THE MISSING LINK in GRAVITATIONAL-WAVE ASTRONOMY: Discoveries Waiting in the Decihertz Range
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October 2020 Deirdre Shoemaker, Ph.D. Center for Gravitational Physics Department of Physics University of Texas at Austin Google Scholar
October 2020 Deirdre Shoemaker, Ph.D. Center for Gravitational Physics Department of Physics University of Texas at Austin Google scholar: http://bit.ly/1FIoCFf I. Earned Degrees B.S. Astronomy & Astrophysics 1990-1994 Pennsylvania State University with Honors and Physics Ph.D. Physics 1995-1999 University of Texas at Austin (advisor: R. Matzner) II. Employment History 1999-2002 Postdoctoral Fellow, Center for Gravitational Wave Physics, Penn State (advisor: S. Finn and J. Pullin) 2002-2004 Research Associate, Center for Radiophysics and Space Research, Cornell (advisor: S. Teukolsky) 2004-2008 Assistant Professor, Physics, Penn State 2008-2011 Assistant Professor, Physics, Georgia Institute of Technology 2009-2011 Adjunct Assistant Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2011-2016 Associate Professor, Physics, Georgia Institute of Technology 2011-2016 Adjunct Associate Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2013-2020 Director, Center for Relativistic Astrophysics 2016-2020 Professor, Physics, Georgia Institute of Technology 2016-2020 Adjunct Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2017-2020 Associate Director of Research and Strategic Initiatives, Institute of Data, Engineering and Science, Georgia Institute of Technology 2020-Present Professor, Physics, University of Texas at Austin 2020-Present Director, Center for Gravitational Physics, University of Texas at Austin III. Honors -
Phase Transitions and Gravitational Wave Tests of Pseudo-Goldstone Dark Matter in the Softly Broken Uð1þ Scalar Singlet Model
PHYSICAL REVIEW D 99, 115010 (2019) Phase transitions and gravitational wave tests of pseudo-Goldstone dark matter in the softly broken Uð1Þ scalar singlet model † Kristjan Kannike* and Martti Raidal National Institute of Chemical Physics and Biophysics, Rävala 10, Tallinn 10143, Estonia (Received 26 February 2019; published 10 June 2019) We study phase transitions in a softly broken Uð1Þ complex singlet scalar model in which the dark matter is the pseudoscalar part of a singlet whose direct detection coupling to matter is strongly suppressed. Our aim is to find ways to test this model with the stochastic gravitational wave background from the scalar phase transition. We find that the phase transition which induces vacuum expectation values for both the Higgs boson and the singlet—necessary to provide a realistic dark matter candidate—is always of the second order. If the stochastic gravitational wave background characteristic to a first order phase transition will be discovered by interferometers, the soft breaking of Uð1Þ cannot be the explanation to the suppressed dark matter-baryon coupling, providing a conclusive negative test for this class of singlet models. DOI: 10.1103/PhysRevD.99.115010 I. INTRODUCTION Is there any other way to test the softly broken Uð1Þ Scalar singlet is one of the most generic candidates for singlet DM model experimentally and to distinguish the the dark matter (DM) of the Universe [1,2], whose proper- particular model from more general versions of singlet scalar ties have been exhaustively studied [3–6] (see [7,8] for a DM? A new probe of physics beyond the Standard Model recent review and references). -
Observing Primordial Gravitational Waves Below the Binary-Black-Hole-Produced Stochastic Background
Digging Deeper: Observing Primordial Gravitational Waves below the Binary-Black-Hole-Produced Stochastic Background The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Regimbau, T. et al. “Digging Deeper: Observing Primordial Gravitational Waves below the Binary-Black-Hole-Produced Stochastic Background.” Physical Review Letters 118.15 (2017): n. pag. © 2017 American Physical Society As Published http://dx.doi.org/10.1103/PhysRevLett.118.151105 Publisher American Physical Society Version Final published version Citable link http://hdl.handle.net/1721.1/108853 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. week ending PRL 118, 151105 (2017) PHYSICAL REVIEW LETTERS 14 APRIL 2017 Digging Deeper: Observing Primordial Gravitational Waves below the Binary-Black-Hole-Produced Stochastic Background † ‡ T. Regimbau,1,* M. Evans,2 