JPL, and my extended family have represented a wonderful source of many different kinds of wisdom and friendship in my
Recommended publications
  • Active Galactic Nuclei: a Brief Introduction
    Active Galactic Nuclei: a brief introduction Manel Errando Washington University in St. Louis The discovery of quasars 3C 273: The first AGN z=0.158 2 <latexit sha1_base64="4D0JDPO4VKf1BWj0/SwyHGTHSAM=">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</latexit> <latexit sha1_base64="H7Rv+ZHksM7/70841dw/vasasCQ=">AAACQHicbVDLSgMxFM34tr6qLt0Ei+BCy0TEx0IoPsBlBWuFTlsyaVqDSWZI7ghlmE9z4ye4c+3GhSJuXZmxFXxdCDk599zk5ISxFBZ8/8EbGR0bn5icmi7MzM7NLxQXly5slBjGayySkbkMqeVSaF4DAZJfxoZTFUpeD6+P8n79hhsrIn0O/Zg3Fe1p0RWMgqPaxXpwzCVQfNIOFIUro1KdMJnhA+yXfX832FCsteVOOzgAobjFxG+lhGTBxpe+HrBOBNjiwd5rpZsky9rFUn5BXvgvIENQQsOqtov3QSdiieIamKTWNogfQzOlBgSTPCsEieUxZde0xxsOaurMNNPPADK85pgO7kbGLQ34k/0+kVJlbV+FTpm7tr97Oflfr5FAd6+ZCh0nwDUbPNRNJIYI52nijjCcgew7QJkRzitmV9RQBi7zgguB/P7yX3CxVSbb5f2z7VLlcBjHFFpBq2gdEbSLKugUVVENMXSLHtEzevHuvCfv1XsbSEe84cwy+lHe+wdR361Q</latexit> The power source of quasars • The luminosity (L) of quasars, i.e. how bright they are, can be as high as Lquasar ~ 1012 Lsun ~ 1040 W. • The energy source of quasars is accretion power: - Nuclear fusion: 2 11 1 ∆E =0.007 mc =6 10 W s g−
    [Show full text]
  • Undergraduate Thesis on Supermassive Black Holes
    Into the Void: Mass Function of Supermassive Black Holes in the local universe A Thesis Presented to The Division of Mathematics and Natural Sciences Reed College In Partial Fulfillment of the Requirements for the Degree Bachelor of Arts Farhanul Hasan May 2018 Approved for the Division (Physics) Alison Crocker Acknowledgements Writing a thesis is a long and arduous process. There were times when it seemed further from my reach than the galaxies I studied. It’s with great relief and pride that I realize I made it this far and didn’t let it overpower me at the end. I have so many people to thank in very little space, and so much to be grateful for. Alison, you were more than a phenomenal thesis adviser, you inspired me to believe that Astro is cool. Your calm helped me stop freaking out at the end of February, when I had virtually no work to show for, and a back that ached with every step I took. Thank you for pushing me forward. Working with you in two different research projects were very enriching experiences, and I appreciate you not giving up on me, even after all the times I blanked on how to proceed forward. Thank you Johnny, for being so appreciative of my work, despite me bringing in a thesis that I myself barely understood when I brought it to your table. I was overjoyed when I heard you wanted to be on my thesis board! Thanks to Reed, for being the quirky, intellectual community that it prides itself on being.
    [Show full text]
  • Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 Xxneutron-Star Binaries: X-Ray Bursters
    Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 XXNeutron-Star Binaries: X-ray bursters [Look at the slides and the pictures in your book, but I won’t test you on this in detail, and we may skip altogether in class.] 22.4 Gamma-Ray Bursts 22.5 Black Holes 22.6 XXEinstein’s Theories of Relativity Special Relativity 22.7 Space Travel Near Black Holes 22.8 Observational Evidence for Black Holes Tests of General Relativity Gravity Waves: A New Window on the Universe Neutron Stars and Pulsars (sec. 22.1, 2 in textbook) 22.1 Neutron Stars According to models for stellar explosions: After a carbon detonation supernova (white dwarf in binary), little or nothing remains of the original star. After a core collapse supernova, part of the core may survive. It is very dense—as dense as an atomic nucleus—and is called a neutron star. [Recall that during core collapse the iron core (ashes of previous fusion reactions) is disintegrated into protons and neutrons, the protons combine with the surrounding electrons to make more neutrons, so the core becomes pure neutron matter. Because of this, core collapse can be halted if the core’s mass is between 1.4 (the Chandrasekhar limit) and about 3-4 solar masses, by neutron degeneracy.] What do you get if the core mass is less than 1.4 solar masses? Greater than 3-4 solar masses? 22.1 Neutron Stars Neutron stars, although they have 1–3 solar masses, are so dense that they are very small.
