The Secret Lives of Stars 2004

Total Page:16

File Type:pdf, Size:1020Kb

The Secret Lives of Stars 2004 WWW.SCIAM.COM COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. SCIENTIFIC AMERICAN Volume 14, Number 4 The Secret Lives of Stars 2004 3 Letter from the Editor YOUTH 4 The First Stars in the Universe BY RICHARD B. LARSON AND VOLKER BROMM Exceptionally massive and bright, the earliest stars changed the course of cosmic history. 12 Fountains of Youth: Early Days in the Life of a Star BY THOMAS P. RAY To make a star, gas and dust must fall inward. So why do astronomers see stuff streaming outward? 18 Companions contents to Young Stars BY ALAN P. BOSS The surprising finding that even the youngest stars commonly exist in sets of two or three has revised thinking about the birth of star systems. 26 The Discovery of Brown Dwarfs BY GIBOR BASRI Less massive than stars but more massive than planets, brown dwarfs were long assumed to be rare. New sky surveys, however, show that the objects may be as common as stars. 42 THE SECRET LIVES OF STARS COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. 34 92 MIDLIFE OLD AGE 34 The Stellar Dynamo 76 Supersoft X-ray Stars and BY ELIZABETH NESME-RIBES, SALLIE L. BALIUNAS AND DMITRY SOKOLOFF Supernovae BY PETER KAHABKA, EDWARD P. J. VAN DEN HEUVEL AND Sunspot cycles—on other stars—are helping astronomers SAUL A. RAPPAPORT study the sun’s variations and the ways they might Supersoft sources—which spew unusually low-energy affect Earth. x-rays—are now thought to be white dwarf stars that The Fury of Solar Storms siphon matter from their stellar companions and then, in 42 many cases, explode. BY JAMES L. BURCH Shock waves from the sun can endanger Earth’s 84 Binary Neutron Stars satellites and astronauts. BY TSVI PIRAN When Stars Collide The inevitable collapse of these paired stellar remnants 50 generates runaway heating that, for a few weeks, emits BY MICHAEL SHARA more light than an entire galaxy. When two stars smash into each other, it can be a very pretty sight. Once considered impossible, these 92 The Brightest Explosions occurrences have turned out to be common in certain galactic neighborhoods. in the Universe BY NEIL GEHRELS, LUIGI PIRO AND PETER J. T. LEONARD 58 X-ray Binaries Every time a gamma-ray burst goes off, a black hole is born. BY EDWARD P. J. VAN DEN HEUVEL AND JAN VAN PARADIJS When ultradense neutron stars feed on their more sedate companions, the binary systems produce outpourings of x-rays and drastically alter the evolution of both stars. Cover illustration by Don Dixon Scientific American Special (ISSN 1048-0943), Volume 14, Number 4, 2004, published by Scientific 68 Magnetars American, Inc., 415 Madison Avenue, New York, NY 10017-1111. Copyright © 2004 by Scientific BY CHRYSSA KOUVELIOTOU, ROBERT C. DUNCAN AND American, Inc. All rights reserved. No part of this issue may be reproduced by any mechanical, photographic or electronic process, or in the form of a phonographic recording, nor may it be stored CHRISTOPHER THOMPSON in a retrieval system, transmitted or otherwise copied for public or private use without written permission of the publisher. Canadian BN No. 127387652RT; QST No. Q1015332537. To purchase Magnetized so intensely, some stars alter the very nature additional quantities: U.S., $10.95 each; elsewhere, $13.95 each. Send payment to Scientific American, Dept. STARS, 415 Madison Avenue, New York, NY 10017-1111. of the quantum vacuum. Inquiries: fax 212-355-0408 or telephone 212-451-8890. Printed in U.S.A. 2 THE SECRET LIVES OF STARS COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. ® letter from the editor Established 1845 The Secret Lives of Stars is published by the staff of Scientific American, with project management by: Exposé on the Stars EDITOR IN CHIEF: John Rennie EXECUTIVE EDITOR: Mariette DiChristina ISSUE EDITOR: Mark Fischetti ISSUE CONSULTANT: George Musser FOR PURE THEATRICS and spectacle, Hollywood ce- ART DIRECTOR: Edward Bell ISSUE DESIGNER: Patti