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Nature, 451, 802, 2008
Vol 451 | 14 February 2008 | doi:10.1038/nature06602 LETTERS Discovery of the progenitor of the type Ia supernova 2007on Rasmus Voss1,2 & Gijs Nelemans3 Type Ia supernovae are exploding stars that are used to measure On 2007 November 5, supernova SN2007on was found in the the accelerated expansion of the Universe1,2 and are responsible for outskirts of the elliptical galaxy NGC 140419. Optical spectra of the most of the iron ever produced3. Although there is general agree- supernova20 showed that the supernova was of type Ia. The position ment that the exploding star is a white dwarf in a binary system, of the supernova, at RA 5 03 h 38 m 50.9 s, dec. 5235u 349 300 the exact configuration and trigger of the explosion is unclear4, (J2000), is about 700 from the core of the host, corresponding to which could hamper their use for precision cosmology. Two fam- 8 kpc for a distance of 20 Mpc to NGC 140421. Observations by the ilies of progenitor models have been proposed. In the first, a white SWIFT mission on November 11 detected the supernova in the dwarf accretes material from a companion until it exceeds the optical/ultraviolet monitor but not in the X-ray telescope22. We ana- Chandrasekhar mass, collapses and explodes5,6. Alternatively, lysed the SWIFT data and determined the position of the supernova two white dwarfs merge, again causing catastrophic collapse and as RA 5 03 h 38 m 50.98 s, dec. 5235u 349 31.00 (J2000), with uncer- an explosion7,8. It has hitherto been impossible to determine if tainty of 10 (Fig. -
Dark Matter Thermonuclear Supernova Ignition
MNRAS 000,1{21 (2019) Preprint 1 January 2020 Compiled using MNRAS LATEX style file v3.0 Dark Matter Thermonuclear Supernova Ignition Heinrich Steigerwald,1? Stefano Profumo,2 Davi Rodrigues,1 Valerio Marra1 1Center for Astrophysics and Cosmology (Cosmo-ufes) & Department of Physics, Federal University of Esp´ırito Santo, Vit´oria, ES, Brazil 2Department of Physics and Santa Cruz Institute for Particle Physics, 1156 High St, University of California, Santa Cruz, CA 95064, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We investigate local environmental effects from dark matter (DM) on thermonuclear supernovae (SNe Ia) using publicly available archival data of 224 low-redshift events, in an attempt to shed light on the SN Ia progenitor systems. SNe Ia are explosions of carbon-oxygen (CO) white dwarfs (WDs) that have recently been shown to explode at sub-Chandrasekhar masses; the ignition mechanism remains, however, unknown. Recently, it has been shown that both weakly interacting massive particles (WIMPs) and macroscopic DM candidates such as primordial black holes (PBHs) are capable of triggering the ignition. Here, we present a method to estimate the DM density and velocity dispersion in the vicinity of SN Ia events and nearby WDs; we argue that (i) WIMP ignition is highly unlikely, and that (ii) DM in the form of PBHs distributed according to a (quasi-) log-normal mass distribution with peak log10¹m0/1gº = 24:9±0:9 and width σ = 3:3 ± 1:0 is consistent with SN Ia data, the nearby population of WDs and roughly consistent with other constraints from the literature. -
Lunar Portrait Rick Bria Captured This Image of the Moon with a 76Mm Televue Refractor and a Canon T1i (In Video Mode) on September 15, 2010
WESTCHESTER AMATEUR ASTRONOMERS NOVEMBER 2010 Sky tch Lunar Portrait Rick Bria captured this image of the Moon with a 76mm Televue Refractor and a Canon T1i (in video mode) on September 15, 2010. The image is a 212 digital stack from a video containing thousands of frames. It was processed in Registax 5 and Photoshop CS5. Notes Rick: A quick look confirms that the Moon has been bombarded with asteroid impacts. These impact craters are a record of the violent conditions in our early solar system. Billions of years ago asteroids hit the Earth, and the Moon with tremendous force, blasting out craters. Since the Moon has no wind, rain, or plate tectonics, its craters