    [Show full text]
  • Radio Observations of the Supermassive Black Hole at the Galactic Center and Its Orbiting Magnetar
    Radio Observations of the Supermassive Black Hole at the Galactic Center and its Orbiting Magnetar Rebecca Rimai Diesing Honors Thesis Department of Physics and Astronomy Northwestern University Spring 2017 Honors Thesis Advisor: Farhad Zadeh ! Radio Observations of the Supermassive Black Hole at the Galactic Center and its Orbiting Magnetar Rebecca Rimai Diesing Department of Physics and Astronomy Northwestern University Honors Thesis Advisor: Farhad Zadeh Department of Physics and Astronomy Northwestern University At the center of our galaxy a bright radio source, Sgr A*, coincides with a black hole four million times the mass of our sun. Orbiting Sgr A* at a distance of 3 arc seconds (an estimated 0.1 pc) and rotating with a period of 3.76 s is a magnetar, or pulsar⇠ with an extremely strong magnetic field. This magnetar exhibited an X-ray outburst in April 2013, with enhanced, highly variable radio emission detected 10 months later. In order to better understand the behavior of Sgr A* and the magnetar, we study their intensity variability as a function of both time and frequency. More specifically, we present the results of short (8 minute) and long (7 hour) radio continuum observations, taken using the Jansky Very Large Array (VLA) over multiple epochs during the summer of 2016. We find that Sgr A*’s flux density (a proxy for intensity) is highly variable on an hourly timescale, with a frequency dependence that di↵ers at low (34 GHz) and high (44 GHz) frequencies. We also find that the magnetar remains highly variable on both short (8 min) and long (monthly) timescales, in agreement with observations from 2014.
    [Show full text]
  • BLACK HOLES: the OTHER SIDE of INFINITY General Information
    BLACK HOLES: THE OTHER SIDE OF INFINITY General Information Deep in the middle of our Milky Way galaxy lies an object made famous by science fiction—a supermassive black hole. Scientists have long speculated about the existence of black holes. German astronomer Karl Schwarzschild theorized that black holes form when massive stars collapse. The resulting gravity from this collapse would be so strong that the matter would become more and more dense. The gravity would eventually become so strong that nothing, not even radiation moving at the speed of light, could escape. Schwarzschild’s theories were predicted by Einstein and then borne out mathematically in 1939 by American astrophysicists Robert Oppenheimer and Hartland Snyder. WHAT EXACTLY IS A BLACK HOLE? First, it’s not really a hole! A black hole is an extremely massive concentration of matter, created when the largest stars collapse at the end of their lives. Astronomers theorize that a point with infinite density—called a singularity—lies at the center of black holes. SO WHY IS IT CALLED A HOLE? Albert Einstein’s 1915 General Theory of Relativity deals largely with the effects of gravity, and in essence predicts the existence of black holes and singularities. Einstein hypothesized that gravity is a direct result of mass distorting space. He argued that space behaves like an invisible fabric with an elastic quality. Celestial bodies interact with this “fabric” of space-time, appearing to create depressions termed “gravity wells” and drawing nearby objects into orbit around them. Based on this principle, the more massive a body is in space, the deeper the gravity well it will create.
    [Show full text]
  • Active Galactic Nuclei
    Active Galactic Nuclei • Optical spectra, distance, line width • Varieties of AGN and unified scheme • Variability and lifetime • Black hole mass and growth • Geometry: disk, BLR, NLR • Reverberation mapping • Jets and blazars • AGN spectra Optical spectrum of an AGN • Variety of different emission lines • Each line has centroid, area, width • There is also continuum emission Emission lines • Shift of line centroid gives recession velocity v/c = Δλ/λ. • The width is usually characterized by the “Full Width at Half Maximum”. For a Gaussian FHWM = 2.35σ. • The line width is determined by the velocity distribution of the line emitting gas, Δv/c = σ/λ. • Area is proportional to the number of detected line photons or the line flux. • Usually characterized by “equivalent width” or range in wavelength over which integration of the continuum produces the same flux as the line. Early observations of AGN • Very wide emission lines have been known since 1908. • In 1959, Woltjer noted that if the profiles are due to Doppler motion and the gas is gravitationally bound then v2 ~ GM/r. For v ~ 2000 km/s, we have 10 r M ≥10 ( 100 pc ) M Sun • So AGN, known at the time as Seyfert galaxies, must either have a very compact and luminous nucleus or be very massive. Quasars • Early radio telescopes found radio emission from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. Quasar optical spectra Redshift of 3C273 is 0.16.