Nemoto lebrities have nothing on PHOTOGRAPHY EDITORS: Bridget Gerety Small, the denizens of the heav- Emily Harrison, Smitha Alampur ens. Stars are born, live and PRODUCTION EDITOR: Richard Hunt die in fiery and fascinating COPY DIRECTOR: Maria-Christina Keller COPY CHIEF: Molly K. Frances ways—ways that we have COPY AND RESEARCH: Daniel C. Schlenoff, only recently been able to Michael Battaglia, David Labrador, Sara Beardsley study in greater detail, like EDITORIAL ADMINISTRATOR: Jacob Lasky so many swarming papa- SENIOR SECRETARY: Maya Harty razzi, using the long-range ASSOCIATE PUBLISHER, PRODUCTION: lenses created by improved William Sherman MANUFACTURING MANAGER: Janet Cermak techniques and new, sharp- ADVERTISING PRODUCTION MANAGER: Carl Cherebin er observatories. PREPRESS AND QUALITY MANAGER: Silvia Di Placido We’ve observed some PRINT PRODUCTION MANAGER: Georgina Franco PRODUCTION MANAGER: Christina Hippeli eye-popping behavior from CUSTOM PUBLISHING MANAGER: Madelyn Keyes-Milch these brazen orbs. As with ASSOCIATE PUBLISHER/VICE PRESIDENT, CIRCULATION: many glamorous beings, Lorraine Leib Terlecki stars often pair off, but the CIRCULATION DIRECTOR: Katherine Corvino FULFILLMENT AND DISTRIBUTION MANAGER: two may blow apart—liter- Rosa Davis ally—one star ripping the ENCOUNTER with a tempestuous starlet tears apart our sun. VICE PRESIDENT AND PUBLISHER: Bruce Brandfon shine from its former part- WESTERN SALES MANAGER: Debra Silver ner in a highly public display. It seems that only about half the stars live as cou- SALES DEVELOPMENT MANAGER: David Tirpack ples—no better than the average state of human relationships. Or consider the WESTERN SALES DEVELOPMENT MANAGER: Valerie Bantner wondrous strange doings of the magnetar, a name itself worthy of a character SALES REPRESENTATIVES: Stephen Dudley, in the blockbuster X-Men films. These intensely magnetized stars emit huge Hunter Millington, Stan Schmidt bursts of magnetic energy that can alter the very nature of the quantum vacu- ASSOCIATE PUBLISHER, STRATEGIC PLANNING: um. Like rebels without a cause, they are furiously active for only a short time: Laura Salant PROMOTION MANAGER: Diane Schube after 10,000 years they wink out. We’ve also been able to see how, after a long RESEARCH MANAGER: Aida Dadurian era of flamboyant x-ray emission, x-ray binaries settle down to become some PROMOTION DESIGN MANAGER: Nancy Mongelli of the most steady, unchanging entities in the cosmos. Not all of these celestial GENERAL MANAGER: Michael Florek BUSINESS MANAGER: Marie Maher objects make it as luminaries, however. We may feel some sympathy for brown MANAGER, ADVERTISING ACCOUNTING AND dwarfs, failed stars that glow so dully nobody could even find one until 1995. COORDINATION: Constance Holmes In this special edition from Scientific American, we invite you to forget about DIRECTOR, SPECIAL PROJECTS: everyday life to spend some time with the stars. In the pages that follow, you’ll Barth David Schwartz find the latest gossip on the glitterati, written by the astronomer shutterbugs MANAGING DIRECTOR, ONLINE: Mina C. Lux themselves. Although the stars have revealed more than ever, they’ve been OPERATIONS MANAGER, ONLINE: Vincent Ma SALES REPRESENTATIVE, ONLINE: Gary Bronson careful not to tell all, lest we grow bored with their antics. As authors Chryssa DIRECTOR, ANCILLARY PRODUCTS: Diane McGarvey Kouveliotou, Robert C. Duncan and Christopher Thompson so aptly put it in PERMISSIONS MANAGER: Linda Hertz “Magnetars”: “What other phenomena, so rare and fleeting that we have not MANAGER OF CUSTOM PUBLISHING: recognized them, lurk out there?” We can hardly wait to find out. Jeremy A. Abbate CHAIRMAN EMERITUS: John J. Hanley CHAIRMAN: John Sargent PRESIDENT AND CHIEF EXECUTIVE OFFICER: Mariette DiChristina Gretchen G. Teichgraeber Executive Editor VICE PRESIDENT AND MANAGING DIRECTOR, INTERNATIONAL: Dean Sanderson Scientific American VICE PRESIDENT: Frances Newburg MARK A. GARLICK [email protected] www.sciam.com THE