Helios Solar Storm Scenario
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General Disclaimer One Or More of the Following Statements May Affect
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) NASA Technical Memorandum 85094 SOLAR RADIO BURST AND IN SITU DETERMINATION OF INTERPLANETARY ELECTRON DENSITY (NASA-^'M-85094) SOLAR RADIO BUFST AND IN N83-35989 SITU DETERMINATION OF INTEFPIAKETARY ELECTRON DENSITY SNASA) 26 p EC A03/MF A01 CSCL 03B Unclas G3/9.3 492134 J. L. Bougeret, J. H. King and R. Schwenn OCT Y'183 RECEIVED NASA Sri FACIUTY ACCESS DEPT. September 1883 I 3 National Aeronautics and Space Administration Goddard Spne Flight Center Greenbelt, Maryland 20771 k it R ^ f A SOLAR RADIO BURST AND IN SITU DETERMINATION OF INTERPLANETARY ELECTRON DENSITY J.-L. Bou eret * J.H. Kinr ^i Laboratory for Extraterrestrial Physics, NASA/Goddard Space Flight. Center, Greenbelt, Maryland 20771, U.S.A. and R. Schwenn Max-Planck-Institut fOr Aeronomie, Postfach 20, D-3411 Katlenburg-Lindau, Federal Republic of Germany - 2 - °t i t: ABSTRACT i • We review and discuss a few interplanetary electron density scales which have been derived from the analysis of interplanetary solar radio bursts, and we compare them to a model derived from 1974-1980 Helioi 1 and 2 in situ i i density observations made in the 0.3-1.0 AU range. -
UC Irvine UC Irvine Previously Published Works
UC Irvine UC Irvine Previously Published Works Title Astrophysics in 2006 Permalink https://escholarship.org/uc/item/5760h9v8 Journal Space Science Reviews, 132(1) ISSN 0038-6308 Authors Trimble, V Aschwanden, MJ Hansen, CJ Publication Date 2007-09-01 DOI 10.1007/s11214-007-9224-0 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Space Sci Rev (2007) 132: 1–182 DOI 10.1007/s11214-007-9224-0 Astrophysics in 2006 Virginia Trimble · Markus J. Aschwanden · Carl J. Hansen Received: 11 May 2007 / Accepted: 24 May 2007 / Published online: 23 October 2007 © Springer Science+Business Media B.V. 2007 Abstract The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords Cosmology: general · Galaxies: general · ISM: general · Stars: general · Sun: general · Planets and satellites: general · Astrobiology · Star clusters · Binary stars · Clusters of galaxies · Gamma-ray bursts · Milky Way · Earth · Active galaxies · Supernovae 1 Introduction Astrophysics in 2006 modifies a long tradition by moving to a new journal, which you hold in your (real or virtual) hands. The fifteen previous articles in the series are referenced oc- casionally as Ap91 to Ap05 below and appeared in volumes 104–118 of Publications of V. -
Progress in Space Weather Modeling in an Operational Environment
J. Space Weather Space Clim. 3 (2013) A17 DOI: 10.1051/swsc/2013037 Ó I. Tsagouri et al., Published by EDP Sciences 2013 RESEARCH ARTICLE OPEN ACCESS Progress in space weather modeling in an operational environment Ioanna Tsagouri1,*, Anna Belehaki1, Nicolas Bergeot2,3, Consuelo Cid4,Ve´ronique Delouille2,3, Tatiana Egorova5, Norbert Jakowski6, Ivan Kutiev7, Andrei Mikhailov8, Marlon Nu´n˜ez9, Marco Pietrella10, Alexander Potapov11, Rami Qahwaji12, Yurdanur Tulunay13, Peter Velinov7, and Ari Viljanen14 1 National Observatory of Athens, P. Penteli, Greece *Corresponding author: e-mail: [email protected] 2 Solar-Terrestrial Centre of Excellence, Brussels, Belgium 3 Royal Observatory of Belgium, Brussels, Belgium 4 Universidad de Alcala´, Alcala´ de Henares, Spain 5 Physikalisch-Meteorologisches Observatorium Davos and World Radiation Center (PMOD/WRC), Davos, Switzerland 6 German Aerospace Center, Institute of Communications and Navigation, Neustrelitz, Germany 7 Bulgarian Academy of Sciences, Sofia, Bulgaria 8 Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Troitsk, Moscow Region, Russia 9 Universidad de Ma´laga, Ma´laga, Spain 10 Istituto Nazionale di Geofisica e Vulcanologia, Rome, Italy 11 Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia 12 University of Bradford, Bradford, UK 13 Middle East Technical University, Ankara, Turkey 14 Finnish Meteorological Institute, Helsinki, Finland Received 19 June 2012 / Accepted 10 March 2013 ABSTRACT This paper aims at providing an overview of latest advances in space weather modeling in an operational environment in Europe, including both the introduction of new models and improvements to existing codes and algorithms that address the broad range of space weather’s prediction requirements from the Sun to the Earth. -
Radial Variation of the Interplanetary Magnetic Field Between 0.3 AU and 1.0 AU
