The Basic Physics of the Binary Black Hole Merger GW150914
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The International Development Research Centre is a public corporation created by the Parliament of Canada in 1970 to support research designed to adapt science and technology to the needs of developing countries. The Centre's activity is concentrated in five sectors: agriculture, food and nutrition sciences; health sciences; information sciences; communications; and social sciences. IDRC is financed solely by the Government of Canada; its policies, however, are set by an international Board of Governors. The Centre's headquarters are in Ottawa, Canada. Regional offices are located in Africa, Asia, Latin America, and the Middle East. ©1978 International Development Research Centre Postal Address: Box 8500, Ottawa, Canada KlG 3H9 Head Office: 60 Queen Street, Ottawa Ronald, K. Selley, L.J. Amoroso, E.C. IDRC IDRC-TS13e Biological synopsis of the manatee. Ottawa, IDRC, 1978. 112 p. /IDRC publication/. Monograph on the manatee, an aquatic mammal (/animal species/) of the /tropical zone/s of I Africa south of Sahara/ and /Latin America/, with an extensive /bibliography/ - discusses the /classification/ of the species and subspecies of the genus Trichechus; /morphology/, /physiology/, /behaviour/, /reproduction/, /animal ecology/ (role in /aquatic plant/ /weed control/), and measures for /animal protection/ of the manatee. UDC: 599.55 ISBN: 0-88936-168-1 Microfiche edition available IDRC-TS13e Biological Synopsis of the Manatee K. Ronald, L.J. Selley, and E.C. Amoroso1 College ofBiological Science, University of Guelph, Guelph, Ontario 1 Present address: Agricultural Research Council, Institute of Animal Physiology, Babraham, Cambridge, England. This work was carried out with the aid of a grant from the International Development Research Centre. -
(K)Cudos at Ψtucson
(K)CUDOs at ΨTucson Work based on collaborative effort with present/former AZ students: Jeremiah Birrell and Lance Labun with contributions from exchange student from Germany Ch. Dietl. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 1/39 1. Introduction 2. Dark Matter (CDM) Generalities 3. Strangeletts 4. Dark Matter (DM) CUDOs 5. CUDO impacts Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 2/39 kudos (from Greek kyddos, singular) = honor; glory; acclaim; praise kudo = back formation from kudos construed as a plural cud (Polish, pronounced c-ood) = miracle cudo (colloq. Polish) = of surprising and exceptional character CUDO=Compact UltraDense Object: A new opportunity to search for dark matter. Not dark matter in form of elementary particles (all present day searches) but (self) bound dark matter. Either an ultra-compact impactor or/and condensation seed for comets. There is a lot of dark matter around, cosmological abundance limit shown below. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 3/39 A new type of meteors What if there are ‘dark’ matter meteor and asteroid-like bodies in the Universe? Could some of them have collided with solar system bodies and the Earth? Are they dressed in visible matter from prior impacts and as condensation seeds? CUDOs’ high density of gravitating matter provides the distinct observable, the surface-penetrating puncture: shot through Only a fraction of the kinetic energy damaging the solid surface. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 4/39 Asteroids of high density Fruitful Discussions with Marshall Eubanks lead to these data. -