SECRET LIVES OF STARS 3 COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. THEFIRST STARS IN THE UNIVERSE Exceptionally massive and bright, the earliest stars changed the course of cosmic history We live in a universe that is full of bright objects. On a clear night one can see thousands of stars with the naked eye. These stars occupy mere- ly a small nearby part of the Milky Way galaxy; tele- scopes reveal a much vaster realm that shines with the light from billions of galaxies. According to our current understanding of cosmology, howev- er, the universe was featureless and dark for a long stretch of its early history. The first stars did not appear until perhaps 100 million years after the big bang, and nearly a billion years passed before galaxies proliferated across the cosmos. Astron- BY RICHARD B. LARSON AND VOLKER BROMM omers have long wondered: How did this dramat- ILLUSTRATIONS BY DON DIXON ic transition from darkness to light come about? 4 SCIENTIFIC AMERICAN Updated from the December 2001 issue COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. EARLIEST COSMIC STRUCTURE mmostost likely took the form of a network of filaments. The first protogalaxies, small-scale systems about 30 to 100 light-years across, coalesced at the nodes of this network. Inside the protogalaxies, the denser regions of gas collapsed to form the first stars (inset). COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. After decades of study, researchers The Dark Ages to longer wavelengths and the universe have recently made great strides toward THE STUDY of the early universe is grew increasingly cold and dark. As- answering this question. Using sophisti- hampered by a lack of direct observa- tronomers have no observations of this cated computer simulation techniques, tions. Astronomers have been able to ex- dark era. But by a billion years after the cosmologists have devised models that amine much of the universe’s history by big bang, some bright galaxies and show how the density fluctuations left training their telescopes on distant galax- quasars had already appeared, so the first over from the big bang could have ies and quasars that emitted their light stars must have formed sometime before.
Recommended publications
  • NSF Current Newsletter Highlights Research and Education Efforts Supported by the National Science Foundation
    March 2012 Each month, the NSF Current newsletter highlights research and education efforts supported by the National Science Foundation. If you would like to automatically receive notifications by e-mail or RSS when future editions of NSF Current are available, please use the links below: Subscribe to NSF Current by e-mail | What is RSS? | Print this page | Return to NSF Current Archive Robotic Surgery Systems Shipped to Medical Research Centers A set of seven identical advanced robotic-surgery systems produced with NSF support were shipped last month to major U.S. medical research laboratories, creating a network of systems using a common platform. The network is designed to make it easy for researchers to share software, replicate experiments and collaborate in other ways. Robotic surgery has the potential to enable new surgical procedures that are less invasive than existing techniques. The developers of the Raven II system made the decision to share it as the best way to move the field forward--though it meant giving competing laboratories tools that had taken them years to develop. "We decided to follow an open-source model, because if all of these labs have a common research platform for doing robotic surgery, the whole field will be able to advance more quickly," said Jacob Rosen, Students with components associate professor of computer engineering at the University of of the Raven II surgical California-Santa Cruz. Rosen and Blake Hannaford, director of the robotics systems. Credit: University of Washington Biorobotics Laboratory, led the team that Carolyn Lagattuta built the Raven system, initially with a U.S.
