NASA's Heliophysics Portfolio (IG-19-018)
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Fundamentals of Impulsive Energy Release in the Corona Heliophysics 2050 Workshop White Paper A
Heliophysics 2050 White Papers (2021) 4093.pdf Fundamentals of impulsive energy release in the corona Heliophysics 2050 Workshop white paper A. Y. Shih (NASA Goddard Space Flight Center), L. Glesener (UMN), S. Krucker (UCB), S. Guidoni (Amer. Univ.), S. Christe (GSFC), K. Reeves (SAO), S. Gburek (PAS), A. Caspi (SwRI), M. Alaoui (GSFC/CUA), J. Allred (GSFC), M. Battaglia (FHNW), W. Baumgartner (MSFC), B. Dennis (GSFC), J. Drake (UMD), K. Goetz (UMN), L. Golub (SAO), I. Hannah (Univ. of Glasgow), L. Hayes (GSFC/USRA), G. Holman (GSFC/Emeritus), A. Inglis (GSFC/CUA), J. Ireland (GSFC), G. Kerr (GSFC/CUA), J. Klimchuk (GSFC), D. McKenzie (MSFC), C. Moore (SAO), S. Musset (Univ. of Glasgow), J. Reep (NRL), D. Ryan (GSFC/AU), P. Saint-Hilaire (UCB), S. Savage (MSFC), R. Schwartz (GSFC/AU), D. Seaton (NOAA), M. Stęślicki (PAS), T. Woods (LASP) Introduction Solar eruptive events are the most energetic and geo-effective space-weather drivers. They originate in the corona near the Sun’s surface as a combination of solar flares (impulsive bursts of radiation across the entire electromagnetic spectrum) and coronal mass ejections (CMEs; expulsions of magnetized plasma into interplanetary space). The radiation and energetic particles they produce can damage satellites, disrupt telecommunications and GPS navigation, and endanger astronauts in space. Many of the processes involved in triggering, driving, and sustaining solar eruptive events–including magnetic reconnection, particle acceleration, plasma heating, and energy transport in magnetized plasmas–also play important roles in phenomena throughout the Universe, such as in magnetospheric substorms, gamma-ray bursts, and accretion disks. The Sun is a unique laboratory to better understand these fundamental physical processes. -
Space Climate Characterization Via Geomagnetic Indices. an Attempt of Integrating Solar, Heliospheric, and Geomagnetic Indices at Various Time-Scales
Geophysical Research Abstracts Vol. 15, EGU2013-8930, 2013 EGU General Assembly 2013 © Author(s) 2013. CC Attribution 3.0 License. Space climate characterization via geomagnetic indices. An attempt of integrating solar, heliospheric, and geomagnetic indices at various time-scales Crisan Demetrescu and Venera Dobrica Institute of Geodynamics, Bucharest, Romania ([email protected]) The so-called space climate concerns the long-term change in the Sun and its effects in the heliosphere and upon the Earth, including the atmosphere and climate. Annual means of measured and reconstructed solar, heliospheric, and magnetospheric parameters are used to infer solar activity signatures at the Hale and Gleissberg cycles timescales. Available open solar flux, modulation strength, cosmic ray flux, total solar irradiance data, reconstructed back to 1700, solar wind parameters (speed, density, dynamic pressure) and the magnitude of the heliospheric magnetic field at 1 AU, reconstructed back to 1870, as well as the time series of geomagnetic activity indices (aa, IDV, IHV), going back to 1870, have been considered. Also, shorter time series of some other geomagnetic indices, designed as proxies for specific current systems, such as the ring current and the auroral electrojet, that develop in the magnetosphere and ionosphere as a consequence of the interraction with the solar wind and heliosperic magnetic field (the Dst and, respectively, AE indices), as well as the merging electric field and convection in the polar ionosphere (the PC index) have been taken into -
Is Earth's Magnetic Field Reversing? ⁎ Catherine Constable A, , Monika Korte B
