Air Force Had Early Warning of Pulsars
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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. -
Planetary Nebulae Jacob Arnold AY230, Fall 2008
Jacob Arnold Planetary Nebulae Jacob Arnold AY230, Fall 2008 1 PNe Formation Low mass stars (less than 8 M) will travel through the asymptotic giant branch (AGB) of the familiar HR-diagram. During this stage of evolution, energy generation is primarily relegated to a shell of helium just outside of the carbon-oxygen core. This thin shell of fusing He cannot expand against the outer layer of the star, and rapidly heats up while also quickly exhausting its reserves and transferring its head outwards. When the He is depleted, Hydrogen burning begins in a shell just a little farther out. Over time, helium builds up again, and very abruptly begins burning, leading to a shell-helium-flash (thermal pulse). During the thermal-pulse AGB phase, this process repeats itself, leading to mass loss at the extended outer envelope of the star. The pulsations extend the outer layers of the star, causing the temperature to drop below the condensation temperature for grain formation (Zijlstra 2006). Grains are driven off the star by radiation pressure, bringing gas with them through collisions. The mass loss from pulsating AGB stars is oftentimes referred to as a wind. For AGB stars, the surface gravity of the star is quite low, and wind speeds of ~10 km/s are more than sufficient to drive off mass. At some point, a super wind develops that removes the envelope entirely, a phenomenon not yet fully understood (Bernard-Salas 2003). The central, primarily carbon-oxygen core is thus exposed. These cores can have temperatures in the hundreds of thousands of Kelvin, leading to a very strong ionizing source. -
Introduction to Astronomy from Darkness to Blazing Glory
Introduction to Astronomy From Darkness to Blazing Glory Published by JAS Educational Publications Copyright Pending 2010 JAS Educational Publications All rights reserved. Including the right of reproduction in whole or in part in any form. Second Edition Author: Jeffrey Wright Scott Photographs and Diagrams: Credit NASA, Jet Propulsion Laboratory, USGS, NOAA, Aames Research Center JAS Educational Publications 2601 Oakdale Road, H2 P.O. Box 197 Modesto California 95355 1-888-586-6252 Website: http://.Introastro.com Printing by Minuteman Press, Berkley, California ISBN 978-0-9827200-0-4 1 Introduction to Astronomy From Darkness to Blazing Glory The moon Titan is in the forefront with the moon Tethys behind it. These are two of many of Saturn’s moons Credit: Cassini Imaging Team, ISS, JPL, ESA, NASA 2 Introduction to Astronomy Contents in Brief Chapter 1: Astronomy Basics: Pages 1 – 6 Workbook Pages 1 - 2 Chapter 2: Time: Pages 7 - 10 Workbook Pages 3 - 4 Chapter 3: Solar System Overview: Pages 11 - 14 Workbook Pages 5 - 8 Chapter 4: Our Sun: Pages 15 - 20 Workbook Pages 9 - 16 Chapter 5: The Terrestrial Planets: Page 21 - 39 Workbook Pages 17 - 36 Mercury: Pages 22 - 23 Venus: Pages 24 - 25 Earth: Pages 25 - 34 Mars: Pages 34 - 39 Chapter 6: Outer, Dwarf and Exoplanets Pages: 41-54 Workbook Pages 37 - 48 Jupiter: Pages 41 - 42 Saturn: Pages 42 - 44 Uranus: Pages 44 - 45 Neptune: Pages 45 - 46 Dwarf Planets, Plutoids and Exoplanets: Pages 47 -54 3 Chapter 7: The Moons: Pages: 55 - 66 Workbook Pages 49 - 56 Chapter 8: Rocks and Ice: -
Lecture 3 - Minimum Mass Model of Solar Nebula
Lecture 3 - Minimum mass model of solar nebula o Topics to be covered: o Composition and condensation o Surface density profile o Minimum mass of solar nebula PY4A01 Solar System Science Minimum Mass Solar Nebula (MMSN) o MMSN is not a nebula, but a protoplanetary disc. Protoplanetary disk Nebula o Gives minimum mass of solid material to build the 8 planets. PY4A01 Solar System Science Minimum mass of the solar nebula o Can make approximation of minimum amount of solar nebula material that must have been present to form planets. Know: 1. Current masses, composition, location and radii of the planets. 2. Cosmic elemental abundances. 3. Condensation temperatures of material. o Given % of material that condenses, can calculate minimum mass of original nebula from which the planets formed. • Figure from Page 115 of “Physics & Chemistry of the Solar System” by Lewis o Steps 1-8: metals & rock, steps 9-13: ices PY4A01 Solar System Science Nebula composition o Assume solar/cosmic abundances: Representative Main nebular Fraction of elements Low-T material nebular mass H, He Gas 98.4 % H2, He C, N, O Volatiles (ices) 1.2 % H2O, CH4, NH3 Si, Mg, Fe Refractories 0.3 % (metals, silicates) PY4A01 Solar System Science Minimum mass for terrestrial planets o Mercury:~5.43 g cm-3 => complete condensation of Fe (~0.285% Mnebula). 0.285% Mnebula = 100 % Mmercury => Mnebula = (100/ 0.285) Mmercury = 350 Mmercury o Venus: ~5.24 g cm-3 => condensation from Fe and silicates (~0.37% Mnebula). =>(100% / 0.37% ) Mvenus = 270 Mvenus o Earth/Mars: 0.43% of material condensed at cooler temperatures. -
