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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 .......................................................................................................................... -
National Space Weather Program Implementation Plan, 2Nd Edition, July 2000
National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ The National Space Weather Program The Implementation Plan 2nd Edition July 2000 National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ NATIONAL SPACE WEATHER PROGRAM COUNCIL Mr. Samuel P. Williamson, Chairman Federal Coordinator Dr. David L. Evans Department of Commerce Colonel Michael A. Neyland, USAF Department of Defense Mr. Robert E. Waldron Department of Energy Mr. James F. Devine Department of the Interior Mr. David Whatley Department of Transportation Dr. Edward J. Weiler National Aeronautics and Space Administration Dr. Margaret S. Leinen National Science Foundation Lt Col Michael R. Babcock, USAF, Executive Secretary Office of the Federal Coordinator for Meteorological Services and Supporting Research National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ NATIONAL SPACE WEATHER PROGRAM Implementation Plan 2nd Edition Prepared by the Committee for Space Weather for the National Space Weather Program Council Office of the Federal Coordinator for Meteorology FCM-P31-2000 Washington, DC July 2000 National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ FOREWORD We are pleased to present this Second Edition of the National Space Weather Program Implementation Plan. We published the program's Strategic Plan in 1995 and the first Implementation Plan in 1997. In the intervening period, we have made tremendous progress toward our goals but much work remains to be accomplished to achieve our ultimate goal of providing the space weather observations, forecasts, and warnings needed by our Nation. -
Arxiv:2101.02901V2 [Astro-Ph.SR] 30 Jan 2021 Can Generate Superflares to Deeply and Statistically Understanding Superflare Uniqueness Compared with Solar flares
Draft version February 2, 2021 Typeset using LATEX default style in AASTeX62 Superflares, chromospheric activities and photometric variabilities of solar-type stars from the second-year observation of TESS and spectra of LAMOST Zuo-Lin Tu,1 Ming Yang,1, 2 H.-F. Wang,3, 4 and F. Y. Wang1, 2 1School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China 2Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China 3South−Western Institute for Astronomy Research, Yunnan University, Kunming, 650500, P. R. China 4LAMOST Fellow ABSTRACT In this work, 1272 superflares on 311 stars are collected from 22,539 solar-type stars from the second- year observation of Transiting Exoplanet Survey Satellite (TESS), which almost covered the northern hemisphere of the sky. Three superflare stars contain hot Jupiter candidates or ultrashort-period planet candidates. We obtain γ = −1:76 ± 0:11 of the correlation between flare frequency and flare energy (dN=dE / E−γ ) for all superflares and get β = 0:42±0:01 of the correlation between superflare duration β and energy (Tduration / E ), which supports that a similar mechanism is shared by stellar superflares and solar flares. Stellar photometric variability (Rvar) is estimated for all solar-type stars, and the 3=2 relation of E / Rvar is included. An indicator of chromospheric activity (S-index) is obtained by using data from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) for 7454 solar-type stars. Distributions of these two properties indicate that the Sun is generally less active than superflare stars. -
High Dispersion Spectroscopy of Solar-Type Superflare Stars. I
High Dispersion Spectroscopy of Solar-type Superflare Stars. I. Temperature, Surface Gravity, Metallicity, and v sini Yuta Notsu1, Satoshi Honda2, Hiroyuki Maehara3,4, Shota Notsu1, Takuya Shibayama5, Daisaku Nogami1,6, and Kazunari Shibata6 [email protected] 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502 2Center for Astronomy, University of Hyogo, 407-2, Nishigaichi, Sayo-cho, Sayo, Hyogo 679-5313 3Kiso Observatory, Institute of Astronomy, School of Science, The University of Tokyo, 10762-30, Mitake, Kiso-machi, Kiso-gun, Nagano 397-0101 4Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232 5Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601 6Kwasan and Hida Observatories, Kyoto University, Yamashina-ku, Kyoto 607-8471 (Received 29-Sep-2014; accepted 26-Dec-2014) Abstract We conducted high dispersion spectroscopic observations of 50 superflare stars with Subaru/HDS, and measured the stellar parameters of them. These 50 targets were selected from the solar-type (G-type main sequence) superflare stars that we had discovered from the Kepler photometric data. As a result of these spectroscopic observations, we found that more than half (34 stars) of our 50 targets have no evidence of binary system. We then estimated effective temperature (Teff ), surface gravity (logg), metallicity ([Fe/H]), and projected rotational velocity (v sini) of these arXiv:1412.8243v2 [astro-ph.SR] 4 Mar 2015 34 superflare stars on the basis of our spectroscopic data. The accuracy of our esti- mations is higher than that of Kepler Input Catalog (KIC) values, and the differences between our values and KIC values ((∆T ) 219K, (∆log g) 0.37 dex, and eff rms ∼ rms ∼ (∆[Fe/H]) 0.46 dex) are comparable to the large uncertainties and systematic rms ∼ differences of KIC values reported by the previous researches. -