Earth and Planetary Science Letters 246 (2006) 1–16 www.elsevier.com/locate/epsl Frontiers Is Earth's magnetic field reversing? ⁎ Catherine Constable a, , Monika Korte b a Institute of Geophysics and Planetary Physics, Scripps Institution of Oceanography, University of California at San Diego, La Jolla, CA 92093-0225, USA b GeoForschungsZentrum Potsdam, Telegrafenberg, 14473 Potsdam, Germany Received 7 October 2005; received in revised form 21 March 2006; accepted 23 March 2006 Editor: A.N. Halliday Abstract Earth's dipole field has been diminishing in strength since the first systematic observations of field intensity were made in the mid nineteenth century. This has led to speculation that the geomagnetic field might now be in the early stages of a reversal. In the longer term context of paleomagnetic observations it is found that for the current reversal rate and expected statistical variability in polarity interval length an interval as long as the ongoing 0.78 Myr Brunhes polarity interval is to be expected with a probability of less than 0.15, and the preferred probability estimates range from 0.06 to 0.08. These rather low odds might be used to infer that the next reversal is overdue, but the assessment is limited by the statistical treatment of reversals as point processes. Recent paleofield observations combined with insights derived from field modeling and numerical geodynamo simulations suggest that a reversal is not imminent. The current value of the dipole moment remains high compared with the average throughout the ongoing 0.78 Myr Brunhes polarity interval; the present rate of change in Earth's dipole strength is not anomalous compared with rates of change for the past 7 kyr; furthermore there is evidence that the field has been stronger on average during the Brunhes than for the past 160 Ma, and that high average field values are associated with longer polarity chrons. -
Doc.10100.Space Weather Manual FINAL DRAFT Version
Doc 10100 Manual on Space Weather Information in Support of International Air Navigation Approved by the Secretary General and published under his authority First Edition – 2018 International Civil Aviation Organization TABLE OF CONTENTS Page Chapter 1. Introduction ..................................................................................................................................... 1-1 1.1 General ............................................................................................................................................... 1-1 1.2 Space weather indicators .................................................................................................................... 1-1 1.3 The hazards ........................................................................................................................................ 1-2 1.4 Space weather mitigation aspects ....................................................................................................... 1-3 1.5 Coordinating the response to a space weather event ......................................................................... 1-3 Chapter 2. Space Weather Phenomena and Aviation Operations ................................................................. 2-1 2.1 General ............................................................................................................................................... 2-1 2.2 Geomagnetic storms .......................................................................................................................... -
A Deep Learning Framework for Solar Phenomena Prediction
FlareNet: A Deep Learning Framework for Solar Phenomena Prediction FDL 2017 Solar Storm Team: Sean McGregor1, Dattaraj Dhuri1,2, Anamaria Berea1,3, and Andrés Muñoz-Jaramillo1,4 1NASA’s 2017 Frontier Development Laboratory 2Tata Institute of Fundamental Research (TIFR), Mumbai, India 3Center for Complexity in Business, University of Maryland, College Park, MD, USA 4SouthWest Research Institute, Boulder, CO, USA Abstract Solar activity can interfere with the normal operation of GPS satellites, the power grid, and space operations, but inadequate predictive models mean we have little warning for the arrival of newly disruptive solar activity. Petabytes of data col- lected from satellite instruments aboard the Solar Dynamics Observatory (SDO) provide a high-cadence, high-resolution, and many-channeled dataset of solar phenomena. Several challenging deep learning problems may be derived from the data, including space weather forecasting (i.e., solar flares, solar energetic particles, and coronal mass ejections). This work introduces a software framework, FlareNet, for experimentation within these problems. FlareNet includes compo- nents for the downloading and management of SDO data, visualization, and rapid experimentation. The system architecture is built to enable collaboration between heliophysicists and machine learning researchers on the topics of image regres- sion, image classification, and image segmentation. We specifically highlight the problem of solar flare prediction and offer insights from preliminary experiments. 1 Introduction The violent release of solar magnetic energy – collectively referred to as “space weather" – is responsible for a variety of phenomena that can disrupt technological assets. In particular, solar flares (sudden brightenings of the solar corona) and coronal mass ejections (CMEs; the violent release of solar plasma) can disrupt long-distance communications, reduce Global Positioning System (GPS) accuracy, degrade satellites, and disrupt the power grid [5]. -
