DEUTSCHE WELLE SOLAR GEOPHYSICAL ACTIVITY REPORT FEBRUARY 2007
|
|
- Ronald Thompson
- 5 years ago
- Views:
Transcription
1 SOLAR GEOPHYSICAL ACTIVITY REPORT FEBRUARY 2007 Steffen Hilbig Mess- und Kontrollzentrale
2 SOLAR GEOPHYSICAL ACTIVITY REPORT February 2007 Aurora Borealis Steffen Hilbig
3 Solar Geophysical Activity Summary 2 Contents... 2 Introduction.. 3 Review.. 4, 5 Solar Images of January , 7, 8 Diagram: Solar Indices (Solar Flux, Sunspot Numbers, Ap-Index) 9 Diagram: Solar Wind Velocity (daily values) Diagram: Solar Wind (development). 11 Diagram: Solar Wind Density (daily values) Diagram: Solar Wind Density (development) Diagram: Planetary A - Indices (daily values).. 14 Diagram: Planetary A - Indices (development) Diagram: Planetary K - Indices (daily values).. 16 Diagram: Planetary K - Indices (development) Diagram: Geomagnetic Activity Diagram: IMF Field B-Components (daily max values)... 19, 20 Northern Auroral Oval Images 21, 22, 23 Northern Auroral Oval Description 24 Space Weather Scales (Ap - Indices) Space Weather Scales (Kp - Indices).. 26 Space Weather Scales (correlation of Ap to Kp Indices) Space Weather Scales (Solar Flares) Diagram: Solar Flares (daily values) Diagram: Solar Flares (development) Long Distance Propagation Summary.. 31, 32 Diagram: Solar Cycles 22 and Glossary... 34, 35 Abbreviations 36 Disclaimer... 37
4 Solar Geophysical Activity Summary 3 Introduction This monthly Solar Geophysical Activity Report summarizes solar- and geomagnetic activities observed during the previous period. It s purpose is to provide an overview of solar events e.g. the changing number of sunspots (on the Earth directed visible disk of the Sun), the planetary A- and K-indices, and to give information of the Sun s activity, the development of solar wind, the velocity, energetic particle enhancements etc., and their influence to the geomagnetic field, especially to propagation mechanism for long- and short range hf radio circuits. Significant sunspots or sunspot groups as well as solar active regions are always identified by the solar region number, to make it more easy to observe their development and movement. If not otherwise stated, please be advised, that all data provided are daily maximum (not smoothed) values. Important sunspots or sunspot groups with particularly high geoeffectivity are always shown as solar images of the corresponding day. All images of the Sun shown in this summary have been issued by Stanford University, Stanford, California, USA, and based on SOHO Michelson Doppler Imager (MDI) 6767 A observations. All information concerning shortwave propagation conditions are based on observations of a global shortwave beacon network project (NCDXF) and selected broadcasting stations. Please don t hesitate to forward any kind of critisism as well as proposals. Those information will be most welcome to rise the level of quality of this report. Steffen Hilbig Direktion Distribution Ausstrahlungskoordination Kurt Schumacher Str. 3 D Bonn TF +49 (0) FAX +49 (0) Steffen.Hilbig@dw-world.de
5 Solar Geophysical Activity Summary 4 Solar Geophysical Activity Summary for February 2007 Space weather conditions are currently extremely quiet. Basically the x-ray corona of the sun has vanished, as well as any geomagnetic activity. Review of solar and geomagnetic events First period of observation, (01 07 February 2007). Solar activity was at very low to low levels during the first period of observation. Region NOAA 0940 produced isolated B- and C-class flares during 01 February No flares were observed during February. The geomagnetic field ranged from quiet to minor storm levels at middle latitudes, while high latitudes experienced quiet to severe storm levels. A recurrent coronal hole high-speed stream disturbed the field during 29 January until 01 February Activity ranged from quiet to minor storm levels during the disturbance with major storm periods detected at higher latitudes. During the disturbance solar wind speeds reached maximum velocities of about 720 km/s early on 31 January, while the Bz component of the Interplanetary Magnetic Field IMF fluctuated between +/- 18 nt on 29 January Activity decreased to quiet levels during the latter half of 01 February and remained so for the balance of the period. By 30 January the IMF Bz component relaxed and did not vary much beyond +/- 5 nt for the remainder of the period. Solar wind speed gradually decreased after 31 January and ended the period near 325 km/s. Second period of observation, (08 14 February 2007). Solar activity again was at very low to low levels. Region 0940 produced an isolated C-class flare at 08 February 2007 as the region rotated around the western limb. The geomagnetic field was generally at quiet to unsettled levels at all latitudes. High latitudes experienced isolated active to minor storm conditions on 04, 07 and 08 February 2007 due to a southward directed Bz component of the IMF. Solar wind speed ranged from a low of 330 km/s on 05 February to a high around 475 km/s on 09 February. The Bz component of the IMF fluctuated between +/- 8 nt for about 24 hours beginning early on 06 February. Thereafter and through the balance of the period Bz did not vary much beyond +/-5 nt. Activity decreased to quiet levels during the latter half of 10 February. On 13 February a solar wind stream hit Earth, leading to a geomagnetic storm (Kp=5) and aurorae borealis visible as southward as southern Skandinavia.