Asteroid Spin Axes
ASTEROID SPIN AXES Asteroid Q Period Amp L1 B1 L2 B2 L3 B3 L4 B4 Sid. period Mod Reference 1 Ceres 9.074170 0.06 332.0 70.0 Saint-Pe, 93 298.0 78.0 186.6 −58.0 Drummond, 98 3 322.0 78.0 Thomas, 05 352.0 80.0 Drummond, 08 346.0 82.0 Drummond, 14 2 Pallas 7.8132 0.16 228.0 43.0 7.8106 Schroll, 76 211.0 38.0 Burchi, 83 200.0 40.0 220.0 15.0 Binzel, 84 44.0 4.0 148.0 55.0 224.0 −4.0 328.0 −55.0 Zappala, 84 49.0 6.0 157.0 53.0 229.0 −6.0 337.0 −53.0 Burchi, 85 54.0 −6.0 7.813 Magnusson, 86 100.0 −22.0 295.0 16.0 Y Drummond, 89 70.0 15.0 250.0 15.0 70.0 −15.0 250.0 −15.0 Y Drummond, 89 3 193.0 43.0 35.0 −12.0 7.813224 Y Torppa, 03 32.0 −21.0 Drummond, 08 3 35.6 −12.6 193.1 44.2 7.813225 Y Higley, 08 2 34.0 −27.0 Y Drummond, 09 3 30.0 −16.0 Y Carry, 10 3 35.0 −12.0 7.81323 Durech, 11 3∗Juno 7.210 0.22 71.0 49.0 7.213 Chang, 62 101.0 29.0 321.0 57.0 141.0 −57.0 281.0 −29.0 Y Zappala, 84 110.0 40.0 7.210 Magnusson, 86 104.0 36.0 316.0 62.0 7.209526 Birch, 89 108.0 34.0 7.20953 Y Erikson, 93 108.0 38.0 7.20953 Y Dotto, 95 3 103.0 27.0 7.209531 Y Kaasalainen, 02 118.0 30.0 Drummond, 08 3 103.0 27.0 7.209531 Durech, 11 103.0 22.0 7.20953091 Y Viikinkoski, 15 104.0 20.0 7.209532 Hanus, 16 4 Vesta 5.342 0.19 14.0 80.0 5.3448 Cailliate, 56 10.689 Y Haupt, 58 57.0 74.0 5.34212 Chang, 62 126.0 65.0 5.342129 Gehrels, 67 139.0 47.0 333.0 39.0 10.6824 Taylor, 73 103.0 43.0 301.0 33.0 5.34213 Taylor, 85 120.0 65.0 325.0 55.0 5.342124 Y Magnusson, 86 85.0 58.0 310.0 60.0 Y Cellino, 87 336.0 55.0 5.3421 Y Drummond, 88 311.0 67.0 Y Drummond, 89 160.0 52.0 340.0 -
Broadband Photometry of the Potentially Hazardous Asteroid (153958) 2002 AM31: a Binary Near-Earth Asteroid
Broadband Photometry of the Potentially Hazardous Asteroid (153958) 2002 AM31: A Binary Near-Earth Asteroid Tamara Davtyan¹, Michael D Hicks² 1-Los Angeles City College, Los Angeles, CA 2-Jet Propulsion Laboratory, Pasadena, CA Abstract The near-Earth asteroid 153958 (2002 AM31) was discovered on January 14, 2002 by the LINEAR NEO survey (MPEC 2002-A102) in New Mexico. The object passed within 0.035 AU of the Earth on July 22 2012 and has been identified as a Potentially Hazardous Asteroid (PHA) by the IAU Minor Planet Center. We were motivated by the PHA's favorable 2012 apparition and obtained 6 nights of time-resolved Bessel BVRI photometry and 5 nights of Bessel R photometry at the JPL Table Mountain Observatory (TMO) 0.6-m telescope. We generated a solar phase curve that was used to fit a standard H-G model ( H R=18.43, G=0.61). The derived G value was found to indicate a high optical albedo and an E-type classification. However, our observations yielded that the object's averaged broad-band colors indices ( B− R=0.217±0.018 mag; V −R=0.066±0.010 mag, R− I=0.001±0.110 mag) were most compatible with an S-type spectral classification (Bus taxonomy). This association obtained through a comparison with the 1341 asteroid spectra collected by SMASS 2 survey (Bus & Binzel 2002) and was best matched by the S-type asteroid 485 Genua. If we adopt a diameter of 0.34 km obtained by Arecibo radar imaging, then we estimate geometric albedo p=0.61. -
The Planetary and Lunar Ephemeris DE 421
IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence. -