Solar and Space Physics: a Science for a Technological Society
Solar and Space Physics: A Science for a Technological Society The 2013-2022 Decadal Survey in Solar and Space Physics Space Studies Board ∙ Division on Engineering & Physical Sciences ∙ August 2012 From the interior of the Sun, to the upper atmosphere and near-space environment of Earth, and outwards to a region far beyond Pluto where the Sun’s influence wanes, advances during the past decade in space physics and solar physics have yielded spectacular insights into the phenomena that affect our home in space. This report, the final product of a study requested by NASA and the National Science Foundation, presents a prioritized program of basic and applied research for 2013-2022 that will advance scientific understanding of the Sun, Sun- Earth connections and the origins of “space weather,” and the Sun’s interactions with other bodies in the solar system. The report includes recommendations directed for action by the study sponsors and by other federal agencies—especially NOAA, which is responsible for the day-to-day (“operational”) forecast of space weather. Recent Progress: Significant Advances significant progress in understanding the origin from the Past Decade and evolution of the solar wind; striking advances The disciplines of solar and space physics have made in understanding of both explosive solar flares remarkable advances over the last decade—many and the coronal mass ejections that drive space of which have come from the implementation weather; new imaging methods that permit direct of the program recommended in 2003 Solar observations of the space weather-driven changes and Space Physics Decadal Survey. For example, in the particles and magnetic fields surrounding enabled by advances in scientific understanding Earth; new understanding of the ways that space as well as fruitful interagency partnerships, the storms are fueled by oxygen originating from capabilities of models that predict space weather Earth’s own atmosphere; and the surprising impacts on Earth have made rapid gains over discovery that conditions in near-Earth space the past decade. -
Exploring the Sun with ALMA
Astronomical Science DOI: 10.18727/0722-6691/5065 Exploring the Sun with ALMA Timothy S. Bastian1 18 Space Vehicles Directorate, Air Force and to gain an understanding of how Miroslav Bárta2 Research Laboratory, Albuquerque, mechanical and radiative energy are Roman Brajša3 USA transferred through that atmospheric Bin Chen4 19 National Astronomical Observatories, layer. Bart De Pontieu5, 6 Chinese Academy of Sciences, Beijing, Dale E. Gary4 China Much of what is currently known about Gregory D. Fleishman4 the chromosphere has relied on spectro- Antonio S. Hales1, 7 scopic observations at optical and ultra- Kazumasa Iwai8 The Atacama Large Millimeter/submilli- violet wavelengths using both ground- Hugh Hudson9, 10 meter Array (ALMA) Observatory opens and space-based instrumentation. While Sujin Kim11, 12 a new window onto the Universe. The a lot of progress has been made, the Adam Kobelski13 ability to perform continuum imaging interpretation of such observations is Maria Loukitcheva4, 14, 15 and spectroscopy of astrophysical phe- complex because optical and ultraviolet Masumi Shimojo16, 17 nomena at millimetre and submillimetre lines in the chromosphere form under Ivica Skokić2, 3 wavelengths with unprecedented sen- conditions of non-local thermodynamic Sven Wedemeyer6 sitivity opens up new avenues for the equilibrium. In contrast, emission from Stephen M. White18 study of cosmology and the evolution the Sun’s chromosphere at millimetre Yihua Yan19 of galaxies, the formation of stars and and submillimetre wavelengths is more planets, and astrochemistry. ALMA also straightforward to interpret as the emis- allows fundamentally new observations sion forms under conditions of local 1 National Radio Astronomy Observatory, to be made of objects much closer to thermodynamic equilibrium and the Charlottesville, USA home, including the Sun. -