6 Solar Geophysical Activity Summary 5 Solar Geophysical Activity Summary for February 2007 Third period of observation, (15 21 February 2007). Solar activity was at very low to low levels. Isolated, optically uncorrelated B- and C-class flares occurred during the period. The geomagnetic field was disturbed during February due to a recurrent coronal hole high-speed stream. Activity ranged from quiet to minor storm levels during the disturbance with a brief period of major storm at high latitudes on 14 February. Solar wind data indicated the recurrent high-speed stream commenced on 12 February by a brief density increase. Velocity reached a peak of 778 km/s at 14/0830 UTC. Maximum IMF Bz variations occurred during February with a peak southward Bz on minus 11 nt at 13/1400 UTC. Field activity decreased to quiet to unsettled levels during February as coronal hole effects subsided. Fourth period of observation (22 28 February 2007). Solar activity was low and decreased to very low levels for the rest of the period with no flares. The geomagnetic field was quiet at all latitudes during the summary period. Ap-Index The maximum Ap-Index number was of 39 (minor storm conditions) on 28 February Sunspots The maximum Sunspot number was of 36 on 02 February and of 27 spots on 20 February Otherwise just a small number of spots have been seen during the entire period. Solar winds Maximum Solar winds have been measured with values of approximately 645 km/s on 01 February 2007, of around 840 km/s to 780 km/s from 15 to 16 February and of around 700 km/s on 28 February Solar Flux Maximum Solar Flux has been observed on 01 and 02 February 2007 with values of around 90. Significant activities The most significant solar event was a
7 Solar Geophysical Activity Summary 6 Solar Geophysical Activity Summary for February 2007 Solar Image Solar disk of 05 February 2007 showing groups NOAA 0940 and 0941
8 Solar Geophysical Activity Summary 7 Solar Geophysical Activity Summary for February 2007 Solar Image Solar Disk of 15 February 2007 appears almost spotless Mess- u.kontrollzentrale
9 Solar Geophysical Activity Summary 8 Solar Geophysical Activity Summary for February 2007 Solar Image Solar Disk of 20 February 2007 showing Regions NOAA 0942 and NOAA 0943 Mess- u.kontrollzentrale
10 9 SOLAR - GEOPHYSICAL ACTIVITY SUMMARY FOR FEBRUARY 2007 NOAA / SEC SOLAR INDICES SFl SSN A-Index Date d
11 10 SOLAR WIND DEVELOPMENT FOR FEBRUARY max min 800 VELOCITY (km/sec) Date d
12 11 SOLAR WIND DAILY VALUES FOR FEBRUARY max min VELOCITY (km/sec) Date d
13 12 SOLAR WIND DENSITY DURING FEBRUARY Protons/ccm 12 Protons / ccm Date d
14 13 SOLWIND DENSITY DEVELOPMENT FOR FEBRUARY Protons / ccm Date d
15 14 DAILY Ap-INDICES DURING FEBRUARY Ap-Indices Ap-Indices Date d
16 15 Ap-INDICES DEVELOPMENT FOR FEBRUARY max min Ap-Indices Date d
17 16 DAILY Kp-INDICES FOR FEBRUARY Kp-Indices Date d
18 17 9 DEVELOPMENT OF K-INDICES DURING FEBRUARY K-Indices 7 6 Kp-Indices Date d
19 18 12 GEOMAGNETIC ACTIVITY OVERVIEW FOR FEBRUARY 2007 Geomagnetic Events quiet - unsett active minor - moderate s. major - severe storm Date d
20 19 IMF - ORIENTATION AND STRENGTH. DAILY B and Bz COMPONENTS FOR FEBRUARY B total Bz south Bz north nt Date d
21 20 30 IMF - ORIENTATION AND STRENGTH. DEVELOPMENT DURING FEBRUARY B total Bz south Bz north Date d
22 Solar Geophysical Activity Summary 21 Solar Geophysical Activity Summary for February 2007 Northern Auroral Region Northern Auroral Oval of 05. February 2007
23 Solar Geophysical Activity Summary 22 Solar Geophysical Activity Summary for February 2006 Northern Auroral Region Northern Auroral Oval of 27 February 2007
24 Solar Geophysical Activity Summary 23 Solar Geophysical Activity Summary for February 2007 Northern Auroral Region Northern Auroral Oval of 28 February 2007
25 Solar Geophysical Activity Summary 24 Image of the Northern Polar Auroral Oval During intensive geomagnetic disturbance, the geomagnetic field structure is deeply affected by high-energy particles released by the Sun. The plots of Northern Polar Auroral Oval estimate the visibility of activity from any location of the northern hemisphere. Images show the potential auroral luminosity from the current solar wind stream conditions and are destined to provide an estimate of the visibility of auroral activity. Colour Levels of activity green NIL - low brown / orange low - moderate red moderate - high The brighter the colour, the more intense the activity. Images and maps of the Polar Auroral Oval provided are based on NOAA data and have been issued by STD Solar Terrestrial Dispatch.
26 Solar Geophysical Activity Summary 25 Space Weather Scales Ap - Index Category Descriptor 0-7 Quiet 8-15 Unsettled Active Minor Storm Major Storm Severe Storm Ap-Indices The geomagnetic Ap Index describes the activity of the geomagnetic field in a given time.
27 Solar Geophysical Activity Summary 26 Space Weather Scales Planetary K Indices (Kp); describe geomagnetic storm levels Category Effects 0-1 Kp-Index values of 0 and 1 represent Inactive to Very quiet magnetic conditions and imply very good to good hf radio signal propagation conditions. 2-4 Represent Quiet to Unsettled and Active magnetic conditions and generally correspond to less-impressive hf radio propagation conditions. 5 Represent Minor Storm conditions and are usually associated with fair to poor propagation for many hf paths. 6 Generally represents Major Storm conditions and are almost always associated with poor hf radio propagation conditions. 7 Represents Severe Storm conditions and are often accompanied by hf radio blackout conditions lasting from minutes to < 6 hours, particularly over high latitudes. 8-9 Represents Very Severe Storm to Extreme Severe Storm conditions and are rarely encountered (except during exceptional periods of solar activity). Kp Indices of values around 8 9 most often produce hf radio blackouts for periods lasting in excess of 6 to >10 hours, depending upon intensity of the solar event. Kp-Indices Planetary K - Index NOAA Geomagnetic storm levels * Indices Descriptor Values 0 Inactive G0 1 Very quiet G0 2 Quiet G0 3 Unsettled G0 4 Active G0 5 Minor storm G1 6 Major storm G2 7 Severe storm G3 8 Very severe storm G4 9 Extremely severe storm G5 * broadcast as voice announcements by WWV and WWVH
28 Solar Geophysical Activity Summary 27 Space Weather Scales Correlation of Kp Indices to Ap Indices Correlation Kp - Indices Ap - Indices Kp-Indices / Ap-Indices
29 Solar Geophysical Activity Summary 28 Space Weather Scales Solar Flares Solar flares are classified according their x-ray brightness in the wavelength range 1 to 8 Ångstrøms. Flare Category Peak (W/m²) between 1 and 8 Ångstrøms Descriptor X - class 1.0 x 10E-4 X-class flares are big. They are major events that can trigger planet-wide radio blackouts and long-lasting radiation storms. M class 1.0 x 10E-5 M-class flares are medium-sized events. They generally cause brief radio blackouts that effect Earth s high latitude regions. C class 1.0 x 10E-6 C-class flares are small events with only few noticeable consequences on Earth. B class 1.0 x 10E-7 B-class flares are very small events with no noticeable consequences on Earth. A class 1.0 x 10E-8 A-class flares are extreme small events with no noticeable consequences on Earth. Classification of solar flares Solar Flares A solar flare is an explosion on the Sun that happens when high energy stored in twisted magnetic fields (usually above sunspots or sunspot areas) is suddenly released. Flares produce a burst of radiation across the entire electromagnetic spectrum from radio waves to x-rays and gamma-rays and has major, minor, small or no consequences to hf propagation. Flares are classified according to the table. Mess- u. Empfangsstation