remain to this day for us to study. The Earth has about one hundred craters that still can be seen (some from Google Earth) compared to the Moon which has about thirty thousand craters. ANNUAL ELECTION It's election time for the Westchester Amateur Astronomers. Please print out the Ballot on Page 8 of this issue, mark your votes, and then bring it to the November 5th meeting or mail to the Club at WAA, PO Box 44, Valhalla, NY 10595 postmarked no later than November 15th. SERVING THE ASTRONOMY COMMUNITY SINCE 1983 Page 1 WESTCHESTER AMATEUR ASTRONOMERS NOVEMBER 2010 Events for November 2010 WAA Lectures Renewing Members. “The Discovery of Supernova 2008ha" Frank Jones - New Rochelle Friday November 5th, 8:00pm Olivier Prache - Pleasantville Miller Lecture Hall, Pace University Tom Boustead - White Plains Pleasantville, NY Rosalind Mendell - Hartsdale Caroline Moore will speak on her discovery of a rare Scott Nammacher - White Plains supernova. -
Bad Habits Asserting Themselves How a Mild Virus Might Turn
Bad Habits Asserting Themselves 3 How a Mild Virus Might Turn Vicious 5 At Last, Facing Down Bullies (and Their Enablers) 7 Is This a Pandemic? Define ‘Pandemic’ 9 Letting the Patient Call the Shots 12 Rotavirus: Every Child Should Be Vaccinated Against Diarrheal Disease, W.H.O. Says 15 1984 thoughtcrime? Does it matter that George Orwell pinched the plot? 16 Diabetes warning signs detected 18 Rogue protein 'spreads in brain' 20 Oily fish 'can halt eye disease' 22 Australia wind farm gets go-ahead 24 Chimps mentally map fruit trees 26 Mobile scanner could detect guns 28 Girls 'hampered by failure fears' 31 Animal Mating Choices More Complex Than Once Thought 33 Hundreds Of Cell-surface Proteins Can Be Simultaneously Studied With New Technique 35 Self-regulation Game Predicts Kindergarten Achievement 38 Prehistoric Complex Including Two 6,000-year-old Tombs Discovered In Britain 39 Fat In Mammalian Cells May Help Explain How Toxin Harms Farm Animals 41 Is Rural Land Use Too Important To Be Left To Farmers? 42 Drinking Water From Air Humidity 43 Cantabrian Cornice Has Experienced Seven Cooling Phases Over Past 41,000 Years 44 Prehistoric Whale Discovered On The West Coast Of Sweden 46 Nanoscale Zipper Cavity Responds To Single Photons Of Light 47 Television Watching Before Bedtime Can Lead To Sleep Debt 50 'Warrior Gene' Linked To Gang Membership, Weapon Use 51 Basket Weaving May Have Taught Humans To Count 53 Archaeologists Locate Confederate Cannons, Naval Yard 55 Flexible Solar Power Shingles Transform Roofs From Wasted Space To Energy -
Probes of the Supernova Engine Chris Fryer (LANL) for LANL Multi- Messenger Team, LANL Light-Curve Team, Nugrid Collaboration
Probes of the Supernova Engine Chris Fryer (LANL) for LANL Multi- Messenger team, LANL light-curve team, NuGrid collaboration Direct Probes of the SN Engine • Neutrinos • Gravitational Waves Indirect Probes • Progenitors • Light Curves • Ejecta Remnants • Compact Remnants • Nucleosynthetic Yields Supernova 1987A After – SN 1987A Before – Sanduleak -69 202 Neutrino-Driven Supernova Mechanism Temperature and Density of the Core Becomes so High that: Iron dissociates into alpha particles Electrons capture onto protons Core collapses nearly at freefall! Velocity (c) Velocity Radius (km) Core reaches nuclear densities! Velocity (c) Velocity Nuclear forces and neutron! degeneracy increase pressure! Bounce!! Radius (km) Neutrino-Driven Supernova Mechanism: Convection Fryer 1999 Anatomy Of the Convection Region Proto- Neutron Star Upflow Accretion Shock Downflow Fryer & Warren 2002 Neutrinos • Neutrinos probe the structure of the core and the behavior of matter at nuclear densities (e.g. Roberts et al. 2012, Reddy et al. 2012). • With modern detectors, a Galactic supernova could be used to probe neutrino physics such as neutrino Flavor-State Coupling (Duan & Friedland 2011) oscillations. Gravitational Waves Fryer et al. 2004 • One of the uncertainties limiting what we can learn from neutrinos is the core rotation. • Gravitational Waves are direct probes of this rotation. Gravitational Waves • For a sufficiently strong signal, we could even probe the nature of the convection. • Unfortunately, even with the next generation of detectors, such detailed neutrino and gravitational wave signals are limited to Galactic (or local Murphy et al. 2009 group) supernovae. Indirect Probes • With indirect probes, we will have to use theory to connect the observations to the physics we want to study. -