    [Show full text]
  • Black-Hole Binaries, Gravitational Waves, and Numerical Relativity
    Black-hole binaries, gravitational waves, and numerical relativity Joan Centrella∗ and John G. Baker† Gravitational Astrophysics Laboratory, NASA/GSFC, 8800 Greenbelt Road, Greenbelt, Maryland 20771, USA Bernard J. Kelly‡ and James R. van Meter§ CRESST and Gravitational Astrophysics Laboratory, NASA/GSFC, 8800 Greenbelt Road, Greenbelt, Maryland 20771, USA and Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA (Dated: November 30, 2010) Understanding the predictions of general relativity for the dynamical interactions of two black holes has been a long-standing unsolved problem in theoretical physics. Black-hole mergers are monu- mental astrophysical events, releasing tremendous amounts of energy in the form of gravitational radiation, and are key sources for both ground- and space-based gravitational-wave detectors. The black-hole merger dynamics and the resulting gravitational waveforms can only be calculated through numerical simulations of Einstein’s equations of general relativity. For many years, nu- merical relativists attempting to model these mergers encountered a host of problems, causing their codes to crash after just a fraction of a binary orbit could be simulated. Recently, however, a series of dramatic advances in numerical relativity has allowed stable, robust black-hole merger simulations. This remarkable progress in the rapidly maturing field of numerical relativity, and the new understanding of black-hole binary dynamics that is emerging is chronicled. Important applications of these fundamental physics results to astrophysics, to gravitational-wave astronomy, and in other areas are also discussed. Contents G. Numerical Approximation Methods 15 H. Extracting the Physics 15 I. Prelude 2 V. Black-Hole Merger Dynamics and Waveforms 16 II.
    [Show full text]
  • Are Gamma-Ray Bursts Signals of Supermassive Black Hole Formation?
    Are Gamma-Ray Bursts Signals of Supermassive Black Hole Formation? K. Abazajian, G. Fuller, X. Shi Department of Physics, University of California, San Diego, La Jolla, California 92093-0350 Abstract. The formation of supermassive black holes through the gravitational 4 collapse of supermassive objects (M ∼> 5 × 10 M⊙) has been proposed as a source of cosmological γ-ray bursts. The major advantage of this model is that such collapses are far more energetic than stellar-remnant mergers. The major drawback of this idea is the severe baryon loading problem in one-dimensional models. We can show that the observed log N − log P (number vs. peak flux) distribution for gamma-ray bursts in the BATSE database is not inconsistent with an identification of supermassive object collapse as the origin of the gamma-ray bursts. This conclusion is valid for a range of plausible cosmological and γ-ray burst spectral parameters. 1. Introduction We investigate aspects of a recent model for the internal engine powering γ-ray bursts (GRBs). This model produces a GRB fireball through neutrino emission and annihilation during the collapse of a supermassive object into a black hole (Fuller & Shi, 1998). This supermassive object may either be a relativistic cluster of stars or a single supermassive star. The collapse of a supermassive object provides an exceedingly large amount of energy to power the burst, much higher than the amount of energy available in stellar remnant models. In addition, the rate of collapse of these objects–when associated with galaxy-type structures–is arXiv:astro-ph/9812287v1 15 Dec 1998 similar to the GRB rate.
    [Show full text]
  • Gamma Ray Bursts from Stellar Collisions
    CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Gamma Ray Bursts from Stellar Collisions Brad M.S. Hansen & Chigurupati Murali Canadian Institute for Theoretical Astrophysics University of Toronto, Toronto, ON M5S 3H8, Canada Received ; accepted –2– ABSTRACT We propose that the cosmological gamma ray bursts arise from the collapse of neutron stars to black holes triggered by collisions or mergers with main sequence stars. This scenario represents a cosmological history qualitatively different from most previous theories because it contains a significant contribution from an old stellar population, namely the globular clusters. Furthermore, the gas poor central regions of globular clusters provide an ideal environment for the generation of the recently confirmed afterglows via the fireball scenario. Collisions resulting from neutron star birth kicks in close binaries may also contribute to the overall rate and should lead to associations between some gamma ray bursts and supernovae of type Ib/c. Subject headings: stars:neutron–supernovae:general–globular clusters:general– gamma rays:bursts– Galaxy:evolution –3– 1. Introduction The detection of X-ray, optical and radio afterglows from gamma-ray burst events (Costa et al 1997; van Paradijs et al 1997, Sahu et al 1997; Frail et al 1997) and concommitant redshifts (Metzger et al 1997) has provided strong support for the cosmological origin of the phenomenon. The success of the fireball model (Cavallo & Rees 1978; Rees & Meszaros 1992; Meszaros & Rees 1993) is largely independent of the origin of the energy, requiring only an energetic and baryon-poor event confined to small scales, thereby giving rise to a relativistic and optically thick outflow.