30 29 10 DAILY NUMBER AND CATEGORY OF SOLAR FLARES FOR FEBRUARY X-flares M-flares C-flares Date d
31 30 SOLAR FLARES - DEVELOPMENT DURING FEBRUARY X-flares M-flares C-flares Cathegory Date d
32 Solar Geophysical Activity Summary 31 Date Solar Activity (Flares) Geomagnetic Field Recent propagation conditions for February 2007 according to observations of a global HF beacon network and selected broadcasting stations obtained by means of s receiving station Bockhacken Remarks 045 NE 090 E 135 SE Great Circle Paths* 01. eruptive minor storm n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 02. quiet minor storm fair good fair good fair - good fair -good fair - poor poor 03. quiet active warning fair fair - good fair fair - good fair fair - poor poor poor 04. quiet quiet fair -good fair - good fair good fair -good fair fair fair - poor 05. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 06. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 07. quiet quiet fair fair fair fair - good fair - good poor poor - unus unusable 08. quiet quiet fair - poor fair - good poor fair - good fair fair fair - poor fair - poor 09. quiet quiet fair - good good fair - good good fair - good fair fair - poor unusable 10. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 11. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 12. quiet unsettled warning fair fair - good fair - good good fair fair fair - poor poor - unus 13. quiet unsettled warning fair good fair fair - good fair fair - poor poor poor 14. quiet unsettled warning fair good fair good fair fair fair - poor poor 15. quiet quiet fair fair - good fair - good good fair fair fair - poor poor - unus 180 S 225 SW 270 W 315 NW 360 N * directions as from location of remote controlled Receiving Station Bockhacken (lat. 51N06.40, long 07E16.45)
33 Solar Geophysical Activity Summary 32 Mess- u.kontrollzentrale Date Solar Activity (Flares) Geomagnetic Field (Status) Recent propagation conditions for February 2007 according to observations of a global HF beacon network and selected broadcasting stations taken by means of s receiving station Bockhacken Remarks 045 NE 090 E 135 SE Great Circle Paths* 16. quiet quiet fair fair - good fair good fair fair fair - poor poor 17. quiet quiet fair - good good fair good fair fair fair - poor fair - poor 18. quiet quiet fair fair - good fair good - fair fair Fair - poor poor poor 19. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 20. quiet quiet poor - fair fair - good fair good fair fair poor unusable 21. quiet quiet n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 22. quiet quiet fair fair - good fair good fair fair fair fair - poor 23. quiet quiet fair good fair - good good fair - good fair - good fair fair 24. quiet quiet fair fair - good fair - good good fair fair - good fair fair - poor 25. quiet active warning n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 26. quiet minor warning n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 27. quiet active warning n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 28. quiet active warning n.o. n.o. n.o. n.o. n.o. n.o. n.o. n.o. 180 S 225 SW 270 W 315 NW 360 N * Directions as from location of remote controlled receiving station Bockhacken (lat 51N06.40, long 07E16.46)
34 SOLAR CYCLE PROGRESSION CYCLES 22, 23 & 24 CYCLE 22 CYCLE 23 February 2007 d
35 Solar Geophysical Activity Summary 34 Glossary of Solar Terms Ap Index: The geomagnetic Ap-Index describes the activity of the geomagnetic field in a given time. It can vary up to values around 100. During very severe geomagnetic storms it can reach values up to 200 and very occasionally more. Aurora: A sporatic, faint visual phenomenon (Polar Lights, Aurorae Borealis, Aurorae Australis), associated with high geomagnetic activity that occurs mainly in the high latitude night skies of the northern and southern hemisphere. Auroral Oval: An elliptical band around each geomagnetic pole ranging from about 75 degrees magnetic latitude to about 65 degrees magnetic latitude under average magnetic conditions. It is the area of those locations of the maximum occurrence of auroras and widens to both higher and lower latitudes during the expansion phases of magnetic substorms. Geomagnetic Activity: Natural variations in the geomagnetic field, classified into: quiet, unsettled, active and geomagnetic storm levels. There are two indices that are used to determine the level of geomagnetic activity: the Ap-index and the Kp-index. Geomagnetic Latitudes: Low latitudes range from 0 20 degrees, middle latitudes range from degrees, high latitudes range from degrees geomagnetic latitude to the north and/or the south of the equator. Geomagnetic Storm: A worldwide disturbance of Earth s magnetic field (magnetosphere), inducted by direct connection to the Sun s interplanetary magnetic field (IMF), distinct with the arrival at Earth of a shock front of the solar wind, which compresses the front of the magnetosphere. A storm occurs when: Ap > (minor storm), Ap (major storm), Ap (severe storm). Interplanetary Magnetic Field (IMF): The interplanetary magnetic field (IMF) is a part of the Sun s magnetic field that is carried into the interplanetary space by the solar wind. The IMF s field varies in strength near Earth from 1 to 37 nt, with an average value on ~6nT. IMF Bz: The IMF is a vector quantity with three directional components, two of which (Bx and By) are orientated parallel to the ecliptic, the third component (Bz) is perpendicular to the ecliptic and is created by waves and other disturbances in the solar wind. When the IMF and geomagnetic field lines are orientated opposite or antiparallel to each other, they can in some cases merge or reconnect, resulting in transfer of energy, mass and momentum from the solar wind flow to the magnetosphere. The strongest coupling with the most dramatic magnetospheric effect occurs, when the Bz-component is orientated southward. Ionospheric Storm: A disturbance of the ionosphere (F-layer), which occurs in connection with geomagnetic activity, usually causing high absorption of hf radio signals. Kp Index: The Kp-Index describes geomagnetic activity and storm levels. This planetary 3 hour range index Kp is an index taken from 13 geomagnetic observatories between 044 degrees and 060 degrees northern or southern geomagnetic latitude and is designed to measure solar particles radiation by its magnetic effects. The scale is 0 9. nt: Nano Tesla, Unit of magnetism, (1nT = 10E-5 Gauss). Mess- u.kontrollzentrale