Where Is the Best Site on Earth? Domes A, B, C, and F, And
Where is the best site on Earth? Saunders et al. 2009, PASP, 121, 976-992 Where is the best site on Earth? Domes A, B, C and F, and Ridges A and B Will Saunders1;2, Jon S. Lawrence1;2;3, John W.V. Storey1, Michael C.B. Ashley1 1School of Physics, University of New South Wales 2Anglo-Australian Observatory 3Macquarie University, New South Wales [email protected] Seiji Kato, Patrick Minnis, David M. Winker NASA Langley Research Center Guiping Liu Space Sciences Lab, University of California Berkeley Craig Kulesa Department of Astronomy and Steward Observatory, University of Arizona Saunders et al. 2009, PASP, 121 976992 Received 2009 May 26; accepted 2009 July 13; published 2009 August 20 ABSTRACT The Antarctic plateau contains the best sites on earth for many forms of astronomy, but none of the existing bases was selected with astronomy as the primary motivation. In this paper, we try to systematically compare the merits of potential observatory sites. We include South Pole, Domes A, C and F, and also Ridge B (running NE from Dome A), and what we call `Ridge A' (running SW from Dome A). Our analysis combines satellite data, published results and atmospheric models, to compare the boundary layer, weather, aurorae, airglow, precipitable water vapour, thermal sky emission, surface temperature, and the free atmosphere, at each site. We ¯nd that all Antarctic sites are likely to be compromised for optical work by airglow and aurorae. Of the sites with existing bases, Dome A is easily the best overall; but we ¯nd that Ridge A o®ers an even better site. -
Superflares and Giant Planets
Superflares and Giant Planets From time to time, a few sunlike stars produce gargantuan outbursts. Large planets in tight orbits might account for these eruptions Eric P. Rubenstein nvision a pale blue planet, not un- bushes to burst into flames. Nor will the lar flares, which typically last a fraction Elike the Earth, orbiting a yellow star surface of the planet feel the blast of ul- of an hour and release their energy in a in some distant corner of the Galaxy. traviolet light and x rays, which will be combination of charged particles, ul- This exercise need not challenge the absorbed high in the atmosphere. But traviolet light and x rays. Thankfully, imagination. After all, astronomers the more energetic component of these this radiation does not reach danger- have now uncovered some 50 “extra- x rays and the charged particles that fol- ous levels at the surface of the Earth: solar” planets (albeit giant ones). Now low them are going to create havoc The terrestrial magnetic field easily de- suppose for a moment something less when they strike air molecules and trig- flects the charged particles, the upper likely: that this planet teems with life ger the production of nitrogen oxides, atmosphere screens out the x rays, and and is, perhaps, populated by intelli- which rapidly destroy ozone. the stratospheric ozone layer absorbs gent beings, ones who enjoy looking So in the space of a few days the pro- most of the ultraviolet light. So solar up at the sky from time to time. tective blanket of ozone around this flares, even the largest ones, normally During the day, these creatures planet will largely disintegrate, allow- pass uneventfully. -
Response of the Total Electron Content at Brazilian Low Latitudes to Corotating Interaction Region and High‑Speed Streams During Solar Minimum 2008 Claudia M
Candido et al. Earth, Planets and Space (2018) 70:104 https://doi.org/10.1186/s40623-018-0875-8 FULL PAPER Open Access Response of the total electron content at Brazilian low latitudes to corotating interaction region and high‑speed streams during solar minimum 2008 Claudia M. N. Candido1,2*, Inez S. Batista2, Virginia Klausner3, Patricia M. de Siqueira Negreti2, Fabio Becker‑Guedes2, Eurico R. de Paula2, Jiankui Shi1 and Emilia S. Correia2,4 Abstract In this work, we investigate the Brazilian low-latitude ionospheric response to two corotating interaction regions (CIRs) and high-speed streams (HSSs) events during the solar minimum of solar cycle 23, in 2008. The studied inter‑ vals are enclosed in the whole heliospheric interval, studied by other authors, for distinct longitudinal