    [Show full text]
  • Effect of the Solar Wind Density on the Evolution of Normal and Inverse Coronal Mass Ejections S
    A&A 632, A89 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935894 & c ESO 2019 Astrophysics Effect of the solar wind density on the evolution of normal and inverse coronal mass ejections S. Hosteaux, E. Chané, and S. Poedts Centre for mathematical Plasma-Astrophysics (CmPA), Celestijnenlaan 200B, KU Leuven, 3001 Leuven, Belgium e-mail: [email protected] Received 15 May 2019 / Accepted 11 September 2019 ABSTRACT Context. The evolution of magnetised coronal mass ejections (CMEs) and their interaction with the background solar wind leading to deflection, deformation, and erosion is still largely unclear as there is very little observational data available. Even so, this evolution is very important for the geo-effectiveness of CMEs. Aims. We investigate the evolution of both normal and inverse CMEs ejected at different initial velocities, and observe the effect of the background wind density and their magnetic polarity on their evolution up to 1 AU. Methods. We performed 2.5D (axisymmetric) simulations by solving the magnetohydrodynamic equations on a radially stretched grid, employing a block-based adaptive mesh refinement scheme based on a density threshold to achieve high resolution following the evolution of the magnetic clouds and the leading bow shocks. All the simulations discussed in the present paper were performed using the same initial grid and numerical methods. Results. The polarity of the internal magnetic field of the CME has a substantial effect on its propagation velocity and on its defor- mation and erosion during its evolution towards Earth. We quantified the effects of the polarity of the internal magnetic field of the CMEs and of the density of the background solar wind on the arrival times of the shock front and the magnetic cloud.
    [Show full text]
  • Predicting the Magnetic Vectors Within Coronal Mass Ejections Arriving at Earth: 2
    Space Weather RESEARCH ARTICLE Predicting the magnetic vectors within coronal mass ejections 10.1002/2015SW001171 arriving at Earth: 1. Initial architecture Key Points: N. P.Savani1,2, A. Vourlidas1, A. Szabo2,M.L.Mays2,3, I. G. Richardson2,4, B. J. Thompson2, • First architectural design to predict A. Pulkkinen2,R.Evans5, and T. Nieves-Chinchilla2,3 a CME’s magnetic vectors (with eight events) 1 2 • Modified Bothmer-Schwenn CME Goddard Planetary Heliophysics Institute (GPHI), University of Maryland, Baltimore County, Maryland, USA, NASA 3 initiation rule to improve reliability Goddard Space Flight Center, Greenbelt, Maryland, USA, Institute for Astrophysics and Computational Sciences (IACS), of chirality Catholic University of America, Washington, District of Columbia, USA, 4Department of Astronomy, University of • CME evolution seen by remote Maryland, College Park, Maryland, USA, 5College of Science, George Mason University, Fairfax, Vancouver, USA sensing triangulation is important for forecasting Abstract The process by which the Sun affects the terrestrial environment on short timescales is Correspondence to: predominately driven by the amount of magnetic reconnection between the solar wind and Earth’s N. P. Savani, magnetosphere. Reconnection occurs most efficiently when the solar wind magnetic field has a southward [email protected] component. The most severe impacts are during the arrival of a coronal mass ejection (CME) when the magnetosphere is both compressed and magnetically connected to the heliospheric environment. Citation: Unfortunately, forecasting magnetic vectors within coronal mass ejections remain elusive. Here we report Savani, N. P., A. Vourlidas, A. Szabo, M.L.Mays,I.G.Richardson,B.J. how, by combining a statistically robust helicity rule for a CME’s solar origin with a simplified flux rope Thompson, A.