|00000575|| J. Geophys. 42, 591 - 598, 1977 Journal of Geophysics Radial Variation of the Interplanetary Magnetic Field between 0.3 AU and 1.0 AU Observations by the Helios-I Spacecraft G. Musmann, F.M. Neubauer and E. Lammers Institut for Geophysik and Meteorologie, Technische Universitiit Braunschweig, Mendelssohnstr. lA, D-3300 Braunschweig, Federal Republic of Germany Abstract. We have investigated the radial dependence of the radial and azimuthal components and the magnitude of the interplanetary magnetic field obtained by the Technical University of Braunschweig magnetometer experiment on-board of Helios-1 from December 10, 1974 to first perihelion on March 15, 1975. Absolute values of daily averages of each quantity have been employed. The regression analysis based on power laws leads to 2.55 y x r- 2 · 0 , 2.26 y x r- i.o and F = 5.53 y x r- i. 6 with standard deviations of 2.5 y, 2.0 y and 3.2 y for the radial and azimuthal components and magnitude, respectively. Here r is the radial distance from the sun in astronomical units. The results are compared with results obtained for Mariners 4, 5 and 10 and Pioneers 6 and 10. The differences are probably due to different epochs in the solar cycle and the different statistical techniques used. Key words: Interplanetary magnetic field - Helios-1 results. Introduction The study of the vanat10n of the components and magnitude of the in terplanetary magnetic field with heliocentric distance is very intersting at the present time. The mission of Mariner 10 to the inner solar system to a heliocentric distance of 0.46 AU and the missions of Pioneer 10 and Pioneer 11 to the outer solar system to heliocentric distances beyond 5 AU have provided new data over a wide range of heliocentric distance. -
Event Report
Event Report 5th AUSTRALIA-SPAIN RESEARCH FORUM 7 November 2019 Australian National University, Canberra Some highlights Convenor, Professor Luis Salvador- Carulla, and other presenters were 01 interviewed by 2XX Community Radio Professor Carlos Garcia-Alonso accepts the Malaspina Award 2019 on behalf of Loyola University Andalusia, Spain, from the Ambassador of Spain in Australia, His Excellency, 02 Mr Manuel Cacho. Artwork from acclaimed Spanish artist, Oscar Martin de Burgos featured in this 03 year’s activities. 5th AUSTRALIA-SPAIN RESEARCH FORUM 7 November 2019, ANU P a g e | 2 5 years bridging Australia and Spain in research and academia The 5th Australia-Spain Research Forum celebrated five years of international research collaboration. Background The Association of Spanish Researchers in Australia-Pacific (SRAP) presents an annual multidisciplinary seminar aimed at the wider community, to highlight Australia-Spain research and present broad research and cultural topics which are of special interest to the Australian and Spanish societies. This year's forum was designed to highlight the successes and challenges of international collaboration in research and academia. The 5th Australia-Spain Research Forum: 5 years Bridging Australia and Spain in Research and Academia, held on Thursday 7 November 2019, in Canberra, Australia, brought together a diverse range of accomplished speakers who reflected on international partnerships and presented a number of case studies about the roles of funding agencies, universities and research organisations -
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. -
The Grand Aurorae Borealis Seen in Colombia in 1859
The Grand Aurorae Borealis Seen in Colombia in 1859 Freddy Moreno C´ardenasa, Sergio Cristancho S´ancheza, Santiago Vargas Dom´ınguezb aCentro de Estudios Astrof´ısicos, Gimnasio Campestre, Bogot´a, Colombia bUniversidad Nacional de Colombia - Sede Bogot´a- Facultad de Ciencias - Observatorio Astron´omico - Carrera 45 # 26-85, Bogot´a- Colombia Abstract On Thursday, September 1, 1859, the British astronomer Richard Car- rington, for the first time ever, observes a spectacular gleam of visible light on the surface of the solar disk, the photosphere. The Carrington Event, as it is nowadays known by scientists, occurred because of the high solar activity that had visible consequences on Earth, in particular reports of outstanding aurorae activity that amazed thousands of people in the western hemisphere during the dawn of September 2. The geomagnetic storm, generated by the solar-terrestrial event, had such a magnitude that the auroral oval expanded towards the equator, allowing low latitudes, like Panama's 9◦N, to catch a sight of the aurorae. An expedition was carried out to review several his- torical reports and books from the northern cities of Colombia allowed the identification of a narrative from Monter´ıa,Colombia (8◦ 45' N), that de- scribes phenomena resembling those of an aurorae borealis, such as fire-like lights, blazing and dazzling glares, and the appearance of an immense S-like shape in the sky. The very low latitude of the geomagnetic north pole in 1859, the lowest value in over half a millennia, is proposed to have allowed the observations of auroral events at locations closer to the equator, and supports the historical description found in Colombia. -