Quasistellar Objects: Overview ENCYCLOPEDIA of ASTRONOMY and ASTROPHYSICS
eaa.iop.org DOI: 10.1888/0333750888/1585 Quasistellar Objects: Overview Patrick Osmer From Encyclopedia of Astronomy & Astrophysics P. Murdin © IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of Physics Publishing Bristol and Philadelphia Downloaded on Thu Mar 02 22:43:08 GMT 2006 [131.215.103.76] Terms and Conditions Quasistellar Objects: Overview ENCYCLOPEDIA OF ASTRONOMY AND ASTROPHYSICS Quasistellar Objects: Overview Quasistellar objects, or quasars, were defined originally as star-like objects of large redshift. Quasars are believed to be powered by the accretion of matter onto massive black holes at the centers of galaxies, a process that emits more energy than thermonuclear reactions. Today, quasars are considered to be the most luminous members of the general class of objects called active galactic nuclei, or AGNs. Quasars are the most luminous objects in the universe. This article begins with a brief history of the discovery of quasars. Next it describes their main properties and the concepts that have been developed to explain them. It continues with a description of their nature and theoretical models. Then additional properties and topics are considered: absorption lines, host galaxies, Figure 1. Optical image of 3C273. The object looks stellar in and luminosity functions and evolution. this image except that it is accompanied by a jet of radiation extending to the lower right. (Credit National Optical Astronomy Observatories/National Science Foundation. History Copyright Association of Universities for Research in In 1960 Mathews and Sandage identified the radio source Astronomy Inc (AURA), all rights reserved.) 3C 48 (the 48th object in the 3rd Cambridge catalog of radio sources) with a star-like object of 16th magnitude. -
The MUSE View of the Planetary Nebula NGC 3132? Ana Monreal-Ibero1,2 and Jeremy R
A&A 634, A47 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936845 & © ESO 2020 Astrophysics The MUSE view of the planetary nebula NGC 3132? Ana Monreal-Ibero1,2 and Jeremy R. Walsh3,?? 1 Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Universidad de La Laguna, Dpto. Astrofísica, 38206 La Laguna, Tenerife, Spain 3 European Southern Observatory, Karl-Schwarzschild Strasse 2, 85748 Garching, Germany Received 4 October 2019 / Accepted 6 December 2019 ABSTRACT Aims. Two-dimensional spectroscopic data for the whole extent of the NGC 3132 planetary nebula have been obtained. We deliver a reduced data-cube and high-quality maps on a spaxel-by-spaxel basis for the many emission lines falling within the Multi-Unit Spectroscopic Explorer (MUSE) spectral coverage over a range in surface brightness >1000. Physical diagnostics derived from the emission line images, opening up a variety of scientific applications, are discussed. Methods. Data were obtained during MUSE commissioning on the European Southern Observatory (ESO) Very Large Telescope and reduced with the standard ESO pipeline. Emission lines were fitted by Gaussian profiles. The dust extinction, electron densities, and temperatures of the ionised gas and abundances were determined using Python and PyNeb routines. 2 Results. The delivered datacube has a spatial size of 6300 12300, corresponding to 0:26 0:51 pc for the adopted distance, and ∼ × ∼ 1 × a contiguous wavelength coverage of 4750–9300 Å at a spectral sampling of 1.25 Å pix− . The nebula presents a complex reddening structure with high values (c(Hβ) 0:4) at the rim. -
Planetary Nebula Associations with Star Clusters in the Andromeda Galaxy Yasmine Kahvaz [email protected]
Marshall University Marshall Digital Scholar Theses, Dissertations and Capstones 2016 Planetary Nebula Associations with Star Clusters in the Andromeda Galaxy Yasmine Kahvaz [email protected] Follow this and additional works at: http://mds.marshall.edu/etd Part of the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Kahvaz, Yasmine, "Planetary Nebula Associations with Star Clusters in the Andromeda Galaxy" (2016). Theses, Dissertations and Capstones. 