The Minor Planet Bulletin, We Feel Safe in Al., 1989)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 43, NUMBER 3, A.D. 2016 JULY-SEPTEMBER 199. PHOTOMETRIC OBSERVATIONS OF ASTEROIDS star, and asteroid were determined by measuring a 5x5 pixel 3829 GUNMA, 6173 JIMWESTPHAL, AND sample centered on the asteroid or star. This corresponds to a 9.75 (41588) 2000 SC46 by 9.75 arcsec box centered upon the object. When possible, the same comparison star and check star were used on consecutive Kenneth Zeigler nights of observation. The coordinates of the asteroid were George West High School obtained from the online Lowell Asteroid Services (2016). To 1013 Houston Street compensate for the effect on the asteroid’s visual magnitude due to George West, TX 78022 USA ever changing distances from the Sun and Earth, Eq. 1 was used to [email protected] vertically align the photometric data points from different nights when constructing the composite lightcurve: Bryce Hanshaw 2 2 2 2 George West High School Δmag = –2.5 log((E2 /E1 ) (r2 /r1 )) (1) George West, TX USA where Δm is the magnitude correction between night 1 and 2, E1 (Received: 2016 April 5 Revised: 2016 April 7) and E2 are the Earth-asteroid distances on nights 1 and 2, and r1 and r2 are the Sun-asteroid distances on nights 1 and 2. CCD photometric observations of three main-belt 3829 Gunma was observed on 2016 March 3-5. Weather asteroids conducted from the George West ISD Mobile conditions on March 3 and 5 were not particularly favorable and so Observatory are described. -
Download Full Issue
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 47, NUMBER 1, A.D. 2020 JANUARY-MARCH 1. SECTION NEWS: COLLABORATIVE ASTEROID PHOTOMETRY FOR STAFFING CHANGES FOR ASTEROID 2051 CHANG THE MINOR PLANET BULLETIN Alessandro Marchini Frederick Pilcher Astronomical Observatory, DSFTA - University of Siena (K54) Minor Planets Section Recorder Via Roma 56, 53100 - Siena, ITALY [email protected] [email protected] One staffing change and one staffing addition for The Minor Planet Bulletin are announced effective with this issue. Riccardo Papini, Massimo Banfi, Fabio Salvaggio Wild Boar Remote Observatory (K49) MPB Distributor Derald Nye is now retired from his 37 years of San Casciano in Val di Pesa (FI), ITALY service to the Minor Planets Bulletin. Derald stepped in to service at the time the MPB made its transition from the original Editor Melissa N. Hayes-Gehrke, Eric Yates and Section founder, Richard G. Hodgson. As Derald reflected in Department of Astronomy, University of Maryland a short essay written in MPB 40, page 53 (2013), the Distributor College Park, MD, USA 20740 position was the longest job he ever held, having retired from being a programmer for 30 years with IBM. (Work for IBM (Received: 2019 October 15) included programming for the space program.) At its peak, Derald was managing nearly 200 subscriptions. That number dropped to Photometric observations of this main-belt asteroid were the dozen or so libraries maintaining a permanent collection conducted in order to determine its rotation period. The following the MPB transitioning to becoming an on-line electronic authors found a synodic rotation period of 12.013 ± journal with limited printing. -
The Basic Physics of the Binary Black Hole Merger GW150914