sectors. CIRs/ HSSs are structures commonly observed during the descending and low solar activity, and they are related to the occurrence of coronal holes. These events cause weak-to-moderate recurrent geomagnetic storms characterized by negative excursions of the interplanetary magnetic feld, IMF_Bz, as well as long-duration auroral activity, consid‑ ered as a favorable scenario for continuous prompt penetration interplanetary electric feld (PPEF). In this study, we used the vertical total electron content (VTEC) calculated from GPS receivers database from the Brazilian Continu‑ ous Monitoring Network managed by the Brazilian Institute of Geography and Statistics. Moreover, we analyzed the F-layer peak height, hmF2 and the critical plasma frequency, foF2, taken from a Digisonde installed at the southern crest of the equatorial ionization anomaly, in Cachoeira Paulista, CP. It was observed that during the CIRs/HSSs-driven geomagnetic disturbances VTEC increased more than 120% over the quiet times averaged values, which is compa‑ rable to intense geomagnetic storms. -
Benchmark Geomagnetic Disturbance Event Description
Benchmark Geomagnetic Disturbance Event Description Project 2013-03 GMD Mitigation Standard Drafting Team May 12, 2016 NERC | Report Title | Report Date 1 of 23 Table of Contents Preface ........................................................................................................................................................................3 Introduction ................................................................................................................................................................4 Background .............................................................................................................................................................4 General Characteristics ...........................................................................................................................................4 Benchmark GMD Event Description ...........................................................................................................................5 Reference Geoelectric Field Amplitude ..................................................................................................................5 Reference Geomagnetic Field Waveshape .............................................................................................................5 Appendix I – Technical Considerations .......................................................................................................................8 Statistical Considerations ........................................................................................................................................8 -
Solar and Geomagnetic Activity During March 1989 and Later Honths and Their Consequences at Earth and in Near-Earth Space
SOLAR AND GEOMAGNETIC ACTIVITY DURING MARCH 1989 AND LATER HONTHS AND THEIR CONSEQUENCES AT EARTH AND IN NEAR-EARTH SPACE J. H. Allen (NOAA/NESDIS/NGDC) Spacecraft Charging Technology Conference Naval Postgraduate School, Monterey, California October 31-November 3, 1989 ABSTRACT From 6-20 March 1989 the large, complex sunspot group Region 5395 rotated across the visible disc of the Sun producing many large flares that bombdrded Earth with a variety of intense radiation although the energetic particle spectra were unusually "soft". Aurorae were observed worldwide at low latitudes. On 13/14 March a "Great" magnetic storm occurred for which Ap* = 279 and AA* = 450. By both measures, this event rates among the largest historical magnetic storms. Geostationary sate1 1 i tes became interpl anetary monitors when the magnetopause moved earthward of 6.5 Re. Ionospheric condi- ticns were extremely disturbed, affecting hf through X-band comnunications and the operation of satellites used for surveys and navigation. At lower altitudes there were problems with satellite drag and due to the large mag- netic field changes associated with field-a1 igned current sheets. We are seeking reports of satellite anomalies at all altitudes. Reports also have been received about effects of these Sol ar-Terrestria1 di sturbances on other technology at Earth and in near-Earth space. This presentation draws heavily on material in a shorter, summary paper "iri prgss" for "EOS" (Allen, et. al., 1989). Recent major solar activity since the abstract. was submitted happened in mid-August, late September, and mid-October 1989. These events and their consequences at Earth and in Space are covered briefly. -
Arxiv:1907.12580V3 [Astro-Ph.SR] 5 Sep 2019 the Role of Magnetic Activity on Planetary Habitability Is a Currently Actively Studied field of Research (See Scalo Et Al