An Opposite Response of the Low-Latitude Ionosphere at Asian
Originally published as: Xiong, C., Lühr, H., Yamazaki, Y. (2019): An Opposite Response of the Low‐Latitude Ionosphere at Asian and American Sectors During Storm Recovery Phases: Drivers From Below or Above. - Journal of Geophysical Research, 124, 7, pp. 6266—6280. DOI: http://doi.org/10.1029/2019JA026917 RESEARCH ARTICLE An Opposite Response of the Low‐Latitude Ionosphere at 10.1029/2019JA026917 Asian and American Sectors During Storm Recovery Key Points: • The dayside low‐latitude ionosphere Phases: Drivers From Below or Above – on 9 11 September 2017 exhibits Chao Xiong1 , Hermann Lühr1 , and Yosuke Yamazaki1 prominent positive/negative responses at the Asian/American 1GFZ German Research Centre for Geosciences, Potsdam, Germany sectors • The global distribution of thermospheric O/N2 ratio measured by GUVI cannot well explain such Abstract In this study, we focus on the recovery phase of a geomagnetic storm that happened on 6–11 longitudinal opposite response of September 2017. The ground‐based total electron content data, as well as the F region in situ electron ionosphere density, measured by the Swarm satellites show an interesting feature, revealing at low and equatorial • We suggest lower atmospheric forcing the main contributor to the latitudes on the dayside ionosphere prominent positive and negative responses at the Asian and American longitudinal opposite response of longitudinal sectors, respectively. The global distribution of thermospheric O/N2 ratio measured by global – ionosphere on 9 11 September 2017 ultraviolet imager on board the Thermosphere, Ionosphere, Mesosphere Energetics and Dynamics satellite cannot well explain such longitudinally opposite response of the ionosphere. Comparison between the equatorial electrojet variations from stations at Huancayo in Peru and Davao in the Philippines suggests that Correspondence to: the longitudinally opposite ionospheric response should be closely associated with the interplay of E C. -
Solar Flare: the "Carrington Event" of 1859
Chas' Compilation: Solar Flare: The "Carrington Event" of 1859 Chas' Compilation A compilation of information and links regarding assorted subjects: politics, religion, science, computers, health, movies, music... essentially whatever I'm reading about, working on or experiencing in life. Saturday, August 08, 2009 About Me Solar Flare: The "Carrington Event" of 1859 Name: Chas Sprague Location: State of In a post I did a few days ago, about sunspot activity, the famous solar storm of 1859, Jefferson, United States often referred to as the "Carrington Event", was frequently mentioned. I've been I was born and raised in reading up on that, and here is some of the information I found: Connecticut, went to college in Boston, dropped out, moved A Super Solar Flare west to San Francisco where I lived for 23 years. I now live in rural Oregon, At 11:18 AM on the cloudless morning of Thursday, September 1, 1859, enjoying a lifestyle I've longed for. 33-year-old Richard Carrington—widely acknowledged to be one of England's foremost solar astronomers—was in his well-appointed private View my complete profile observatory. Just as usual on every sunny day, his telescope was projecting an 11-inch-wide image of the sun on a screen, and Carrington Previous Posts skillfully drew the sunspots he saw. ● True Health Care Reform: Reduce On that morning, he was capturing the likeness of an enormous group of the "Wedge" sunspots. Suddenly, before his eyes, two brilliant beads of blinding white ● Obama Supporters Can't Take a light appeared over the sunspots, intensified rapidly, and became kidney- Joke shaped. -
Midlatitude Ionospheric F2-Layer Response to Eruptive Solar Events