August 5, 2016 The basic physics of the binary black hole merger GW150914 The LIGO Scientific Collaboration and The Virgo Collaboration¤ The first direct gravitational-wave detection was made by the Advanced Laser Interferometer Gravitational Wave Observatory on September 14, 2015. The GW150914 signal was strong enough to be apparent, without using any waveform model, in the filtered detec- tor strain data. Here those features of the signal visible in these data are used, along with only such concepts from Newtonian physics and general relativity as are ac- cessible to anyone with a general physics background. The simple analysis presented here is consistent with the fully general-relativistic analyses published else- Figure 1 The instrumental strain data in the Livingston detec- where, in showing that the signal was produced by the tor (blue) and Hanford detector (red), as shown in Figure 1 of inspiral and subsequent merger of two black holes. The [1]. Both have been bandpass- and notch-filtered. The Hanford black holes were each of approximately 35M , still strain has been shifted back in time by 6.9 ms and inverted. ¯ Times shown are relative to 09:50:45 Coordinated Universal orbited each other as close as 350 km apart and sub- » Time (UTC) on September 14, 2015. sequently merged to form a single black hole. Similar reasoning, directly from the data, is used to roughly es- timate how far these black holes were from the Earth, A black hole is a region of space-time where the gravita- and the energy that they radiated in gravitational waves. -
Asteroid Spin Axes
ASTEROID SPIN AXES Asteroid Q Period Amp L1 B1 L2 B2 L3 B3 L4 B4 Sid. period Mod Reference 1 Ceres 3 9.074170 0.06 332.0 +70.0 N Saint-Pe, 93 298.0 +78.0 186.6 −58.0 N Drummond, 98 3 322.0 +78.0 N Thomas, 05 352.0 +80.0 N Drummond, 08 346.0 +82.0 N Drummond, 14 2∗Pallas 3 7.8132 0.16 228.0 +43.0 7.8106 N Schroll, 76 211.0 +38.0 N Burchi, 83 200.0 +40.0 220.0 +15.0 N Binzel, 84 44.0 +4.0 148.0 +55.0 224.0 −4.0 328.0 −55.0 N Zappala, 84 49.0 +6.0 157.0 +53.0 229.0 −6.0 337.0 −53.0 N Burchi, 85 54.0 −6.0 7.813 N Magnusson, 86 100.0 −22.0 295.0 +16.0 Y Drummond, 89 70.0 +15.0 250.0 +15.0 70.0 −15.0 250.0 −15.0 Y Drummond, 89 3 35.0 −12.0 193.0 +43.0 7.813225 Y Torppa, 03 32.0 −21.0 N Drummond, 08 3 35.6 −12.6 193.1 +44.2 7.813225 Y Higley, 08 2 34.0 −27.0 Y Drummond, 09 3 30.0 −16.0 7.8132214 Y Carry, 10 3 35.0 −12.0 7.81323 Durech, 11 30.0 −13.0 7.81322 Y Hanus, 17 3 Juno 3 7.210 0.22 71.0 +49.0 7.213 N Chang, 62 101.0 +29.0 321.0 +57.0 141.0 −57.0 281.0 −29.0 Y Zappala, 84 110.0 +40.0 7.210 N Magnusson, 86 104.0 +36.0 316.0 +62.0 7.209526 N Birch, 89 108.0 +34.0 7.20953 Y Erikson, 93 108.0 +38.0 7.20953 Y Dotto, 95 3 103.0 +27.0 7.209531 Y Kaasalainen, 02 118.0 +30.0 N Drummond, 08 3 103.0 +27.0 7.209531 Durech, 11 103.0 +22.0 7.20953091 Y Viikinkoski, 15 104.0 +20.0 7.209532 Hanus, 16 4 Vesta 3 5.342 0.19 14.0 +80.0 5.3448 N Cailliate, 56 10.689 Y Haupt, 58 57.0 +74.0 5.34212 N Chang, 62 126.0 +65.0 5.342129 N Gehrels, 67 139.0 +47.0 333.0 +39.0 10.6824 N Taylor, 73 103.0 +43.0 301.0 +33.0 5.34213 N Taylor, 85 120.0 +65.0 325.0 +55.0 5.342124 -
The Planetary and Lunar Ephemerides DE430 and DE431
IPN Progress Report 42-196 • February 15, 2014 The Planetary and Lunar Ephemerides DE430 and DE431 William M. Folkner,* James G. Williams,† Dale H. Boggs,† Ryan S. Park,* and Petr Kuchynka* ABSTRACT. — The planetary and lunar ephemerides DE430 and DE431 are generated by fitting numerically integrated orbits of the Moon and planets to observations. The present-day lunar orbit is known to submeter accuracy through fitting lunar laser ranging data with an updated lunar gravity field from the Gravity Recovery and Interior Laboratory (GRAIL) mission. The orbits of the inner planets are known to subkilometer accuracy through fitting radio tracking measurements of spacecraft in orbit about them. Very long baseline interfer- ometry measurements of spacecraft at Mars allow the orientation of the ephemeris to be tied to the International Celestial Reference Frame with an accuracy of 0′′.0002. This orien- tation is the limiting error source for the orbits of the terrestrial planets, and corresponds to orbit uncertainties of a few hundred meters. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of fitting spacecraft tracking data. The orbits of Uranus, Neptune, and Pluto are determined primarily from astrometric observations, for which measurement uncertainties due to the Earth’s atmosphere, combined with star catalog uncertainties, limit position accuracies to several thousand kilometers. DE430 and DE431 differ in their integrated time span and lunar dynamical modeling. The dynamical model for DE430 included a damping term between the Moon’s liquid core and solid man- tle that gives the best fit to lunar laser ranging data but that is not suitable for backward integration of more than a few centuries. -
Multi-Messenger Observations of a Binary Neutron Star Merger
The Astrophysical Journal Letters, 848:L12 (59pp), 2017 October 20 https://doi.org/10.3847/2041-8213/aa91c9 © 2017. The American Astronomical Society. All rights reserved. Multi-messenger Observations of a Binary Neutron Star Merger LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-Hxmt Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF (Deeper, Wider, Faster Program),AST3, and CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, Caltech- NRAO, TTU-NRAO, and NuSTAR Collaborations,Pan-STARRS,TheMAXITeam,TZACConsortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H.E.S.S. Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT (See the end matter for the full list of authors.) Received 2017 October 3; revised 2017 October 6; accepted 2017 October 6; published 2017 October 16 Abstract On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. -
The Minor Planet Bulletin, 30(3), Pp
1 THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 31, NUMBER 1, A.D. 2004 JANUARY-MARCH 1. ASTROMETRIC PROGRAM FOR JR refers to asteroids nearby to the 3:1 mean motion resonance NEAR-EARTH OBJECT SOURCES with Jupiter, MC are the Mars Crossers, NU are objects in the ν 6 secular resonance. Sergio Foglia UAI Minor Planets Section Recorder References F. Bisleri 11, I-20148 Milano, Italy € [email protected] Morbidelli et. al. (2003). Understanding the distribution on Near Earth Objects. http://www.obs-nice.fr/morby/ESA/ esa.html (Received: 24 September Revised: 6 October) MPC Orbit Database. ftp://ftp-cfa.harvard.edu/pub/MPCORB/ 2003 Sep. 17, Minor Planet Center A new astroometric program is proposed for asteroids located in likely source regions supplying the near-Earth Proper Elements of Minor Planets. http://hamilton.dm object population. .unipi.it/astdys/ 2003 Sep. 17, Asteroid Dynamic Site According to Morbidelli et al. (2003), near-Earth objects (NEOs) come mainly from 5 sources with the following contributions to the population: the ν 6 resonance region at the inner border of the asteroid main belt (37 ± 8 %), the 3:1 resonance region in the middle of the asteroid main belt (23 ± 8 %), the Intermediate Mars-Crossing (IMC) population (25 ± 3 %), the Outer Belt (OB) population€ (8 ± 1 %), and the population of dormant Jupiter Family Comets (JFC) (6 ± 4 %). Astrometric measurements of objects in these source regions would be very useful to increase knowledge about the NEO source population and solar system dynamics.