Explaining Iptf14hls As a Common Envelope Jets Supernova
MNRAS 000, 1–5 (2017) Preprint 20 December 2017 Compiled using MNRAS LATEX style file v3.0 Explaining iPTF14hls as a common envelope jets supernova Noam Soker1⋆, Avishai Gilkis2† 1 Department of Physics, Technion – Israel Institute of Technology, Haifa 3200003, Israel 2 Institute of Astronomy, University of Cambridge, Madingley Rise, Cambridge, CB3 0HA, UK 20 December 2017 ABSTRACT We propose a common envelope jets supernova scenario for the enigmatic supernova iPTF14hls where a neutron star that spirals-in inside the envelope of a massive giant star accretes mass and launches jets that power the ejection of the circumstellar shell and a few weeks later the explosion itself. To account for the kinetic energy of the circumstellar gas and the explosion, the neutron star should accrete a mass of ≈ 0.3M⊙. The tens×M⊙ of circumstellar gas that accounts for some absorption lines is ejected while the neutron star orbits for about one to several weeks inside the envelope of the giant star. In the last hours of the interaction the neutron star merges with the core, accretes mass, and launches jets that eject the core and the inner envelope to form the explosion itself and the medium where the supernova photosphere resides. The remaining neutron star accretes fallback gas and further powers the supernova. We attribute the 1954 pre-explosion outburst to an eccentric orbit and temporary mass accretion by the neutron star at periastron passage prior to the onset of the common envelope phase. Key words: stars: jets — supernovae: general — binaries: close 1 INTRODUCTION cases, in iPFT14hls there is no evidence for ejecta-CSM col- lision. -
Light Curve Powering Mechanisms of Superluminous Supernovae
Light Curve Powering Mechanisms of Superluminous Supernovae A dissertation presented to the faculty of the College of Arts and Science of Ohio University In partial fulfillment of the requirements for the degree Doctor of Philosophy Kornpob Bhirombhakdi May 2019 © 2019 Kornpob Bhirombhakdi. All Rights Reserved. 2 This dissertation titled Light Curve Powering Mechanisms of Superluminous Supernovae by KORNPOB BHIROMBHAKDI has been approved for the Department of Physics and Astronomy and the College of Arts and Science by Ryan Chornock Assistant Professor of Physics and Astronomy Joseph Shields Interim Dean, College of Arts and Science 3 Abstract BHIROMBHAKDI, KORNPOB, Ph.D., May 2019, Physics Light Curve Powering Mechanisms of Superluminous Supernovae (111 pp.) Director of Dissertation: Ryan Chornock The power sources of some superluminous supernovae (SLSNe), which are at peak 10{ 100 times brighter than typical SNe, are still unknown. While some hydrogen-rich SLSNe that show narrow Hα emission (SLSNe-IIn) might be explained by strong circumstellar interaction (CSI) similar to typical SNe IIn, there are some hydrogen-rich events without the narrow Hα features (SLSNe-II) and hydrogen-poor ones (SLSNe-I) that strong CSI has difficulties to explain. In this dissertation, I investigate the power sources of these two SLSN classes. SN 2015bn (SLSN-I) and SN 2008es (SLSN-II) are the targets in this study. I perform late-time multi-wavelength observations on these objects to determine their power sources. Evidence supports that SN 2008es was powered by strong CSI, while the late-time X-ray non-detection we observed neither supports nor denies magnetar spindown as the most preferred power origin of SN 2015bn. -
Gravitational-Wave Radiation from Merging Binary Black Holes and Supernovae