Predictability of the Variable Solar-Terrestrial Coupling Ioannis A
https://doi.org/10.5194/angeo-2020-94 Preprint. Discussion started: 26 January 2021 c Author(s) 2021. CC BY 4.0 License. Predictability of the variable solar-terrestrial coupling Ioannis A. Daglis1,15, Loren C. Chang2, Sergio Dasso3, Nat Gopalswamy4, Olga V. Khabarova5, Emilia Kilpua6, Ramon Lopez7, Daniel Marsh8,16, Katja Matthes9,17, Dibyendu Nandi10, Annika Seppälä11, Kazuo Shiokawa12, Rémi Thiéblemont13 and Qiugang Zong14 5 1Department of Physics, National and Kapodistrian University of Athens, 15784 Athens, Greece 2Department of Space Science and Engineering, Center for Astronautical Physics and Engineering, National Central University, Taiwan 3Department of Physics, Universidad de Buenos Aires, Buenos Aires, Argentina 10 4Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 5Solar-Terrestrial Department, Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of RAS (IZMIRAN), Moscow, 108840, Russia 6Department of Physics, University of Helsinki, Helsinki, Finland 7Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA 15 8National Center for Atmospheric Research, Boulder, CO 80305, USA 9GEOMAR Helmholtz Centre for Ocean Research, Kiel, Germany 10IISER, Kolkata, India 11Department of Physics, University of Otago, Dunedin, New Zealand 12Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan 20 13LATMOS, Universite Pierre et Marie Curie, Paris, France 14School of Earth and Space Sciences, Peking University, Beijing, China 15Hellenic Space Center, Athens, Greece 16Faculty of Engineering and Physical Sciences, University of Leeds, Leeds, UK 17Christian-Albrechts Universität, Kiel, Germany 25 Correspondence to: Ioannis A. Daglis ([email protected]) Abstract. In October 2017, the Scientific Committee on Solar-Terrestrial Physics (SCOSTEP) Bureau established a 30 committee for the design of SCOSTEP’s Next Scientific Program (NSP). -
Chapter 11 RADIO OBSERVATIONS of CORONAL MASS
Chapter 11 RADIO OBSERVATIONS OF CORONAL MASS EJECTIONS Angelos Vourlidas Solar Physics Branch, Naval Research Laboratory, Washington, DC [email protected] Abstract In this chapter we review the status of CME observations in radio wavelengths with an emphasis on imaging. It is an area of renewed interest since 1996 due to the upgrade of the Nancay radioheliograph in conjunction with the continu- ous coverage of the solar corona from the EIT and LASCO instruments aboard SOHO. Also covered are analyses of Nobeyama Radioheliograph data and spec- tral data from a plethora of spectrographs around the world. We will point out the shortcomings of the current instrumentation and the ways that FASR could contribute. A summary of the current understanding of the physical processes that are involved in the radio emission from CMEs will be given. Keywords: Sun: Corona, Sun: Coronal Mass Ejections, Sun:Radio 1. Coronal Mass Ejections 1.1 A Brief CME Primer A Coronal Mass Ejection (CME) is, by definition, the expulsion of coronal plasma and magnetic field entrained therein into the heliosphere. The event is detected in white light by Thompson scattering of the photospheric light by the coronal electrons in the ejected mass. The first CME was discovered on December 14, 1971 by the OSO-7 orbiting coronagraph (Tousey 1973) which recorded only a small number of events (Howard et al. 1975). Skylab ob- servations quickly followed and allowed the first study of CME properties ( Gosling et al. 1974). Observations from many thousands of events have been collected since, from a series of space-borne coronagraphs: Solwind (Michels et al. -
Heliophysics Division Space Weather Strategy HPAC, June 30 – July 1, 2020