1052. http://mds.marshall.edu/etd/1052 This Thesis is brought to you for free and open access by Marshall Digital Scholar. It has been accepted for inclusion in Theses, Dissertations and Capstones by an authorized administrator of Marshall Digital Scholar. For more information, please contact [email protected], [email protected]. PLANETARY NEBULA ASSOCIATIONS WITH STAR CLUSTERS IN THE ANDROMEDA GALAXY A thesis submitted to the Graduate College of Marshall University In partial fulfillment of the requirements for the degree of Master of Physical and Applied Science in Physics by Yasmine Kahvaz Approved by Dr. Timothy Hamilton, Committee Chairperson Dr. Maria Babiuc Hamilton Dr. Ralph Oberly Marshall University Dec 2016 ACKNOWLEDGEMENTS I would like to thank my advisor, Dr. Timothy Hamilton at Shawnee State University, for his guidance, advice and support for all the aspects of this project. My committee, including Dr. Timothy Hamilton, Dr. Maria Babiuc Hamilton, and Dr. Ralph Oberly, provided a review of this thesis. This research has made use of the following databases: The Local Group Survey (low- ell.edu/users/massey/lgsurvey.html) and the PHAT Survey (archive.stsci.edu/prepds/phat/). I would also like to thank the entire faculty of the Physics Department of Marshall University for being there for me every step of the way through my undergrad and graduate degree years. -
Pos(Westerbork)006 S 4.0 International License (CC BY-NC-ND 4.0)
Exploring the time-varying Universe PoS(Westerbork)006 Richard Strom ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] Lodie Voûte ASTRON, Anton Pannekoek Inst. Of Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands E-mail: [email protected] Benjamin Stappers School of Phys. & Astron., Alan Turing Bldg., University of Manchester, Oxford Road, Manchester M13 9PL, UK E-mail: [email protected] Gemma Janssen ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] Jason Hessels ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] 50 Years Westerbork Radio Observatory, A Continuing Journey to Discoveries and Innovations Richard Strom, Arnold van Ardenne, Steve Torchinsky (eds) Published with permission of the Netherlands Institute for Radio Astronomy (ASTRON) under the terms of the Creative CommonsAttribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Exploring the time-varying Universe Chapter 5.1 The earliest start Richard Strom* Introduction The WSRT interferometrically measures Fourier components of the sky bright- ness distribution from a region set by the primary beam of the telescope ele- ments, at a radio frequency determined by the receiver. This information is used to construct a two-dimensional image of radio emission from the piece of sky observed. Because it is an east-west interferometer array, the information obtained at any instant of time can only be used to construct a one-dimensional map (the telescope so synthesized has the response of a fan beam – narrow in one direction, but orthogonally very elongated). -
Size and Scale Attendance Quiz II
Size and Scale Attendance Quiz II Are you here today? Here! (a) yes (b) no (c) are we still here? Today’s Topics • “How do we know?” exercise • Size and Scale • What is the Universe made of? • How big are these things? • How do they compare to each other? • How can we organize objects to make sense of them? What is the Universe made of? Stars • Stars make up the vast majority of the visible mass of the Universe • A star is a large, glowing ball of gas that generates heat and light through nuclear fusion • Our Sun is a star Planets • According to the IAU, a planet is an object that 1. orbits a star 2. has sufficient self-gravity to make it round 3. has a mass below the minimum mass to trigger nuclear fusion 4. has cleared the neighborhood around its orbit • A dwarf planet (such as Pluto) fulfills all these definitions except 4 • Planets shine by reflected light • Planets may be rocky, icy, or gaseous in composition. Moons, Asteroids, and Comets • Moons (or satellites) are objects that orbit a planet • An asteroid is a relatively small and rocky object that orbits a star • A comet is a relatively small and icy object that orbits a star Solar (Star) System • A solar (star) system consists of a star and all the material that orbits it, including its planets and their moons Star Clusters • Most stars are found in clusters; there are two main types • Open clusters consist of a few thousand stars and are young (1-10 million years old) • Globular clusters are denser collections of 10s-100s of thousand stars, and are older (10-14 billion years -
Discovering Milky Way HII Regions