N. Christensen,1,3, E. Katsavounidis,2 B. Sathyaprakash,4, and S. Vitale2 1Artemis, Université Côte d’Azur, CNRS, Observatoire Côte d’Azur, CS 34229, Nice cedex 4, France 2LIGO, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA 3Physics and Astronomy, Carleton College, Northfield, Minnesota 55057, USA 4Department of Physics, The Pennsylvania State University, University Park, Pennsylvania 16802, USA and School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom (Received 25 November 2016; revised manuscript received 9 February 2017; published 14 April 2017) The merger rate of black hole binaries inferred from the detections in the first Advanced LIGO science run implies that a stochastic background produced by a cosmological population of mergers will likely mask the primordial gravitational wave background. -
Physical Review D
PHYSICAL REVIEW D PERIODICALS For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 99, NUMBER 12 CONTENTS D15 JUNE 2019 The Table of Contents is a total listing of Parts A and B. Part A consists of articles 121301–124004, and Part B articles 124005–126016(A) PART A RAPID COMMUNICATIONS Equation of state of dense matter in the multimessenger era (6 pages) .......................................................... 121301(R) Ying Zhou, Lie-Wen Chen, and Zhen Zhang Dark matter decaying in the late Universe can relieve the H0 tension (6 pages) ............................................... 121302(R) Kyriakos Vattis, Savvas M. Koushiappas, and Abraham Loeb Steady flows, nonlinear gravitostatic waves, and Zeldovich pancakes in a Newtonian gas (6 pages) ....................... 121303(R) Eugene B. Kolomeisky Constraint of void bias on primordial non-Gaussianity (7 pages) ................................................................. 121304(R) Kwan Chuen Chan, Nico Hamaus, and Matteo Biagetti New constraint from supernova explosions on light particles beyond the Standard Model (6 pages) ....................... 121305(R) Allan Sung, Huitzu Tu, and Meng-Ru Wu ARTICLES Constraints on the ultrahigh-energy cosmic neutrino flux from the fourth flight of ANITA (11 pages) .................... 122001 P. W. Gorham et al. (ANITA Collaboration) Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run (20 pages) .... 122002 B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration) LISA Pathfinder micronewton cold gas thrusters: In-flight characterization (10 pages) ....................................... 122003 M. Armano et al. (LISA Pathfinder Collaboration) Observation of seasonal variation of atmospheric multiple-muon events in the NOvA Near Detector (11 pages) ....... -
Observational Signatures from Tidal Disruption Events of White Dwarfs
Doctoral Dissertation 博士論文 Observational signatures from tidal disruption events of white dwarfs (白色矮星の潮汐破壊現象からの観測兆候) A Dissertation Submitted for the Degree of Doctor of Philosophy December 2020 令和 2 年 12 月 博士(理学)申請 Department of Physics, Graduate School of Science, The University of Tokyo 東京大学大学院理学系研究科物理学専攻 Kojiro Kawana 川名 好史朗 i Abstract Recent advances in optical surveys have yielded a large sample of astronomical transients, including classically known novae and supernovae (SNe) and also newly discovered classes of transients. Among them, tidal disruption events (TDEs) have a unique feature that they can probe massive black holes (MBHs). A TDE is an event where a star approaching close to a BH is disrupted by tides of the BH. The disrupted star leaves debris bound to the BH emitting multi-wavelength and multi-messenger signals, which are observed as a transient. The observational signatures of TDEs bring us insights into physical processes around the BH, such as dynamics in the general relativistic gravity, accretion physics, and environmental information around BHs. Event rates of TDEs also inform us of populations of BHs. A large number of BHs have been detected, but still there are big mysteries. The most mysterious BHs are intermediate mass BHs (IMBHs) because they are a missing link: there is almost no certain evidence of IMBHs, while there are many detections of stellar mass BHs and supermassive BHs (SMBHs). Searches for IMBHs are not only important to reveal mysteries of IMBHs themselves, but also to understand origin(s) of SMBHs. Several scenarios to form SMBHs have been proposed, but it is still unclear which scenario(s) are real in the Universe. -
Stochastic Gravitational Wave Backgrounds