Midlatitude ionospheric F2-layer response to eruptive solar events-caused geomagnetic disturbances over Hungary during the maximum of the solar cycle 24: a case study K. A. Berényi *,1,2, V. Barta 2, Á. Kis 2 1 Eötvös Loránd University, Budapest, Hungary 2 Research Centre for Astronomy and Earth Sciences, GGI, Hungarian Academy of Sciences, Sopron, Hungary Published in Advances in Space Research Abstract In our study we analyze and compare the response and behavior of the ionospheric F2 and of the sporadic E-layer during three strong (i.e., Dst <-100nT) individual geomagnetic storms from years 2012, 2013 and 2015, winter time period. The data was provided by the state-of the art digital ionosonde of the Széchenyi István Geophysical Observatory located at midlatitude, Nagycenk, Hungary (IAGA code: NCK, geomagnetic lat.: 46,17° geomagnetic long.: 98,85°). The local time of the sudden commencement (SC) was used to characterize the type of the ionospheric storm (after Mendillo and Narvaez, 2010). This way two regular positive phase (RPP) ionospheric storms and one no-positive phase (NPP) storm have been analyzed. In all three cases a significant increase in electron density of the foF2 layer can be observed at dawn/early morning (around 6:00 UT, 07:00 LT). Also we can observe the fade-out of the ionospheric layers at night during the geomagnetically disturbed time periods. Our results suggest that the fade-out effect is not connected to the occurrence of the sporadic E-layers. Keywords: ionospheric storm, geomagnetic disturbance, space weather, midlatitude F2-layer, sporadic E-layer *Corresponding author. -
Extreme Solar Eruptions and Their Space Weather Consequences Nat
Extreme Solar Eruptions and their Space Weather Consequences Nat Gopalswamy NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Abstract: Solar eruptions generally refer to coronal mass ejections (CMEs) and flares. Both are important sources of space weather. Solar flares cause sudden change in the ionization level in the ionosphere. CMEs cause solar energetic particle (SEP) events and geomagnetic storms. A flare with unusually high intensity and/or a CME with extremely high energy can be thought of examples of extreme events on the Sun. These events can also lead to extreme SEP events and/or geomagnetic storms. Ultimately, the energy that powers CMEs and flares are stored in magnetic regions on the Sun, known as active regions. Active regions with extraordinary size and magnetic field have the potential to produce extreme events. Based on current data sets, we estimate the sizes of one-in-hundred and one-in-thousand year events as an indicator of the extremeness of the events. We consider both the extremeness in the source of eruptions and in the consequences. We then compare the estimated 100-year and 1000-year sizes with the sizes of historical extreme events measured or inferred. 1. Introduction Human society experienced the impact of extreme solar eruptions that occurred on October 28 and 29 in 2003, known as the Halloween 2003 storms. Soon after the occurrence of the associated solar flares and coronal mass ejections (CMEs) at the Sun, people were expecting severe impact on Earth’s space environment and took appropriate actions to safeguard technological systems in space and on the ground. -
Saturday, 28 March 2020 EASTERN STATES (NSW, ACT
WEEK 13: Sunday, 22 March - Saturday, 28 March 2020 EASTERN STATES (NSW, ACT, TAS, VIC) Start Consumer Closed Date Genre Title Episode Title Series Episode TV Guide Text Country of Origin Language Year Repeat Classification Subtitles Time Advice Captions 2020-03-22 0500 News - Overseas Korean News Korean News 0 News via satellite from YTN Korea, in Korean, no subtitles. SOUTH KOREA Korean-100 2013 NC 2020-03-22 0530 News - Overseas Indonesian News Indonesian News 0 News via satellite from TVRI Jakarta, in Indonesian, no subtitles. INDONESIA Indonesian-100 2013 NC 2020-03-22 0610 News - Overseas Hong Kong News Hong Kong News 0 News via satellite from TVB Hong Kong, in Cantonese, no subtitles. HONG KONG Cantonese-100 2013 NC 2020-03-22 0630 News - Overseas Chinese News Chinese News 0 News via satellite from CCTV Beijing, in Mandarin, no subtitles. CHINA Mandarin-100 2013 NC 2020-03-22 0700 News - Overseas Russian News Russian News 0 News via satellite from NTV Moscow, in Russian, no subtitles. RUSSIA Russian-100 2013 NC 2020-03-22 0730 News - Overseas Polish News Polish News 0 Wydarzenia from Polsat in Warsaw via satellite, in Polish, no subtitles. POLAND Polish-100 2013 NC News from Public Broadcasting Services Limited, Malta, in Maltese, no 2020-03-22 0800 News - Overseas Maltese News Maltese News 0 MALTA Maltese-100 2013 NC subtitles. News via satellite from public broadcaster MRT in Skopje, in 2020-03-22 0830 News - Overseas Macedonian News Macedonian News 0 MACEDONIA Macedonian-100 2013 NC Macedonian, no subtitles. 2020-03-22 0900 News - Overseas Croatian News Croatian News 0 News via satellite from HRT Croatia, in Croatian, no subtitles.