Draft version September 6, 2019 Typeset using LATEX default style in AASTeX62 Flaring activity of Proxima Centauri from TESS observations: quasi-periodic oscillations during flare decay and inferences on the habitability of Proxima b Krisztian´ Vida,1 Katalin Olah´ ,1 Zsolt Kov} ari´ ,1 Lidia van Driel-Gesztelyi,1, 2, 3 Attila Moor,´ 1 and Andras´ Pal´ 1 1Konkoly Observatory, MTA CSFK, H-1121 Budapest, Konkoly Thege M. ´ut15-17, Hungary 2University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK 3LESIA, Observatoire de Paris, Universit´ePSL, CNRS, Sorbonne Universit´e,Universit´ede Paris, 5 place Jules Janssen, 92195 Meudon, France (Received; Revised; Accepted) Submitted to ApJ ABSTRACT We analyze the light curve of the M5.5 dwarf Proxima Centauri obtained by the TESS in Sectors 11 and 12. In the ≈ 50 day-long light curve we identified and analyzed 72 flare events. The flare rate was 1.49 events per day, in total, 7.2% of the data was classified as flaring. The estimated flare energies were in the order of 1030 − 1032 ergs in the TESS passband (≈ 4:8× higher in bolometric energies, but in the same order of magnitude). Most of the eruptions appeared in groups. Two events showed quasi- periodic oscillations during their decay phase with a time scale of a few hours, that could be caused by quasiperiodic motions of the emitting plasma or oscillatory reconnection. From the cumulative flare frequency distribution we estimate that superflares with energy output of 1033 ergs are expected to occur three times per year, while a magnitude larger events (with 1034 ergs) can occur every second year. -
Improvement of Global Ionospheric TEC Derivation with Multi-Source Data in Modip Latitude
atmosphere Article Improvement of Global Ionospheric TEC Derivation with Multi-Source Data in Modip Latitude Weizheng Fu 1,2 , Guanyi Ma 1,3,* , Weijun Lu 1,3 , Takashi Maruyama 4, Jinghua Li 1, Qingtao Wan 1, Jiangtao Fan 1 and Xiaolan Wang 1 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (W.F.); [email protected] (W.L.); [email protected] (J.L.); [email protected] (Q.W.); [email protected] (J.F.); [email protected] (X.W.). 2 Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan 3 School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China 4 National Institute of Information and Communications Technology, Tokyo 183-8795, Japan; [email protected] * Correspondence: [email protected] Abstract: Global ionospheric total electron content (TEC) is generally derived with ground-based Global Navigation Satellite System (GNSS) observations based on mathematical models in a solar- geomagnetic reference frame. However, ground-based observations are not well-distributed. There is a lack of observations over sparsely populated areas and vast oceans, where the accuracy of TEC derivation is reduced. Additionally, the modified dip (modip) latitude is more suitable than geomagnetic latitude for the ionosphere. This paper investigates the improvement of global TEC with multi-source data and modip latitude, and a simulation with International Reference Ionosphere (IRI) model is developed. Compared with using ground-based observations in geomagnetic latitude, the mean improvement was about 10.88% after the addition of space-based observations and the adoption Citation: Fu, W.; Ma, G.; Lu, W.; of modip latitude. -
Extras Discovery of an X-Ray Superflare from an L Dwarf
A&A 634, L13 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937163 & c ESO 2020 Astrophysics LETTER TO THE EDITOR EXTraS discovery of an X-ray superflare from an L dwarf Andrea De Luca1,2, Beate Stelzer3,4, Adam J. Burgasser5, Daniele Pizzocaro1, Piero Ranalli6, Stefanie Raetz3, Martino Marelli1, Giovanni Novara7, Cristian Vignali8,9, Andrea Belfiore1, Paolo Esposito7, Paolo Franzetti1, Marco Fumana1, Roberto Gilli9, Ruben Salvaterra1, and Andrea Tiengo7,2 1 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, Via A. Corti 12, 20133 Milano, Italy e-mail: [email protected] 2 INFN, Sezione di Pavia, Via A. Bassi 6, 27100 Pavia, Italy 3 Institut für Astronomie and Astrophysik Tübingen, Eberhard-Karls Universität Tübingen, Sand 1 72076, Germany 4 INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy 5 Center for Astrophysics and Space Science, University of California San Diego, 9500 Gilman Drive, La Jolla, CA 92092, USA 6 Combient Mix AB, Kyrkogatan 22, 41115 Gothenburg, Sweden 7 Scuola Universitaria Superiore IUSS Pavia, Piazza della Vittoria 15, 27100 Pavia, Italy 8 Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, Via P. Gobetti 93/2, 40129 Bologna, Italy 9 INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via P. Gobetti 93/3, 40129 Bologna, Italy Received 21 November 2019 / Accepted 7 January 2020 ABSTRACT We present the first detection of an X-ray flare from an ultracool dwarf of spectral class L. The event was identified in the EXTraS database of XMM-Newton variable sources, and its optical counterpart, J0331−27, was found through a cross-match with the Dark Energy Survey Year 3 release.