36 Solar Geophysical Activity Summary 35 Glossary of Solar Terms Solar Activity: Transient perturbations of the solar atmosphere as measured by enhanced x-ray emissions of the sun. Solar Flares: Solar Flares are tremendous explosions on the Sun s surface. They occur in vicinity of sunspots and usually along the dividing line between areas of opposite fields. Flares release many forms of energy (s. Solar wind). Solar Flux (SFl): The solar flux is used as the basic indicator of solar activity and to determine the level of radiation being received from the sun. The solar flux is measured in solar flux units (SFU) and is the amount of radio noise or flux that is emitted at a frequency of 2800 MHz (10.7 cm). The solar flux is closely related to the amount of ionization and hence the electron concentration in the F-region of the ionosphere. As a result it gives a good indication of conditions especially for long distance radio communication on hf circuits. Solar Wind: A stream of charged particles and magnetic fields emanating from the sun. Under undisturbed conditions this winds velocity is measured with approximately 250 to 450 kilometers per second. In cases of severe or extreme disturbance its tremendous velocity is measured with > km/s. Sunspots: Areas seen as dark spots, in contrast with it surroundings on the Suns surface. Sunspots are areas with extreme concentrations of energy (magnetic flux). Sunspot Number (SSN): The sunspot number summarizes the number of sunspots to be seen on the (Earth directed) visible disc of the Suns surface and gives an index of sunspot activity (R). Sudden Ionospheric Disturbance (SID): One of the different hf radio propagation anomalies due to ionospheric changes resulting from solar activities. Anomalies include short wave fades (or fadeouts), enhancements of atmospherics, phase shifts of electromagnetic radio waves, absorptions, cosmic noise etc. Solar Cycle or Sunspot Cycle: The approximately 11-year quasi periodic variation in the sunspot number. (see diagram of solar cycles 22 and 23). Space Weather: Describes the conditions in space that effect Earth and its technological systems. It is a consequence of the behavior of the Sun, the nature of Earth s magnetic field and atmosphere, and our location in the solar system. Mess- u.kontrollzentrale
37 Solar Geophysical Activity Summary 36 Abbreviations and Terms: ACE = Advanced Composition Explorer Satellite AGU = American Geophysical Union Ap = Planetary A-Index AIP = American Institutes of Physics Bx, By, Bz = B-Components of the IMF CME = Coronal Mass Ejection DK0WCY = Auroa-Beacon DK0WCY, Scheggerott HSS = High Solar Stream IMF = Interplanetary Magnetic Field IARU = International Amateur Radio Union IPS = Radio & Space Services, The Australian Space Weather Agency Kp = Planetary K-Index lat = Latitude long = Longitude minor = minor geomagnetic storm major = major geomagnetic storm NCDXF = Northern California DX-Foundation Inc. NGDC = National Geophysical Data Center n.o. = not observed NOAA = National Oceanic and Atmospheric Administration nt = NanoTesla PCA = Polar Cap Absorption R = Index of Sunspot activity SEC = Space Weather Environment Center SFl = Solar Flux SFU = Solar Flux Units SI = Sudden Impulse SID = Sudden Ionospheric Disturbance SIDC = Solar Influence Data Analysis Center SSN = Sunspot Number STD = Solar Terrestrial Dispatch unsett = unsettled unus = unusable WWV = National Bureau of Standards, Fort Collins, Colorado WWVH = National Bureau of Standards, Maui, Hawaii
38 Solar Geophysical Activity Summary 37 Disclaimer This Solar Geophysical Activity and Propagation Summary has been prepared and compiled by Steffen Hilbig,, Bonn, Germany. Results are based on own observations and numerous valuable data provided by different services and institutions as mentioned below. I herewith reserve the rights not to be responsible for completeness and quality of the information. Liability claims regarding damage caused by the use of any information given in this summary will therefore be rejected. shall be under no liability whatsoever resulting from any use of the given information. AGU, American Geophysical Union, Washington, DC, USA AIP, American Institutes of Physics Aurora-Beacon DK0WCY, Scheggerott, Germany IonoProbe, Realtime Space Weather Monitor IPS Radio & Space Services, Haymarket, NSW, Australia Joint USAF/NOAA, Propagation Bulletin Max Planck Institut für Aeronomie, Göttingen - Lindau, Germany NCDXF/IARU Northern California International Beacon Transmission Network NGDC, National Geophysical Data Center, Boulder, Colorado, USA NOAA, National Oceanic and Atmospheric Administration, Boulder, Colorado, USA Real Time Propagation Monitor, SM5AJV, Stockholm, Sweden SEC, US Space Weather Environment Services Center, Boulder, Colorado, USA SIDC, Solar Influence Data Analysis Center, RWC, Belgium STD, Solar Terrestrial Dispatch WWV, National Bureau of Standards, Fort Collins, Colorado, USA WWVH, National Bureau of Standards, Maui, Hawaii, USA and others
DEUTSCHE WELLE SOLAR GEOPHYSICAL ACTIVITY REPORT. October 2006
DEUTSCHE WELLE SOLAR GEOPHYSICAL ACTIVITY REPORT October 2006 Steffen Hilbig Mess- un Kontrollzentrale DEUTSCHE WELLE SOLAR GEOPHYSICAL ACTIVITY REPORT October 2006 Aurora Borealis Steffen Hilbig Solar
More informationTracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus
Tracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus In June 2015, the Sun emitted several M-Class flares over a 2-day period. These flares were concurrent with
More informationChapter 8 Geospace 1
Chapter 8 Geospace 1 Previously Sources of the Earth's magnetic field. 2 Content Basic concepts The Sun and solar wind Near-Earth space About other planets 3 Basic concepts 4 Plasma The molecules of an
More informationGeomagnetic Disturbance Report Reeve Observatory
Event type: Various geomagnetic disturbances including coronal hole high-speed stream, coronal mass ejection, sudden impulse and reverse shock effects Background: This background section defines the various
More informationUnderstanding Solar Indices
Understanding Solar Indices By Ken Larson KJ6RZ Long distance HF radio communications is made possible by a region of charged particles in the Earth s upper atmosphere, 30 to 200 miles above the Earth
More informationGeomagnetic storms. Measurement and forecasting
Geomagnetic storms. Measurement and forecasting Anna Gustavsson 17 October 2006 Project of the Space Physics Course 2006 Umeå University 1 Introduction Effects of magnetic storms on technology Geomagnetic
More informationEFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER
Indian J.Sci.Res.3(2) : 121-125, 2012 EFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER a1 b c SHAM SINGH, DIVYA SHRIVASTAVA AND A.P. MISHRA Department of Physics, A.P.S.University, Rewa,M.P.,
More informationSTCE Newsletter. 6 Jan Jan 2014
Published by the STCE - this issue : 16 Jan 2014. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationINTERPLANETARY ASPECTS OF SPACE WEATHER
INTERPLANETARY ASPECTS OF SPACE WEATHER Richard G. Marsden Research & Scientific Support Dept. of ESA, ESTEC, P.O. Box 299, 2200 AG Noordwijk, NL, Email: Richard.Marsden@esa.int ABSTRACT/RESUME Interplanetary
More informationSpace Weather and Satellite System Interaction
Space Engineering International Course, Kyutech, 4 th Quarter Semester 2017 Space Weather and Satellite System Interaction Lecture 2: Space Weather Concept, Reporting and Forecasting Assoc. Prof. Ir. Dr.