Stochastic Gravitational Wave Backgrounds Nelson Christensen1;2 z 1ARTEMIS, Universit´eC^oted'Azur, Observatoire C^oted'Azur, CNRS, 06304 Nice, France 2Physics and Astronomy, Carleton College, Northfield, MN 55057, USA Abstract. A stochastic background of gravitational waves can be created by the superposition of a large number of independent sources. The physical processes occurring at the earliest moments of the universe certainly created a stochastic background that exists, at some level, today. This is analogous to the cosmic microwave background, which is an electromagnetic record of the early universe. The recent observations of gravitational waves by the Advanced LIGO and Advanced Virgo detectors imply that there is also a stochastic background that has been created by binary black hole and binary neutron star mergers over the history of the universe. Whether the stochastic background is observed directly, or upper limits placed on it in specific frequency bands, important astrophysical and cosmological statements about it can be made. This review will summarize the current state of research of the stochastic background, from the sources of these gravitational waves, to the current methods used to observe them. Keywords: stochastic gravitational wave background, cosmology, gravitational waves 1. Introduction Gravitational waves are a prediction of Albert Einstein from 1916 [1,2], a consequence of general relativity [3]. Just as an accelerated electric charge will create electromagnetic waves (light), accelerating mass will create gravitational waves. And almost exactly arXiv:1811.08797v1 [gr-qc] 21 Nov 2018 a century after their prediction, gravitational waves were directly observed [4] for the first time by Advanced LIGO [5, 6]. -
Km-Scale Space Gravitational Wave Detector
Formation Flying Meetup May 9, 2019 km-scale Space Gravitational Wave Detector Yuta Michimura Department of Physics, University of Tokyo Science-Driven Approach C-DECIGO (10 kg, 10 km Fabry-Perot) Motivations • Demonstration of multiband gravitational wave detection - Detect BBHs and BNSs a few days before the merger • IMBH search with unprecedented sensitivity • km-scale space mission A. Sesana, Phys. Rev. Lett. 116, 231102 (2016) • Demonstration of interferometry and formation flight for B-DECIGO and DECIGO 3 Existing Space GW Projects LISA TianQin B-DECIGO Arm length 2.5e6 km 1.7e5 km 100 km Interferometry Optical Optical Fabry-Pérot transponder transponder cavity Laser frequency Reference cavity, Reference cavity, Iodine, 515 nm stabilization 1064 nm 1064 nm Orbit Heliocentric Geocentric, facing Geocentric (TBD) J0806.3+1527 Flight Constellation Constellation Formation flight configuration flight flight Test mass 1.96 kg 2.45 kg 30 kg Force noise req. 8e-15 N/rtHz 7e-15 N/rtHz 1e-16 N/rtHz Achieved CQG 33, 035010 (2016) PRL 120, 061101 (2018) 4 Sensitivity Comparison LISA: https://perf-lisa.in2p3.fr/ KAGRA: PRD 97, 122003 (2018) TianQin: arXiv:1902.04423 (from Yi-Ming Hu) aLIGO: LIGO-T1800044 B-DECIGO: PTEP 2016, 093E01 (2016) ET: http://www.et-gw.eu/index.php/etdsdocument CE: CQG 34, 044001 (2017) TianQin LISA KAGRA B-DECIGO ET aLIGO CE 5 Horizon Distance B-DECIGO LISA ET CE TianQin z=10 aLIGO B-DECIGO x 30 z=1 KAGRA GW150914 GW170817 Optimal direction and polarization 6 SNR threshold 8 Horizon Distance B-DECIGO LISA ET CE TianQin z=10 aLIGO B-DECIGO x 30 z=1 We can barely detect O1/O2 KAGRA binaries with B-DECIGO x 30 sensitivity GW150914 We can also search for 3 GW170817 O(10 ) Msun IMBH upto z=10 Optimal direction and polarization 7 SNR threshold 8 C-DECIGO • Target sensitivity C-DECIGO = B-DECIGO x 30 = DECIGO x 300 • For GW150914 and GW170817 like binaries, C-DECIGO can measure coalescence time to < ~150 sec a few days before the merger S. -
New Building Offers Most Advanced Technology Of