Discovering Milky Way HII Regions Tom Bania Institute for Astrophysical Research Department of Astronomy Boston University GBT HRDS Green Bank Telescope HII Region Discovery Survey AO HRDS AreciBo OBservatory HII Region Discovery Survey SHRDS Southern HII Region Discovery Survey Milky Way H II Regions HII regions are zones of ionizeD gas surrounDing O anD B type stars (Masses > 8 M¤ ) l Lifetimes <10 Myr → Trace star formation at present epoch Emit at radio wavelengths via Bremsstrahlung (free-free) continuum and radio recomBination line (RRL) emission → Thermal plasma emission mechanisms Emit at infrared (IR) due to presence of dust → The Brightest oBjects in the Galaxy at radio and IR wavelengths! The signature of HII regions is a high IR anD raDio flux H II Regions anD Galaxies The GBT Galactic H II Region Discovery Survey T.M. Bania (Boston University), L. D. Anderson (West Virginia University) Dana S. Balser (NRAO), and RoBert T. Rood (University of Virginia) GBT HRDS CollaBorators NormalizeD to Age 30 Tom Bania (Boston University) Dana Balser (NRAO) BoB RooD (University of Virginia) Loren Anderson (West Virginia University) H II Region Surveys Eagle NeBula NGC 6611 M 16 S 49 RCW 165 Gum 83 “Pillars of Creation” POSS RaDio Continuum Surveys Dwingeloo 25 m telescope 1390 MHz Westerhout (1958) RaDio RecomBination Lines (RRLs) H109α Antenna Temperature Antenna Frequency HoglunD & Mezger (1965) RaDio Wavelength Sky Surveys Continuum surveys Began in the 1950s Recombination line surveys Began in the 1960s MPIfR W43 100 m 4.875 GHz Altenhoff -
Interstellar Medium (ISM)
Interstellar Medium (ISM) Interstellar gas and dust Constituents of the ISM 60 40 15 Gas radiation field (CMB, ~ 1eV cm-3 various starlight, dust) ISM is very dilute, far from LTE Because the density of the ISM is extremely low, par>cles have a large mean free path 1 1 cm 3 λ 1015 − cm mfp ≈ n σ ≈ n H c H 3 Typical par>cle velocity: m v2 = k T 2 H B The collision >me scale is then: 1/2 1 λ T − n − τ 1.3 1011 H s c ≈ v ≈ × K 1 cm 3 − -3 Adop>ng T=100 K, nH=1 cm , we obtain about 1 collision in 500 years Local thermodynamic equilibrium (LTE) requires all species, including ions, electrons neutrals, and photons collide with each other sufficiently frequently. LTE applies inside the stars, NOT in the dilute ISM The mul>-phase interstellar gas • The various gas phases exist in pressure equilibrium: 3 4 3 n T 10 10 Kcm− · ≈ − (Kim et al. 1998) • The existence of a mul>-phase medium requires that energy flows through the system, e.g., by injec>on of energy through supernova explosions and/or stellar winds • The hot gas from SN explosions and stellar winds fills a large frac>on of the interstellar space, compressing the HI and molecular gas into a filamentary, fractal structure. Distribu>on of HI gas in the Large Magellanic Cloud Material Flow and Energy Balance of the ISM Infall from the 1 0.5M yr− intergalactic ∼ ⊙ Stars extragalactic medium gravitational and photons nuclear energies ISM 7 109M ∼ × ⊙ starlight stellar ejecta Star formation stellar winds photons kinetic energy 1 supernovae 1.3M yr− 1 ∼ ⊙ 0.5M yr− ISM ∼ ⊙ kinetic, thermal, chemical, STARS magnetic, gravitational and cosmic ray energies 1 0.2M yr− ∼ ⊙ radiative cooling stellar remnants extragalactic sky Abundance of elements in the solar neighborhood Hydrogen Asplund et al. -
Activity 3: Nebulas - 1 Where Stars Are Born
Day 2: Stars and constellations Activity 3: Nebulas - 1 Where Stars Are Born Introduction A nebula is an interstellar cloud of dust and gas. Some nebulas are called “star nurseries” because that’s where stars are formed, or "born." Our own Sun was born 4.6 billion years ago! Supplies (for each child) • Clear glass jar with a lid • Plastic spoon • Water • Tempera paint (at least 2 colors, blues, purples, and pinks work well) • Glitter • Cotton balls (about 18 per child, depending on the size of the jar) Get kids thinking In this activity, kids will create a model of a nebula. A nebula looks like a big cloud of dust and gas located in interstellar space. They are very far away — the closest one to Earth is called the Helix Nebula and it is 700 light years away. That means even if you could travel at the speed of light, it would take you 700 years to get there! Ask kids: If nebulas are so far away, how do we know what they look like? Astronomers use very powerful space telescopes, such as the Hubble telescope, to take pictures of nebulas. Share photographs of the Helix Nebula and the Orion Nebula (see pages 17-18). If you have access to the Internet, watch this video from NASA, Flight Through the Orion Nebula. https://www.smithsonianmag.com/smart-news/take-trip-through-orion-nebula-nasas-awe- some-video-1-180967825/ 16 Day 2: Stars and constellations Activity 3: Nebulas - 1 Where Stars Are Born Helix Nebula 17 Day 2: Stars and constellations Activity 3: Nebulas - 1 Where Stars Are Born Orion Nebula On a clear night, if you look at the constellation Orion, you might get a glimpse of a star nursery.