    [Show full text]
  • Arxiv:2101.07771V4 [Stat.AP] 9 Jun 2021
    Received Jan-19-2021; Revised Jun-02-2021; Accepted XX-XX-XXX DOI: xxx/xxxx SURVEY Critical Risk Indicators (CRIs) for the electric power grid: A survey and discussion of interconnected effects Che-Castaldo, Judy P.*1 | Cousin, Rémi2 | Daryanto, Stefani3 | Deng, Grace4 | Feng, Mei-Ling E.1 | Gupta, Rajesh K.5 | Hong, Dezhi5 | McGranaghan, Ryan M.6 | Owolabi, Olukunle O.7 | Qu, Tianyi8 | Ren, Wei3 | Schafer, Toryn L. J.4 | Sharma, Ashutosh9,10 | Shen, Chaopeng9 | Sherman, Mila Getmansky8 | Sunter, Deborah A.7 | Tao, Bo3 | Wang, Lan11 | Matteson, David S.4 1Conservation & Science Department, Lincoln Park Zoo, Illinois, USA Abstract 2International Research Institute for Climate The electric power grid is a critical societal resource connecting multiple infrastruc- and Society, Earth Institute / Columbia University, New York, USA tural domains such as agriculture, transportation, and manufacturing. The electrical 3Department of Plant and Soil Sciences, grid as an infrastructure is shaped by human activity and public policy in terms of College of Agriculture, Food and Environment / University of Kentucky, demand and supply requirements. Further, the grid is subject to changes and stresses Kentucky, USA due to diverse factors including solar weather, climate, hydrology, and ecology. The 4 Department of Statistics and Data Science, emerging interconnected and complex network dependencies make such interactions Cornell University, New York, USA 5Halicioglu Data Science Institute and increasingly dynamic, posing novel risks, and presenting new challenges to manage Department of Computer Science & the coupled human-natural system. This paper provides a survey of models and meth- Engineering, University of California, San ods that seek to explore the significant interconnected impact of the electric power Diego, California, USA 6Atmosphere Space Technology Research grid and interdependent domains.
    [Show full text]
  • Cmes, Solar Wind and Sun-Earth Connections: Unresolved Issues
    CMEs, solar wind and Sun-Earth connections: unresolved issues Rainer Schwenn Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany [email protected] In recent years, an unprecedented amount of high-quality data from various spaceprobes (Yohkoh, WIND, SOHO, ACE, TRACE, Ulysses) has been piled up that exhibit the enormous variety of CME properties and their effects on the whole heliosphere. Journals and books abound with new findings on this most exciting subject. However, major problems could still not be solved. In this Reporter Talk I will try to describe these unresolved issues in context with our present knowledge. My very personal Catalog of ignorance, Updated version (see SW8) IAGA Scientific Assembly in Toulouse, 18-29 July 2005 MPRS seminar on January 18, 2006 The definition of a CME "We define a coronal mass ejection (CME) to be an observable change in coronal structure that occurs on a time scale of a few minutes and several hours and involves the appearance (and outward motion, RS) of a new, discrete, bright, white-light feature in the coronagraph field of view." (Hundhausen et al., 1984, similar to the definition of "mass ejection events" by Munro et al., 1979). CME: coronal -------- mass ejection, not: coronal mass -------- ejection! In particular, a CME is NOT an Ejección de Masa Coronal (EMC), Ejectie de Maså Coronalå, Eiezione di Massa Coronale Éjection de Masse Coronale The community has chosen to keep the name “CME”, although the more precise term “solar mass ejection” appears to be more appropriate. An ICME is the interplanetry counterpart of a CME 1 1.