Gravitational-wave radiation from merging binary black holes and Supernovae I. Kamaretsos Submitted for the degree of Doctor of Philosophy School of Physics and Astronomy Cardiff University October 2012 Declaration of authorship • Declaration: This work has not previously been accepted in substance for any degree and is not concurrently submitted in candidature for any degree. Signed: :::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::: (candidate) Date: ::::::::::::::::::: • Statement 1: This thesis is being submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (PhD). Signed: :::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::: (candidate) Date: ::::::::::::::::::: • Statement 2: This thesis is the result of my own independent work/investigation, except where otherwise stated. Other sources are acknowledged by explicit refer- ences. Signed: :::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::: (candidate) Date: ::::::::::::::::::: • Statement 3 I hereby give consent for my thesis, if accepted, to be available for photo- copying and for inter-library loan, and for the title and summary to be made available to outside organisations. Signed: :::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::::: (candidate) Date: ::::::::::::::::::: i Summary of thesis This thesis is conceptually divided into two parts. The first and main part concerns the generation of gravitational radiation that is emitted from merging black-hole binary systems using Numerical Relativity -
The Carnegie Supernova Project. I. Third Photometry Data Release of Low-Redshift Type Ia Supernovae and Other White Dwarf Explosions
The Astronomical Journal, 154:211 (34pp), 2017 November https://doi.org/10.3847/1538-3881/aa8df0 © 2017. The American Astronomical Society. All rights reserved. The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions Kevin Krisciunas1 , Carlos Contreras2,3, Christopher R. Burns4 , M. M. Phillips2 , Maximilian D. Stritzinger2,3 , Nidia Morrell2 , Mario Hamuy5, Jorge Anais2, Luis Boldt2, Luis Busta2 , Abdo Campillay2, Sergio Castellón2, Gastón Folatelli2,6, Wendy L. Freedman4,7, Consuelo González2, Eric Y. Hsiao2,3,8 , Wojtek Krzeminski2,17, Sven Eric Persson4 , Miguel Roth2,9, Francisco Salgado2,10 , Jacqueline Serón2,11, Nicholas B. Suntzeff1, Simón Torres2,12, Alexei V. Filippenko13,14 , Weidong Li13,17, Barry F. Madore4,15 , D. L. DePoy1, Jennifer L. Marshall1 , Jean-Philippe Rheault1, and Steven Villanueva1,16 1 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA; [email protected] 2 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 3 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 4 Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA 5 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile 6 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Instituto de Astrofísica de La Plata (IALP), CONICET, Paseo del Bosque S/N, B1900FWA La Plata, Argentina 7 Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA 8 Department of Physics, Florida State University, Tallahassee, FL 32306, USA 9 GMTO Corporation, Avenida Presidente Riesco 5335, Suite 501, Las Condes, Santiago, Chile 10 Leiden Observatory, Leiden University, P.O. -
How Rapidly Do Neutron Stars Spin at Birth? Constraints from Archival X
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 November 2018 (MN LATEX style file v2.2) How rapidly do neutron stars spin at birth? Constraints from archival X-ray observations of extragalactic supernovae Rosalba Perna1, Roberto Soria2, Dave Pooley3, Luigi Stella4 1 JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO, 80309 2 MSSL, University College London, Holmbury St mary, Dorking RH5 6NT, UK 3 Astronomy Department, University of Wisconsin-Madison 475 North Charter st., Madison, WI 53706, USA 4 INAF - Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Rome, Italy 1 November 2018 ABSTRACT Traditionally, studies aimed at inferring the distribution of birth periods of neu- tron stars are based on radio surveys. Here we propose an independent method to constrain the pulsar spin periods at birth based on their X-ray luminosities. In