Heliophysics Division Space Weather Strategy HPAC, June 30 – July 1, 2020 1 Heliophysics Space Weather Strategy This strategy outlines the goals and objectives of NASA Heliophysics Division with respect to space weather. It is consistent with the goals and agency responsibilities articulated in the 2019 National Space Weather Strategy and Action Plan, as well as the Agency’s efforts in human and robotic exploration. Context • Understanding space weather is the domain of Heliophysics. Space weather is the applied expression of Heliophysics. In Priority 1 of the 2020 NASA Science Plan, Strategy 1.4 pertains directly to space weather: Develop a Directorate-wide, target-user focused approach to applied programs, including Earth Science Applications, Space Weather, Planetary Defense, and ⁻ Space Situational Awareness. 2 Space Weather Strategy Vision • Advance the science of space weather to empower a technological society safely thriving on Earth and expanding into space. Mission • Establish a preeminent space weather capability that supports robotic and human space exploration and meets national, international, and societal needs by advancing measurement and analysis techniques, and by expanding knowledge and understanding for transitioning into improved operational space weather forecasts and nowcasts. 3 1. Observe • Advance observation techniques, technology, Goals and capability 2. Analyze • NASA plays a vital role in space • Advance research, analysis and modeling weather research by providing capability unique, significant, and exploratory 3. Predict observations and data streams for • Improve space weather forecast and nowcast theory, modeling, and data analysis capabilities research, and for operations. 4. Transition • NASA’s contributions to observing • Transition capabilities to operational and understanding space weather environments are critical for the success of the National and International space 5. -
A Decadal Strategy for Solar and Space Physics
Space Weather and the Next Solar and Space Physics Decadal Survey Daniel N. Baker, CU-Boulder NRC Staff: Arthur Charo, Study Director Abigail Sheffer, Associate Program Officer Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities to retain US scientific leadership • Provides well-respected source for priorities & scientific motivations to agencies, OMB, OSTP, & Congress” “Most useful approach: • Frame discussion identifying key science questions – Focus on what to do, not what to build – Discuss science breadth & depth (e.g., impact on understanding fundamentals, related fields & interdisciplinary research) • Explain measurements & capabilities to answer questions • Discuss complementarity of initiatives, relative phasing, domestic & international context” *From “The Role of NRC Decadal Surveys in Prioritizing Federal Funding for Science & Technology,” Jon Morse, Office of Science & Technology Policy (OSTP), NRC Workshop on Decadal Surveys, November 14-16, 2006 2 Context The Sun to the Earth—and Beyond: A Decadal Research Strategy in Solar and Space Physics Summary Report (2002) Compendium of 5 Study Panel Reports (2003) First NRC Decadal Survey in Solar and Space Physics Community-led Integrated plan for the field Prioritized recommendations Sponsors: NASA, NSF, NOAA, DoD (AFOSR and ONR) 3 Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities -
1859 Carrington Event
Sun – Part 28 - 1859 Carrington event Sunspots recorded by Richard Carrington, 1859 Aurora On 1 September 1859, English astronomer Richard Carrington continued the daytime heliographic measurements of sunspots from his observatory in Surrey, which he had begun in 1857. Sunspot number had been very high ever since 28 August, but, on this particular day, he became one of the first two people to independently make the first observation of a solar flare. The other observer was Richard Hodgson, an amateur astronomer with an observatory in Essex. What they saw, with the naked eye on a projection of the Sun through a telescope onto a screen, was a 'white light flare' in the Sun's photosphere. When Carrington learned that the nearby Kew Observatory magnetometer had concurrently recorded a crochet, an instantaneous perturbation of Earth's ionosphere, he connected the two, identifying that the flare he had observed was associated with the numerous sunspots he had observed during previous days and the terrestrial effects which had been experienced on Earth. The flare was associated with a massive coronal mass ejection (CME) which had begun the 150 million km journey from the Sun 18 hours earlier (normally it takes 3-4 days for a CME to reach Earth). It was proposed that this great speed was facilitated by an earlier CME which had 'cleared the way' a few days earlier. The CME which produced the flare on 1 September 1859 was part of the largest geomagnetic storm ever recorded by ground-based magnetometers. During the 1-2 September storm, aurorae were visible around the world, those in the Northern Hemisphere observed as far south as the Caribbean and sub-Saharan Africa.