    [Show full text]
  • Executive Sessions of the Senate Permanent Subcommittee on Investigations of the Committee on Government Operations
    S. Prt. 107–84 EXECUTIVE SESSIONS OF THE SENATE PERMANENT SUBCOMMITTEE ON INVESTIGATIONS OF THE COMMITTEE ON GOVERNMENT OPERATIONS VOLUME 4 EIGHTY-THIRD CONGRESS FIRST SESSION 1953 ( MADE PUBLIC JANUARY 2003 Printed for the use of the Committee on Governmental Affairs U.S. GOVERNMENT PRINTING OFFICE 83–872 WASHINGTON : 2003 For sale by the Superintendent of Documents, U.S. Government Printing Office Internet: bookstore.gpo.gov Phone: toll free (866) 512–1800; DC area (202) 512–1800 Fax: (202) 512–2250 Mail: Stop SSOP, Washington, DC 20402–0001 VerDate Jan 31 2003 21:53 Mar 31, 2003 Jkt 083872 PO 00000 Frm 00003 Fmt 5011 Sfmt 5011 E:\HR\OC\83872PL.XXX 83872PL COMMITTEE ON GOVERNMENTAL AFFAIRS 107TH CONGRESS, SECOND SESSION JOSEPH I. LIEBERMAN, Connecticut, Chairman CARL LEVIN, Michigan FRED THOMPSON, Tennessee DANIEL K. AKAKA, Hawaii TED STEVENS, Alaska RICHARD J. DURBIN, Illinois SUSAN M. COLLINS, Maine ROBERT G. TORRICELLI, New Jersey GEORGE V. VOINOVICH, Ohio MAX CLELAND, Georgia THAD COCHRAN, Mississippi THOMAS R. CARPER, Delaware ROBERT F. BENNETT, Utah MARK DAYTON, Minnesota JIM BUNNING, Kentucky PETER G. FITZGERALD, Illinois JOYCE A. RECHTSCHAFFEN, Staff Director and Counsel RICHARD A. HERTLING, Minority Staff Director DARLA D. CASSELL, Chief Clerk PERMANENT SUBCOMMITTEE ON INVESTIGATIONS CARL LEVIN, Michigan, Chairman DANIEL K. AKAKA, Hawaii, SUSAN M. COLLINS, Maine RICHARD J. DURBIN, Illinois TED STEVENS, Alaska ROBERT G. TORRICELLI, New Jersey GEORGE V. VOINOVICH, Ohio MAX CLELAND, Georgia THAD COCHRAN, Mississippi THOMAS R. CARPER, Delaware ROBERT F. BENNETT, Utah MARK DAYTON, Minnesota JIM BUNNING, Kentucky PETER G. FITZGERALD, Illinois ELISE J. BEAN, Staff Director and Chief Counsel KIM CORTHELL, Minority Staff Director MARY D.
    [Show full text]
  • Solar Wind Properties and Geospace Impact of Coronal Mass Ejection-Driven Sheath Regions: Variation and Driver Dependence E
    Solar Wind Properties and Geospace Impact of Coronal Mass Ejection-Driven Sheath Regions: Variation and Driver Dependence E. K. J. Kilpua, D. Fontaine, C. Moissard, M. Ala-lahti, E. Palmerio, E. Yordanova, S. Good, M. M. H. Kalliokoski, E. Lumme, A. Osmane, et al. To cite this version: E. K. J. Kilpua, D. Fontaine, C. Moissard, M. Ala-lahti, E. Palmerio, et al.. Solar Wind Properties and Geospace Impact of Coronal Mass Ejection-Driven Sheath Regions: Variation and Driver Dependence. Space Weather: The International Journal of Research and Applications, American Geophysical Union (AGU), 2019, 17 (8), pp.1257-1280. 10.1029/2019SW002217. hal-03087107 HAL Id: hal-03087107 https://hal.archives-ouvertes.fr/hal-03087107 Submitted on 23 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. RESEARCH ARTICLE Solar Wind Properties and Geospace Impact of Coronal 10.1029/2019SW002217 Mass Ejection-Driven Sheath Regions: Variation and Key Points: Driver Dependence • Variation of interplanetary properties and geoeffectiveness of CME-driven sheaths and their dependence on the E. K. J. Kilpua1 , D. Fontaine2 , C. Moissard2 , M. Ala-Lahti1 , E. Palmerio1 , ejecta properties are determined E.