More informationGeomagnetic Disturbance Report Reeve Observatory
Event type: Geomagnetic disturbances due to recurrent coronal hole high-speed stream Background: This background section defines the events covered. A coronal hole is a large dark region of less dense
More informationGeomagnetic Disturbances (GMDs) History and Prediction
Geomagnetic Disturbances (GMDs) History and Prediction J. Patrick Donohoe, Ph.D., P.E. Dept. of Electrical and Computer Engineering Mississippi State University Box 9571 Miss. State, MS 39762 donohoe@ece.msstate.edu
More informationINVESTIGATIONS OF THE STRUCTURE OF THE DIURNAL VARIATIONS OF GEOMAGNETIC FIELD
Geologica Macedonica, Vol. 26, No. 1, pp. 37 51 (2012) GEOME 2 ISSN 0352 1206 Manuscript received: May 6, 2012 UDC: 556.385 Accepted: October 10, 2012 Original scientific paper INVESTIGATIONS OF THE STRUCTURE
More informationSTCE Newsletter. 7 Dec Dec 2015
Published by the STCE - this issue : 18 Dec 2015. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationSTCE Newsletter. 18 Jan Jan 2016
Published by the STCE - this issue : 29 Jan 2016. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationSolar and Interplanetary Disturbances causing Moderate Geomagnetic Storms
J. Astrophys. Astr. (2008) 29, 263 267 Solar and Interplanetary Disturbances causing Moderate Geomagnetic Storms Santosh Kumar, M. P. Yadav & Amita Raizada Department of P.G. Studies and Research in Physics
More informationIntroduction to Space Weather and Propagation
Introduction to Space Weather and Propagation Carl Luetzelschwab K9LA ARRL Vice Director, Central Division k9la@arrl.net https://k9la.us K9LA 1 What Is Space Weather? Space weather is the quiet Sun Electromagnetic
More informationSolar Activity The Solar Wind
Solar Activity The Solar Wind The solar wind is a flow of particles away from the Sun. They pass Earth at speeds from 400 to 500 km/s. This wind sometimes gusts up to 1000 km/s. Leaves Sun at highest speeds
More informationSpace Weather. S. Abe and A. Ikeda [1] ICSWSE [2] KNCT
Space Weather S. Abe and A. Ikeda [1] ICSWSE [2] KNCT Outline Overview of Space Weather I. Space disasters II. Space weather III. Sun IV. Solar wind (interplanetary space) V. Magnetosphere VI. Recent Space
More informationThe Sun sends the Earth:
The Sun sends the Earth: Solar Radiation - peak wavelength.visible light - Travels at the speed of light..takes 8 minutes to reach Earth Solar Wind, Solar flares, and Coronal Mass Ejections of Plasma (ionized
More informationCHAPTER 2 DATA. 2.1 Data Used
CHAPTER DATA For the analysis, it is required to use geomagnetic indices, which are representatives of geomagnetic activity, and Interplanetary Magnetic Field (IMF) data in addition to f F,which is used
More informationModule 4: Astronomy - The Solar System Topic 2 Content: Solar Activity Presentation Notes
The Sun, the largest body in the Solar System, is a giant ball of gas held together by gravity. The Sun is constantly undergoing the nuclear process of fusion and creating a tremendous amount of light
More informationThis page intentionally left blank!
This page intentionally left blank! Solar-Terrestrial Data Available on the k4msu.com Website The original title was going to be... Is KK4BKD a Spy Using k4msu.com to Send Secret Messages? Or, what else
More informationSolar Dynamics Affecting Skywave Communications
Solar Dynamics Affecting Skywave Communications Ken Larson KJ6RZ October 2010 1 Page Subject 3 1.0 Introduction 3 2.0 Structure of the Sun 3 2.1 Core 3 2.2 Radiation Zone 4 2.3 Convection Zone 4 2.4 Photosphere
More informationThe Solar wind - magnetosphere - ionosphere interaction
The Solar wind - magnetosphere - ionosphere interaction Research seminar on Sun-Earth connections Eija Tanskanen Friday January 27, 2006 12-14 a.m., D115 Outline 1. Basics of the Earth s magnetosphere
More information8.2 The Sun pg Stars emit electromagnetic radiation, which travels at the speed of light.
8.2 The Sun pg. 309 Key Concepts: 1. Careful observation of the night sky can offer clues about the motion of celestial objects. 2. Celestial objects in the Solar System have unique properties. 3. Some
More informationSolar-terrestrial relation and space weather. Mateja Dumbović Hvar Observatory, University of Zagreb Croatia
Solar-terrestrial relation and space weather Mateja Dumbović Hvar Observatory, University of Zagreb Croatia Planets Comets Solar wind Interplanetary magnetic field Cosmic rays Satellites Astronauts HELIOSPHERE
More informationEffect of Solar Flare X-Rays on digisonde fmin values. S. C. Tripathi H. Haralambous
Effect of Solar Flare X-Rays on digisonde fmin values S. C. Tripathi H. Haralambous SOLAR FLARE Solar flares occur when the sun's magnetic field twists up and reconnects, blasting energy outward and superheating
More informationDirected Reading. Section: Solar Activity SUNSPOTS. Skills Worksheet. 1. How do the gases that make up the sun s interior and atmosphere behave?