The magazine of Montclair State University MONTCLAIR Fall/Winter 2017 NEW BUILDING OFFERS MOST ADVANCED TECHNOLOGY OF ANY SCHOOL IN THE COUNTRY Alumnus Michael Price ’81, a writer and producer of The Simpsons, returned to campus at Homecoming to discuss his career with School of Communication and Media Director Keith Strudler and to dedicate the Michael Price Audio Production Center. See story in Alumni News, page 46. CONTENTS | FALL/WINTER 2017 FEATURES Poetic Justice 12 Ruth Bader Ginsburg spends day on campus, tackles The Merchant of Venice at round-table discussion Connecting Threads 17 Student mentors support personal growth of middle school boys in Newark Looking for Home Students travel to Greece to film the human stories 20 of the refugee crisis Hollywood East School of Communication and Media’s new home 24 is nation’s most technologically advanced university media production facility, rivaling professional studios Solving Cosmic Mysteries 30 Faculty on LIGO team help with historic detection of neutron stars’ collision 3 Feedback 4 Headlines 35 Athletics 41 Alumni Connections 47 Class Notes 54 In Memoriam 56 Lasting Lessons DEPARTMENTS Photo by Gennadi Novash MONTCLAIR The magazine of Montclair State University FROM President Susan A. Cole THE Vice President for University Advancement John T. Shannon Associate Vice President for PRESIDENT External Relations Carol Blazejowski ’78 n October, I had the honor of delivering the “President-to-Presidents Lecture” at Assistant Vice President for the annual meeting of the American Association of State Colleges and Universities Communications and Marketing Ellen Griffin I(AASCU), where 200 presidents and chancellors gathered to explore issues facing higher education to ensure that we, as leaders, are doing our best to provide future Assistant Vice President for generations with the tools they need to lead our country forward. -
National Science Foundation LIGO FACTSHEET NSF and the Laser Interferometer Gravitational-Wave Observatory
e National Science Foundation LIGO FACTSHEET NSF and the Laser Interferometer Gravitational-Wave Observatory In 1916, Albert What is LIGO? Einstein published the LIGO consists of two widely separated laser paper that predicted interferometers located within the United States – one gravitational waves – in Hanford, Washington, and the other in Livingston, ripples in the fabric of Louisiana – each housed inside an L-shaped, ultra-high space-time resulting vacuum tunnel. The twin LIGO detectors operate in from the most violent unison to detect gravitational waves. Caltech and MIT phenomena in our led the design, construction and operation of the NSF- universe, from funded facilities. supernovae explosions to the collision of black What are gravitational waves? holes. For 100 years, Gravitational waves are distortions of the space and that prediction has time which emit when any object that possesses mass stimulated scientists accelerates. This can be compared in some ways to how around the world who accelerating charges create electromagnetic fields (e.g. have been seeking light and radio waves) that antennae detect. To generate to directly detect gravitational waves that can be detected by LIGO, the gravitational waves. objects must be highly compact and very massive, such as neutron stars and black holes. Gravitational-wave In the 1970s, the National Science Foundation (NSF) detectors act as a “receiver.” Gravitational waves travel joined this quest and began funding the science to Earth much like ripples travel outward across a pond. and technological innovations behind the Laser However, these ripples in the fabric of space-time carry Interferometer Gravitational-Wave Observatory (LIGO), information about their violent origins and about the the instruments that would ultimately yield a direct nature of gravity – information that cannot be obtained detection of gravitational waves. -
Arxiv:2104.05033V2 [Gr-Qc] 2 May 2021 Academy of Science, Beijing, China, 100190; University of Chinese Academy of Sciences, Bei- Jing 100049, China
Mission Design for the TAIJI misson and Structure Formation in Early Universe Xuefei Gong, Shengnian Xu,Shanquan Gui, Shuanglin Huang and Yun-Kau Lau ∗ Abstract Gravitational wave detection in space promises to open a new window in astronomy to study the strong field dynamics of gravitational physics in astro- physics and cosmology. The present article is an extract of a report on a feasibility study of gravitational wave detection in space, commissioned by the National Space Science Center, Chinese Academy of Sciences almost a decade ago. The objective of the study was to explore various possible mission options to detect gravitational waves in space alternative to that of the (e)LISA mission concept and look into the requirements on the technological fronts. On the basis of relative merits and bal- ance between science and technological feasibility, a set of representative mission options were studied and in the end a mission design was recommended as the start- ing point for research and development in the Chinese Academy of