    [Show full text]
  • Long-Term Evolution and Physical Properties of Rotating Radio Transients
    LONG-TERM EVOLUTION AND PHYSICAL PROPERTIES OF ROTATING RADIO TRANSIENTS by Ali Arda Gençali Submitted to the Graduate School of Engineering and Natural Sciences in partial fulfillment of the requirements for the degree of Master of Science Sabancı University June 2018 c Ali Arda Gençali 2018 All Rights Reserved LONG-TERM EVOLUTION AND PHYSICAL PROPERTIES OF ROTATING RADIO TRANSIENTS Ali Arda Gençali Physics, Master of Science Thesis, 2018 Thesis Supervisor: Assoc. Prof. Ünal Ertan Abstract A series of detailed work on the long-term evolutions of young neutron star pop- ulations, namely anomalous X-ray pulsars (AXPs), soft gamma repeaters (SGRs), dim isolated neutron stars (XDINs), “high-magnetic-field” radio pulsars (HBRPs), and central compact objects (CCOs) showed that the X-ray luminosities, LX, and the rotational prop- erties of these systems can be reached by the neutron stars evolving with fallback discs and conventional dipole fields. Remarkably different individual source properties of these populations are reproduced in the same model as a result of the differences in their initial conditions, magnetic moment, initial rotational period, and the disc properties. In this the- sis, we have analysed the properties of the rotating radio transients (RRATs) in the same model. We investigated the long-term evolution of J1819–1458, which is the only RRAT detected in X-rays. The period, period derivative and X-ray luminosity of J1819–1458 11 can be reproduced simultaneously with a magnetic dipole field strength B0 ∼ 5 × 10 G on the pole of the neutron star, which is much smaller than the field strength inferred from the dipole-torque formula.
    [Show full text]
  • Educational Guide for Black Holes
    NATIONAL STANDARDS SCIENCE AS INQUIRY Abilities necessary to do scientific inquiry identify questions and concepts that guide scientific investigation design and conduct scientific investigations use technology and mathematics to improve investigations and communications formulate and revise scientific explanations and models using logic and evidence recognize and analyze alternative explanations and models communicate and defend a scientific argument Understanding about scientific inquiry PHYSICAL SCIENCE Structure and properties of matter Interactions of energy and matter Motions and forces EARTH AND SPACE SCIENCE Origin and evolution of the universe SCIENCE AND TECHNOLOGY Understanding about science and technology HISTORY AND NATURE OF SCIENCE Science as a human endeavor Nature of scientific knowledge Historical perspectives 1 BLACK HOLES: THE OTHER SIDE OF INFINITY General Information Deep in the middle of our Milky Way galaxy lies an object made famous by science fiction—a supermassive black hole. Scientists have long speculated about the existence of black holes. German astronomer Karl Schwarzschild theorized that black holes form when massive stars collapse. The resulting gravity from this collapse would be so strong that the matter would become more and more dense. The gravity would eventually become so strong that nothing, not even radiation moving at the speed of light, could escape. Schwarzschild’s theories were predicted by Einstein and then borne out mathematically in 1939 by American astrophysicists Robert Oppenheimer and Hartland Snyder. WHAT EXACTLY IS A BLACK HOLE? First, it’s not really a hole! A black hole is an extremely massive concentration of matter, created when the largest stars collapse at the end of their lives.
    [Show full text]
  • Black Holes, Neutrinos and Gravitational Proprieties of Antimatter
    Black holes, neutrinos and gravitational proprieties of antimatter Dragan Slavkov Hajdukovic CERN, CH-1211 Geneva 23 and Cetinje, Montenegro [email protected] Abstract The gravitational proprieties of antimatter are still a secret of nature. One outstanding possibility is that there is gravitational repulsion between matter and antimatter (in short we call it antigravity). We argue that in the case of antigravity, the collapse of a black hole doesn’t end with singularity and that deep inside the horizon, the gravitational field may be sufficiently strong to create (from the vacuum) neutrino-antineutrino pairs of all flavours. The created antineutrinos (neutrinos) should be violently ejected outside the horizon of a black hole composed from matter (antimatter). Our calculations suggest that both, the supermassive black hole in the centre of our Galaxy (Southern Sky) and in the centre of the Andromeda Galaxy (Northern Sky) may produce a flux of antineutrinos measurable with the new generation of the neutrino telescopes; like the IceCube Neutrino Detector under construction at the South Pole, and the future one cubic kilometre telescope in the Mediterranean Sea. A by the way result of our consideration, is a conjecture allowing determination of the absolute neutrino masses. In addition, we predict that in the case of microscopic black holes which may be eventually produced at the Large Hadron Collider at CERN, their thermal (Hawking’s) radiation should be dominated by a non-thermal radiation caused by antigravity. 1. Introduction A huge majority of physicists thinks that particles and antiparticles (for instance protons and antiprotons) have the same acceleration in the gravitational field of the Earth.