Skills Worksheet Directed Reading Section: Solar Activity 1. How do the gases that make up the sun s interior and atmosphere behave? 2. What causes the continuous rising and sinking of the sun s gases?
More informationTHE SOLAR WIND & SOLAR VARIABILITY
The Sun-Earth System: CONTENTS AN OVERVIEW The Stars Around Us 1 Our Dependence on the Sun 3 The Sun s Inconstancy 3 Intruders from Afar 5 What Gets By 5 Voyages of Discovery in an Age of Exploration 6
More informationComparative study of solar and geomagnetic indices for the solar cycle 22 and 23 C. M Tiwari Dept. of Physics, APS University, Rewa (M. P.
International Association of Scientific Innovation and Research (IASIR) (An Association Unifying the Sciences, Engineering, and Applied Research) International Journal of Emerging Technologies in Computational
More informationHELIOSTAT III - THE SOLAR CHROMOSPHERE
HELIOSTAT III - THE SOLAR CHROMOSPHERE SYNOPSIS: In this lab you will observe, identify, and sketch features that appear in the solar chromosphere. With luck, you may have the opportunity to watch a solar
More informationSTCE Newsletter. 7 May May 2018
Published by the STCE - this issue : 18 May 2018. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationSTCE Newsletter. 11 Jan Jan 2016
Published by the STCE - this issue : 21 Jan 2016. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationIntroduction to Space Weather
Introduction to Space Weather We may have been taught that there is a friendly, peaceful nonhostile relationship between the Sun and the Earth and that the Sun provides a constant stream of energy and
More informationUsing This Flip Chart
Using This Flip Chart Solar storms can cause fluctuations in the magnetosphere called magnetic storms. These magnetic storms have disabled satellites and burned out transformers shutting down power grids.
More informationSolar Flare Durations
Solar Flare Durations Whitham D. Reeve 1. Introduction Scientific investigation of solar flares is an ongoing pursuit by researchers around the world. Flares are described by their intensity, duration
More information1 2 3 US Air Force 557 th Weather Wing maintains a website with many operational products both on terrestrial as on space weather. The operational holy grail for the military are stoplight charts, indicating
More informationAn Introduction to Space Weather. J. Burkepile High Altitude Observatory / NCAR
An Introduction to Space Weather J. Burkepile High Altitude Observatory / NCAR What is Space Weather? Space Weather refers to conditions in interplanetary space, produced by the Sun, that can disrupt
More informationSpace Weather Awareness in the Arctic. Torsten Neubert Head of Section for Solar System Physics
Space Weather Awareness in the Arctic Torsten Neubert Head of Section for Solar System Physics Technology in the Arctic There is significant potential Resources Tourism helped by receding ocean ice There
More informationChapter 24: Studying the Sun. 24.3: The Sun Textbook pages
Chapter 24: Studying the Sun 24.3: The Sun Textbook pages 684-690 The sun is one of the 100 billion stars of the Milky Way galaxy. The sun has no characteristics to make it unique to the universe. It is
More informationGeomagnetic Sudden Impulses
Geomagnetic Sudden Impulses Whitham D. Reeve 2013 W. Reeve 1. Introduction This article discusses geomagnetic sudden impulses observed with the SAM-III magnetometer system at Anchorage, Alaska USA during
More information1-4-1A. Sun Structure
Sun Structure A cross section of the Sun reveals its various layers. The Core is the hottest part of the internal sun and is the location of nuclear fusion. The heat and energy produced in the core is
More informationResponse of the Earth s magnetosphere and ionosphere to the small-scale magnetic flux rope in solar wind by the MHD simulation
Response of the Earth s magnetosphere and ionosphere to the small-scale magnetic flux rope in solar wind by the MHD simulation Kyung Sun Park 1, Dae-Young Lee 1, Myeong Joon Kim 1, Rok Soon Kim 2, Kyungsuk
More informationSpace Weather Effects of Coronal Mass Ejection
J. Astrophys. Astr. (2006) 27, 219 226 Space Weather Effects of Coronal Mass Ejection K. N. Iyer 1,, R. M. Jadav 1, A. K. Jadeja 1, P. K. Manoharan 2, Som Sharma 3 and Hari Om Vats 3 1 Department of Physics,
More informationThe Solar Wind Space physics 7,5hp
The Solar Wind Space physics 7,5hp Teknisk fysik '07 1 Contents History... 3 Introduction... 3 Two types of solar winds... 4 Effects of the solar wind... 5 Magnetospheres... 5 Atmospheres... 6 Solar storms...
More informationThe Sun Our Star. Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun
The Sun Our Star Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun General Properties Not a large star, but larger than most Spectral type G2 It
More informationThe Dancing Lights Program
The Sun Teacher Background: The Dancing Lights Program Margaux Krahe Many people think the Sun is just a fiery yellow ball. The Sun is not actually burning because fire requires oxygen. Really, the Sun
More informationChapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He
Our sole source of light and heat in the solar system A common star: a glowing ball of plasma held together by its own gravity and powered by nuclear fusion at its center. Nuclear fusion: Combining of
More informationCenter Data Analysis Service supported by the FAGS
Solar Influences Data analysis Center Data Analysis Service supported by the FAGS SUNSPOT BULLETIN 2 n Provisional international and normalized hemispheric daily sunspot numbers for September 2 computed
More informationSolar Transients P.K. Manoharan
Solar Transients P.K. Manoharan Radio Astronomy Centre National Centre for Radio Astrophysics Tata Institute of Fundamental Research Ooty 643001, India 1 Solar Flares and associated Coronal Mass Ejections
More informationSTCE Newsletter. 29 Jan Feb 2018
STCE Newsletter 29 Jan 2018-4 Feb 2018 Published by the STCE - this issue : 8 Feb 2018. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative
More informationChapter 8 The Sun Our Star
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 8 The Sun
More informationYour web browser (Safari 7) is out of date. For more security, comfort and the best experience on this site: Update your browser Ignore
Your web browser (Safari 7) is out of date. For more security, comfort and the best experience on this site: Update your browser Ignore AURO RA northern lights (aurora borealis), southern lights (aurora
More informationThe Interior Structure of the Sun
The Interior Structure of the Sun Data for one of many model calculations of the Sun center Temperature 1.57 10 7 K Pressure 2.34 10 16 N m -2 Density 1.53 10 5 kg m -3 Hydrogen 0.3397 Helium 0.6405 The
More informationEffect of CME Events of Geomagnetic Field at Indian Station Alibag and Pondicherry
Effect of CME Events of Geomagnetic Field at Indian Station Alibag and Pondicherry Babita Chandel Sri Sai University Palampur, Himachal Pradesh, India Abstract: Space weather activity CMEs, and solar energetic
More informationSTCE Newsletter. 28 Dec Jan 2016
Published by the STCE - this issue : 8 Jan 2016. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationTransmission and Dispatching Operations Manual
MANUAL 12 Transmission and Dispatching Operations Manual October 2012 4.2.10 Adverse Operating Conditions NYISO Actions The NYISO may perform the following actions under adverse operating conditions: 1.