par- ticular, the observed luminosity distribution of supernovae poses a constraint on the initial rotational energy of the embedded pulsars, via the LX − E˙ rot correlation found for radio pulsars, and under the assumption that this relation continues to hold beyond the observed range. We have extracted X-ray luminosities (or limits) for a large sample of historical SNe observed with Chandra, XMM and Swift, that have been firmly clas- sified as core-collapse supernovae. We have then compared these observational limits with the results of Monte Carlo simulations of the pulsar X-ray luminosity distribu- tion, for a range of values of the birth parameters. We find that a pulsar population dominated by millisecond periods at birth is ruled out by the data. -
A Series of Energetic Eruptions Leading to a Peculiar H-Rich Explosion of a Massive Star
A series of energetic eruptions leading to a peculiar H-rich explosion of a massive star Iair Arcavi1;2;3;4, D. Andrew Howell1;3, Daniel Kasen5;7;8, Lars Bildsten2;3, Griffin Hosseinzadeh1;3, Curtis McCully1;3, Zheng Chuen Wong1;3, Sarah Rebekah Katz1;3, Avishay Gal-Yam9, Jesper Sollerman10, Francesco Taddia10, Giorgos Leloudas9;11, Christoffer Fremling10, Peter E. Nugent6;8, Assaf Horesh12;9, Kunal Mooley13, Clare Rumsey14, S. Bradley Cenko15;16, Melissa L. Graham17;7;8, Daniel A. Perley11, Ehud Nakar18, Nir J. Shaviv12, Omer Bromberg18, Ken J. Shen7;8, Eran O. Ofek9, Yi Cao19, Xi- aofeng Wang20, Fang Huang20, Liming Rui20, Tianmeng Zhang21, Wenxiong Li20, Zhitong Li20, Jujia Zhang22;23, Stefano Valenti24, David Guevel1;3, Benjamin Shappee25;26, Christopher S. Kochanek27;28, Thomas W.-S. Holoien27;28, Alexei V.Filippenko7;8, Rob Fender13, Anders Nyholm10, Ofer Yaron9, Mansi M. Kasliwal19, Mark Sullivan29, Nadja Blagorodnova19, Richard S. Walters19, Ragnhild Lunnan19, Danny Khazov9, Igor Andreoni30;31;32, Russ R. Laher33, Nick Konidaris34, Przemek Wozniak35 and Brian Bue36 1Las Cumbres Observatory, Goleta, CA 93117, USA 2Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 3Department of Physics, University of California, Santa Barbara, CA 93106, USA 4Einstein Fellow 5Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA 6Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA 7Department of Physics, University of California, -
Supernovae Without Host Galaxy?-Hypervelocity Stars In
Astronomy & Astrophysics manuscript no. hypervelocity-stars˙langcor c ESO 2018 November 7, 2018 Supernovae without host galaxies? Hypervelocity stars in foreign galaxies Peter-Christian Zinn1, Philipp Grunden1, and Dominik J. Bomans1 Astronomical Institute, Ruhr-University Bochum, Universit¨atsstraße 150, D-44801 Bochum e-mail: [email protected] Received 05/07/2011; accepted 14/09/2011 ABSTRACT Context. Harvesting the SAI supernova catalog, the most complete list of supernovae (SNe) currently available, we search for SNe that apparently do not occur within a distinct host galaxy but lie a great distance (several arcmin) apart from the host galaxy given in the catalog or even show no sign of an identifiable galaxy in their direct vicinity. Aims. We attempt to distinguish between two possible explanations of this host-lessness of a fraction of reported SNe, namely (i) that a host galaxy is too faint (of too low surface brightness) to be detected within the limits of currently available surveys (presumably a low surface brightness galaxy) or (ii) a hypervelocity star (HVS) is the progenitor of the SN that exploded kiloparsecs away from its host galaxy. Methods. We use deep imaging to test the first explanation. If no galaxy is identified within our detection limit of ∼ 27 mag arcsec2, which is the central surface brightness of the faintest known LSB galaxy so far, we discard this explanation and propose that the SN, after several other checks, had a hypervelocity star progenitor. We focus on observations for which this is the case and give lower limits to the actual space velocities of the progenitors, making them the first hypervelocity stars known in galaxies other than our own Milky Way.