    [Show full text]
  • The (Black Hole Mass)-(Host Spheroid Luminosity) Relation at High and Low
    Draft version July 22, 2018 Preprint typeset using LATEX style emulateapj v. 03/07/07 THE (BLACK HOLE MASS)–(HOST SPHEROID LUMINOSITY) RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES Alister W. Graham1 and Nicholas Scott Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia. Draft version July 22, 2018 ABSTRACT From a sample of 72 galaxies with reliable supermassive black hole masses Mbh, we derive the Mbh– (host spheroid luminosity, L) relation for i) the subsample of 24 core-S´ersic galaxies with partially depleted cores, and ii) the remaining subsample of 48 S´ersic galaxies. Using Ks-band Two Micron 1.10±0.20 All Sky Survey data, we find the near-linear relation Mbh L for the core-S´ersic spheroids ∝ Ks thought to be built in additive dry merger events, while M L2.73±0.55 for the S´ersic spheroids built bh Ks from gas-rich processes. After converting literature B-band∝ disk galaxy magnitudes into inclination- and dust-corrected bulge magnitudes, via a useful new equation presented herein, we obtain a similar result. Unlike with the Mbh–(velocity dispersion) diagram, which is also updated here using the same galaxy sample, it remains unknown whether barred and non-barred S´ersic galaxies are offset from each other in the Mbh–L diagram. While black hole feedback has typically been invoked to explain what was previously thought to be a nearly constant M /M mass ratio of 0.2%, we advocate that the near-linear M – bh Spheroid ∼ bh L and Mbh–MSpheroid relations observed at high masses may have instead largely arisen from the additive dry merging of galaxies.
    [Show full text]
  • A Portrait of a Black Hole
    Overview_Black Holes A picture of a dark monster. The image is the first direct visual evidence of a black hole. This particularly massive specimen is at the center of the supergiant galaxy Messier 87 and was acquired by the Event Horizon Telescope (EHT), an array of eight ground-based radio telescopes distributed around the globe. A portrait of a black hole Black holes swallow all light, making them invisible. That’s what you’d think anyway, but astronomers thankfully know that this isn’t quite the case. They are, in fact, surrounded by a glowing disc of gas, which makes them visible against this bright background, like a black cat on a white sofa. And that’s how the Event Horizon Telescope has now succeeded in taking the first picture of a black hole. Researchers from the Max Planck Institute for Radio Astronomy in Bonn and the Institute for Radio Astronomy in the Millimeter Range (IRAM) in Grenoble, France, were among those making the observations. Photo: EHT Collaboration TEXT HELMUT HORNUNG n spring 2017, scientists linked up objects at extremely small angles of less tion of the Max Planck Institute for Ra- eight telescopes spread out over than 20 microarcseconds. With that dio Astronomy. In the 2017 observing one face of the globe for the first resolution, our eyes would see individ- session alone, the telescopes recorded time, forming a virtual telescope ual molecules on our own hands. approximately four petabytes of data. with an effective aperture close to This is such a huge volume that it was the Idiameter of the entire planet.
    [Show full text]
  • Neutron Star
    Explosive end of a star (masses M > 8 M⊙ ) Death of massive stars M > 8 M⊙ nuclear reactions stop at Fe ⟹ contraction continues to T = 1010 K (e− degenerate gas cannot support the star for core mass Mcore > 1.4 M⊙ ) ⟹ Fe photo-disintegration (production of α particles, neutrons, protons) ⟹ energy absorbed, contraction goes faster, density grows to point when: e− + p → n + νe ⟹ e− are removed support of e− degenerate gas drops ⟹ collapse continues 12 17 3 T = 10 K, core density 3×10 kg / m ⟹ neutron degeneracy pressure ⟹ collapse suddenly stops ⟹ matter falling inward at high high speed matter bounces when core reached ⟹ shock front outwards ⟹ STAR EXPLODES (SUPERNOVA) ⟹ STAR EXPLODES (SUPERNOVA) Not clear what happens, some or all of the following processes: • Shock wave blows apart outer layer, mainly light elements • Shock wave heats gas to T = 1010 K ⟹ explosive nuclear reactions ⟹ fusion produce Fe-peak elements ⟹ outer layer blown apart • Enormous amount of neutrinos formed. Most escape without interaction, some lift off mass in outer layer External envelope falling inwards at speed up to v ~ 70,000 km/s Bounce backward when core reached → Shock front outward Star destroyed by explosion Stellar explosion = supernova (computer simulation) Video: https://www.youtube.com/watch?v=xVk48Nyd4zY Final result of core collapse: neutron star Supernova remnant: Crab Nebula Distance: 6500 light years Explosion seen in 1054 Size of the bubble: ~ 10 pc Final result of core collapse: neutron star Supernova remnant: Crab Nebula Distance: 6500 light
    [Show full text]