    [Show full text]
  • Ten Years of PAMELA in Space
    Ten Years of PAMELA in Space The PAMELA collaboration O. Adriani(1)(2), G. C. Barbarino(3)(4), G. A. Bazilevskaya(5), R. Bellotti(6)(7), M. Boezio(8), E. A. Bogomolov(9), M. Bongi(1)(2), V. Bonvicini(8), S. Bottai(2), A. Bruno(6)(7), F. Cafagna(7), D. Campana(4), P. Carlson(10), M. Casolino(11)(12), G. Castellini(13), C. De Santis(11), V. Di Felice(11)(14), A. M. Galper(15), A. V. Karelin(15), S. V. Koldashov(15), S. Koldobskiy(15), S. Y. Krutkov(9), A. N. Kvashnin(5), A. Leonov(15), V. Malakhov(15), L. Marcelli(11), M. Martucci(11)(16), A. G. Mayorov(15), W. Menn(17), M. Mergè(11)(16), V. V. Mikhailov(15), E. Mocchiutti(8), A. Monaco(6)(7), R. Munini(8), N. Mori(2), G. Osteria(4), B. Panico(4), P. Papini(2), M. Pearce(10), P. Picozza(11)(16), M. Ricci(18), S. B. Ricciarini(2)(13), M. Simon(17), R. Sparvoli(11)(16), P. Spillantini(1)(2), Y. I. Stozhkov(5), A. Vacchi(8)(19), E. Vannuccini(1), G. Vasilyev(9), S. A. Voronov(15), Y. T. Yurkin(15), G. Zampa(8) and N. Zampa(8) (1) University of Florence, Department of Physics, I-50019 Sesto Fiorentino, Florence, Italy (2) INFN, Sezione di Florence, I-50019 Sesto Fiorentino, Florence, Italy (3) University of Naples “Federico II”, Department of Physics, I-80126 Naples, Italy (4) INFN, Sezione di Naples, I-80126 Naples, Italy (5) Lebedev Physical Institute, RU-119991 Moscow, Russia (6) University of Bari, I-70126 Bari, Italy (7) INFN, Sezione di Bari, I-70126 Bari, Italy (8) INFN, Sezione di Trieste, I-34149 Trieste, Italy (9) Ioffe Physical Technical Institute, RU-194021 St.
    [Show full text]
  • The Time of Perihelion Passage and the Longitude of Perihelion of Nemesis
    The Time of Perihelion Passage and the Longitude of Perihelion of Nemesis Glen W. Deen 820 Baxter Drive, Plano, TX 75025 phone (972) 517-6980, e-mail [email protected] Natural Philosophy Alliance Conference Albuquerque, N.M., April 9, 2008 Abstract If Nemesis, a hypothetical solar companion star, periodically passes through the asteroid belt, it should have perturbed the orbits of the planets substantially, especially near times of perihelion passage. Yet almost no such perturbations have been detected. This can be explained if Nemesis is comprised of two stars with complementary orbits such that their perturbing accelerations tend to cancel at the Sun. If these orbits are also inclined by 90° to the ecliptic plane, the planet orbit perturbations could have been minimal even if acceleration cancellation was not perfect. This would be especially true for planets that were all on the opposite side of the Sun from Nemesis during the passage. With this in mind, a search was made for significant planet alignments. On July 5, 2079 Mercury, Earth, Mars+180°, and Jupiter will align with each other at a mean polar longitude of 102.161°±0.206°. Nemesis A, a brown dwarf star, is expected to approach from the south and arrive 180° away at a perihelion longitude of 282.161°±0.206° and at a perihelion distance of 3.971 AU, the 3/2 resonance with Jupiter at that time. On July 13, 2079 Saturn, Uranus, and Neptune+180° will align at a mean polar longitude of 299.155°±0.008°. Nemesis B, a white dwarf star, is expected to approach from the north and arrive at that same longitude and at a perihelion distance of 67.25 AU, outside the Kuiper Belt.
    [Show full text]