Sciences. The Xuefei Gong Institute of Applied Mathematics, Academy of Mathematics and System Science, Chinese Academy of Science, Beijing, China, 100190. e-mail: [email protected] Shengnian Xu Institute of Applied Mathematics, Academy of Mathematics and System Science, Chinese Academy of Science, Beijing, China, 100190. e-mail: [email protected] Shanquan Gui School of Physical Science and Technology, Lanzhou University, Lanzhou, 730000, China; Depart- ment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China. e-mail: [email protected]. Shuanglin Huang Institute of Applied Mathematics, Academy of Mathematics and System Science, Chinese arXiv:2104.05033v2 [gr-qc] 2 May 2021 Academy of Science, Beijing, China, 100190; University of Chinese Academy of Sciences, Bei- jing 100049, China. -
LIGO- India Project by Indian Astrophysicist Mr. Karan Jani (Date
A Report on GTU ITAP & CiC3 organized Discourse on LIGO- India Project By Indian Astrophysicist Mr. Karan Jani rd (Date: 23 August 2016) About GTU ITAP ITAP & NI Gujarat Technological University (GTU) is a premier academic and research institution which has driven new ways of thinking since its 2007 founding, established by the Government of Gujarat vide Gujarat Act No. 20 of 2007. GTU is a State University with 486 affiliated colleges in its fold operating across the state of Gujarat through its FIVE zones at Ahmedabad, Gandhinagar, Vallabh Vidyanagar, Rajkot and Surat. The University caters to the fields of Engineering, Architecture, Management, Pharmacy and Computer Science. The University has about 4 lakh students enrolled in a large number of Diploma, Under Graduate, Post Graduate programs along with the robust Doctoral program. GTU is associated with Institute and Student development activity right through its inception. In the same direction GTU has established “Integrated Training & Placement (ITAP) Cell”, wings to support Institutes to enhance employability skill in students which help their students to get job and also it would help them to fit in turbulence environment. This Cell also works for development of entrepreneur skills, which helps students to established new business generate employability for society. Enhance awareness regarding corporate professionalism Enhance soft skills and Employability skills Development of Entrepreneurship skill of students Specific focus on how stakeholders (Students) will able to fit with today’s turbulence Environment of corporate. GTU Integrated Training & Placement (ITAP) and Community Innovation & Co-Creation Centre (CiC3) has collaboratively organized a Discourse on LIGO (Laser Interferometer Gravitational-Wave Observatory) for India Project by renowned Indian Astrophysicist Mr Karan Jani. -
Forecasts on the Speed of Gravitational Waves at High Ζ
Prepared for submission to JCAP Forecasts on the speed of gravitational waves at high z Alexander Bonillaa, Rocco D'Agostinob;c, Rafael C. Nunesd, Jos´e C. N. de Araujod aDepartamento de F´ısica,Universidade Federal de Juiz de Fora, 36036-330, Juiz de Fora, MG, Brazil. bDipartimento di Fisica, Universit`adi Napoli \Federico II", Via Cinthia 21, I-80126, Napoli, Italy. cIstituto Nazionale di Fisica Nucleare (INFN), Sezione di Napoli, Via Cinthia 9, I-80126 Napoli, Italy. dDivis~aode Astrof´ısica,Instituto Nacional de Pesquisas Espaciais, Avenida dos Astronautas 1758, S~aoJos´edos Campos, 12227-010, SP, Brazil. E-mail: abonilla@fisica.ufjf.br, [email protected], [email protected], [email protected] Abstract. The observation of GW170817 binary neutron star (BNS) merger event has imposed strong bounds on the speed of gravitational waves (GWs) locally, inferring that the speed of GWs propagation is equal to the speed of light. Current GW detectors in operation will not be able to observe BNS merger to long cosmological distance, where possible cosmo- logical corrections on the cosmic expansion history are expected to play an important role, specially for investigating possible deviations from general relativity. Future GW detectors designer projects will be able to detect many coalescences of BNS at high z, such as the third generation of the ground GW detector called Einstein Telescope (ET) and the space-based detector deci-hertz interferometer gravitational wave observatory (DECIGO). In this paper, we relax the condition cT =c = 1 to investigate modified GW propagation where the speed of GWs propagation is not necessarily equal to the speed of light.