More informationThe Sun. Never look directly at the Sun, especially NOT through an unfiltered telescope!!
The Sun Introduction We will meet in class for a brief discussion and review of background material. We will then go outside for approximately 1 hour of telescope observing. The telescopes will already
More informationThe Structure of the Magnetosphere
The Structure of the Magnetosphere The earth s magnetic field would resemble a simple magnetic dipole, much like a big bar magnet, except that the solar wind distorts its shape. As illustrated below, the
More informationSOLAR WIND PROTON DENSITY INCREASE AND GEOMAGNETIC BACKGROUND ANOMALIES BEFORE STRONG M6+ EARTHQUAKES. V. Straser*, G. Cataldi
SOLAR WIND PROTON DENSITY INCREASE AND GEOMAGNETIC BACKGROUND ANOMALIES BEFORE STRONG M6+ EARTHQUAKES V. Straser*, G. Cataldi *International Earthquake and Volcano Prediction Center E-mail: valentino.straser@alice.it
More informationGuidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.
Guidepost The Sun is the source of light an warmth in our solar system, so it is a natural object to human curiosity. It is also the star most easily visible from Earth, and therefore the most studied.
More informationTeacher Background: The Dancing Lights Program
Teacher Background: The Dancing Lights Program The Sun Many people think the Sun is just a fiery yellow ball. The Sun isn t actually burning because fire requires oxygen. Really, the Sun a giant ball of
More informationThe Magnetic Sun. CESAR s Booklet
The Magnetic Sun CESAR s Booklet 1 Introduction to planetary magnetospheres and the interplanetary medium Most of the planets in our Solar system are enclosed by huge magnetic structures, named magnetospheres
More informationVerification of Short-Term Predictions of Solar Soft X-ray Bursts for the Maximum Phase ( ) of Solar Cycle 23
Chin. J. Astron. Astrophys. Vol. 3 (2003), No. 6, 563 568 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics Verification of Short-Term Predictions of Solar
More informationThe Structure of the Sun. CESAR s Booklet
How stars work In order to have a stable star, the energy it emits must be the same as it can produce. There must be an equilibrium. The main source of energy of a star it is nuclear fusion, especially
More informationSignatures of Geomagnetic Storms and Coronal Mass Ejections on Electron and Ion Temperatures At Low Latitude Upper Ionosphere
International Journal of Physics and Applications. ISSN 0974-3103 Volume 7, Number 1 (2015), pp. 43-48 International Research Publication House http://www.irphouse.com Signatures of Geomagnetic Storms
More informationA LOOK AT PROPAGATION FOR THE 2017/2018 CONTEST SEASON
A LOOK AT PROPAGATION FOR THE 2017/2018 CONTEST SEASON Frank Donovan W3LPL Carl Luetzelschwab K9LA 1 THANKS TO THE WWROF FOR SPONSORING THIS WEBINAR wwrof.org And thanks to Ken K4ZW for facilitating this
More informationThis project has received funding from the European Union s Horizon 2020 research and innovation programme under the Marie-Sklodowska-Curie grant
This project has received funding from the European Union s Horizon 2020 research and innovation programme under the Marie-Sklodowska-Curie grant agreement number 721624. Space weather and the variable
More informationMonthly Geomagnetic Bulletin
HARTLAND OBSERVATORY Monthly Geomagnetic Bulletin BRISTOL CHANNEL December 2002 02/12/HA Hartland NERC 2002 1. HARTLAND OBSERVATORY MAGNETIC DATA 1.1 Introduction This bulletin is published to meet the
More informationSpace weather. Introduction to lectures by Dr John S. Reid. Image courtesy:
Space weather Introduction to lectures by Dr John S. Reid Image courtesy: http://www.astro-photography.com/ss9393.htm Sunspot 9393 First pass from late March to early April, 2001 See: Storms from the Sun
More informationSTCE Newsletter. 4 Jan Jan 2016
Published by the STCE - this issue : 15 Jan 2016. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationSpace Physics. An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres. May-Britt Kallenrode. Springer
May-Britt Kallenrode Space Physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres With 170 Figures, 9 Tables, Numerous Exercises and Problems Springer Contents 1. Introduction
More informationA Correlative Study of Climate Changes and Solar Activity
10 A Correlative Study of Climate Changes and Solar Activity S. R. Lahauriya and A. P. Mishra Department of Physics, Govt. P. G. Autonomous College, Datia (M.P.) Abstract:- The Sun is ultimate source of
More informationThe importance of solar wind magnetic. the upcoming Sunjammer solar sail. field observations & mission
The importance of solar wind magnetic field observations & the upcoming Sunjammer solar sail mission J. P. Eastwood The Blackett Laboratory, Imperial College London, London SW7 2AZ, UK 13 November 2013
More information1 Introduction. Cambridge University Press Physics of Space Plasma Activity Karl Schindler Excerpt More information
1 Introduction Space plasma phenomena have attracted particular interest since the beginning of the exploration of space about half a century ago. Already a first set of pioneering observations (e.g.,
More informationActivities of the Japanese Space Weather Forecast Center at Communications Research Laboratory
J. RADIAT. RES., 43: SUPPL., S53 S57 (2002) Activities of the Japanese Space Weather Forecast Center at Communications Research Laboratory SHINICHI WATARI 1 * and FUMIHIKO TOMITA 1 Space weather / ISES/SEP
More informationThe Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:
The Sun Basic Properties Radius: Mass: 5 R Sun = 6.96 km 9 R M Sun 5 30 = 1.99 kg 3.33 M ρ Sun = 1.41g cm 3 Luminosity: L Sun = 3.86 26 W Effective Temperature: L Sun 2 4 = 4πRSunσTe Te 5770 K The Sun
More informationNICT SPACE WEATHER ACTIVITIES
Prepared by NICT Agenda Item: 3 Discussed in Ad-Hoc Meeting on Space Weather NICT SPACE WEATHER ACTIVITIES Tsutomu Nagatsuma Space Weather and Environment Informatics Laboratory, Applied Electromagnetic
More informationRadio Observations and Space Weather Research
Radio Observations and Space Weather Research Jasmina Magdalenić Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium What is space weather and why is it important? Eruptive processes:
More informationMAGNETIC POLES AND CLIMATE
MAGNETIC POLES AND CLIMATE Reno, NV June 25, 2009 1 The strength of the Earth s magnetic field varies tremendously around the world. The following figure shows the magnetic field intensity around the world,
More informationSpace Weather and Amateur Radio: Science, Forecasting and Effects. The Aerospace Corporation Dayton Hamvention Antenna Forum 19 May 2017
Space Weather and Amateur Radio: Science, Forecasting and Effects The Aerospace Corporation Dayton Hamvention Antenna Forum 19 May 2017 What is Space Weather? Essentially Space Weather is: A planet s interaction
More informationUnusually extreme cosmic ray events in July 2005
ESA Space Weather Week 2, November 2005 Unusually extreme cosmic ray events in July 2005 A. Papaioannou 1, M. Gerontidou 1, G. Mariatos 1, H. Mavromichalaki 1, C. Plainaki 1 1 University of Athens, Physics
More informationPlanetary Magnetospheres
1 Planetary Magnetospheres Vytenis M. Vasyliūnas Max-Planck-Institut für Sonnensystemforschung Heliophysics Summer School: Year 4 July 28 August 4, 2010 Boulder, Colorado July 23, 2010 Figure 1: Schematic
More informationThere are two more types of solar wind! The ballerina Sun right before activity minimum. The ballerina dancing through the solar cycle
There are two more types of solar wind! 3. Low speed wind of "maximum" type Similar characteristics as (2), except for Lectures at the International Max-Planck-Research School Oktober 2002 by Rainer Schwenn,
More informationMAGNETIC STORM EFFECTS IN THE ATMOSPHERIC ELECTRIC FIELD VARIATIONS
MAGNETIC STORM EFFECTS IN THE ATMOSPHERIC ELECTRIC FIELD VARIATIONS N.G. Kleimenova 1, O.V. Kozyreva 1, S. Michnowski 2, M. Kubicki 2, N.N. Nikiforova 1 1 Institute of the Earth Physics RAS, Moscow, Russia,
More informationThe Dynamic Magnetosphere. Ioannis A. Daglis. National Observatory of Athens, Greece
310/1749-42 ICTP-COST-USNSWP-CAWSES-INAF-INFN International Advanced School on Space Weather 2-19 May 2006 The Dynamic Magnetosphere: Reaction to and Consequences of Solar Wind Variations Yannis DAGLIS
More informationSPACE WEATHER: STORMS FROM THE SUN
GIFT 2013 - Natural Hazards Vienna, Austria, 10 April 2013 SPACE WEATHER: STORMS FROM THE SUN Norma B. Crosby Belgian Institute for Space Aeronomy Ringlaan-3-Avenue Circulaire, B-1180 Brussels, Belgium
More information1.3j describe how astronomers observe the Sun at different wavelengths
1.3j describe how astronomers observe the Sun at different wavelengths 1.3k demonstrate an understanding of the appearance of the Sun at different wavelengths of the electromagnetic spectrum, including
More informationExplain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere.
Chapter 29 and 30 Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere. Explain how sunspots are related to powerful magnetic fields on the sun.
More informationResponse of morning auroras and cosmic noise absorption to the negative solar wind pressure pulse: A case study
ÓPTICA PURA Y APLICADA. www.sedoptica.es Sección Especial: 37 th AMASON / Special Section: 37 th AMASON Aurora Response of morning auroras and cosmic noise absorption to the negative solar wind pressure
More informationSolar eruptive phenomena
Solar eruptive phenomena Andrei Zhukov Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium 26/01/2018 1 Eruptive solar activity Solar activity exerts continous influence on the solar
More informationSun s Properties. Overview: The Sun. Composition of the Sun. Sun s Properties. The outer layers. Photosphere: Surface. Nearest.
Overview: The Sun Properties of the Sun Sun s outer layers Photosphere Chromosphere Corona Solar Activity Sunspots & the sunspot cycle Flares, prominences, CMEs, aurora Sun s Interior The Sun as an energy
More informationTransmission and Dispatching Operations Manual
MANUAL 12 Transmission and Dispatching Operations Manual April 2016 4.2.9 Adverse Operating Conditions NYISO Actions The NYISO may perform the following actions under adverse operating conditions: 1. Notify
More informationSpace Physics: Recent Advances and Near-term Challenge. Chi Wang. National Space Science Center, CAS
Space Physics: Recent Advances and Near-term Challenge Chi Wang National Space Science Center, CAS Feb.25, 2014 Contents Significant advances from the past decade Key scientific challenges Future missions
More informationCTU Presents. The Fitful Rise of Solar Cycle 24 What it Means in the Coming Year. Frank Donovan W3LPL
CTU Presents The Fitful Rise of Solar Cycle 24 What it Means in the Coming Year Frank Donovan W3LPL Introduction This presentation focuses on: The four major fall and winter DX contests: CQ WW SSB and
More informationSpace Weather. ~ Affects of solar activities onto Earth. Cause-Effect Time Intervals range from immediate (precisely, 8 minutes) to several days.
Space Weather ~ Affects of solar activities onto Earth Cause-Effect Time Intervals range from immediate (precisely, 8 minutes) to several days. days Two difficulties arise for forecasting (modelling):
More informationThe Sun ASTR /17/2014
The Sun ASTR 101 11/17/2014 1 Radius: 700,000 km (110 R ) Mass: 2.0 10 30 kg (330,000 M ) Density: 1400 kg/m 3 Rotation: Differential, about 25 days at equator, 30 days at poles. Surface temperature: 5800
More informationCoronal Mass Ejections in the Heliosphere
Coronal Mass Ejections in the Heliosphere N. Gopalswamy (NASA GSFC) http://cdaw.gsfc.nasa.gov/publications Plan General Properties Rate & Solar Cycle Variability Relation to Polarity Reversal CMEs and
More information! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun. The Sun & Solar Activity
! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun The Sun & Solar Activity The Sun in Perspective Planck s Law for Black Body Radiation ν = c / λ
More information