Space Weather. S. Abe and A. Ikeda [1] ICSWSE [2] KNCT
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1 Space Weather S. Abe and A. Ikeda [1] ICSWSE [2] KNCT
2 Outline Overview of Space Weather I. Space disasters II. Space weather III. Sun IV. Solar wind (interplanetary space) V. Magnetosphere VI. Recent Space Weather
3 I. Space disasters Satellite breakdown(24/10/03) Japanese satellite Midori 2 disappeared on 24 Oct because of intense solar activity.
4 I. Space disasters Transformer fault (13 Mar. 1989, Quebec, Canada) Large-scale power failure occurred on 13 Mar at Canada because the intense aurora flowed inductive current in the electric power line and a transformer broke down. Broken transformer At that time, intense Aurora was observed by a satellite Dynamics Explorer-1
5 I. Space disasters Train accident (5 Feb. 1986, Canadian Rockies) Radio communication was disrupted, railway signaling failed, and so train accident occurred.
6 II. Space weather Recently, human activities intensify in the space environment. It becomes more important that we have a better understanding of the disturbances occur in space, and have a space weather forecasting system to prevent space disasters. Space environment for space weather is the space between the Sun and Earth and in the Earth s vicinity.
7 II. Stage of Space weather Solar wind Magnetosphere Sun Nasa The sun - Solar wind (interplanetary space) - magnetosphere
8 III. Sun An enormous amount of energy is constantly being radiated from the Sun and into space in the form of electromagnetic waves such as visible light, ultraviolet and infrared emissions. At the same time, solar atmosphere (corona) create outward flow of plasma (solar wind) which fills all regions of space surrounding the Sun. The sun occasionally radiates energy through burst-like phenomena called solar flares and coronal mass ejections (CME), and these events produce drastic changes in the space environment. large sunspot 28 Oct. 2003
9 III. Sun Active regions (sunspot groups) 16 Jul Sunspots are dark spots on the solar surface. The scale size of large sunspots are larger than that of the Earth. They consists of a cold central umbra with very strong local magnetic fields. Sunspot group Optical wave length image The relative sunspot number is one of a commonly used index. R=k(10g+f) R:Sunspot number k :coefficient to adjust for differences in the observer or telescope g : number of sunspot groups f : total number of individual sunspots
10 III. Sun Active regions (sunspot groups) 12 Aug Sunspots are dark spots on the solar surface. The scale size of large sunspots are larger than that of the Earth. They consists of a cold central umbra with very strong local magnetic fields. Optical wave length image The relative sunspot number is one of a commonly used index. R=k(10g+f) R:Sunspot number k :coefficient to adjust for differences in the observer or telescope g : number of sunspot groups f : total number of individual sunspots
11 X-ray image III. Sun Active regions (sunspot groups) 12 Aug The left panel shows the sun taken by X-ray. We can see bottom of the solar corona. In the image, the sunspot groups are blight. The bright region is a called active region which is the group of sunspots.
12 III. Sun Active regions (sunspot groups) 12 Aug Sunspots are dark spots on the solar surface that can be as large as 10^5 km. They consists of a cold central umbra with very strong local magnetic fields. Magnetic field image
13 III. Sun Flares 29 Oct A solar flare is a localized explosive release of energy that appears as a sudden, short lived brightening of an area in the chromosphere. Large flares eject large amounts of energetic particles. Flares are essentially highenergy particles.
14 III. Sun X ray flux X-ray intensity(10-12 Aug. 2011) Solar flares occur as explosive releases of energy in the outer atmosphere of the Sun, and radiate electromagnetic emissions that extend across the spectrum from γ- and X- rays, to the radio wave range. The enhancement of X-ray flux is observable around the Earth. The flares which are exceed C class are alarming phenomenon.
15 III. Sun X ray flux X-ray intensity(27-29 Oct. 2003) Solar flares occur as explosive releases of energy in the outer atmosphere of the Sun, and radiate electromagnetic emissions that extend across the spectrum from γ- and X- rays, to the radio wave range. The enhancement of X-ray flux is observable around the Earth. The flares which are exceed C class are alarming phenomenon.
16 III. Sun High-energy particles (Proton Flux) Proton Flux (10-12 Aug. 2011) High-energy particles are observable when large flares (or CMEs) occur. If density of the high-energy particles exceed the dashed line, It is Proton event. We need to alarm.
17 III. Sun High-energy particles (Proton Flux) Proton Flux (27-29 Oct. 2011) High-energy particles are observable when large flares (or CMEs) occur. If density of the high-energy particles exceed the dashed line, It is Proton event. We need to alarm.
18 Coronagraph III. Sun Coronal mass ejection (CME) Oct CMEs events originate in closed field regions in the corona, where magnetic field is strong enough to constrain the plasma from expanding outward. CMEs often occurs with flares, however CMEs are not generated by solar flares (The origin of CMEs not clear). CMEs mainly produce plasma.
19 III. Sun Coronal holes 12 Aug Extreme UV images shows us the the upper corona. At this wavelength range, we observe the emission line spectrum produced by the heavy ions in the corona. The regions surrounding sunspots and other active regions are areas where the magnetic field is strong. Extreme UV image The dark region in the X-ray image is called coronal holes,where intensities of magnetic fields are weaker than those in active region.
20 Extreme UV image III. Sun Coronal holes 12 Aug The magnetic fields in the coronal holes are open and extending far out into interplanetary space. Life times of coronal holes can be as long as several months. Therefore the coronal holes reappear in the Sun s 27-day rotation cycle. High-speed solar wind flows from coronal holes and causes disturbance in the earth s magnetosphere.
21 IV. Solar wind (interplanetary space) The Sun radiates a stream of plasma we refer to as the solar wind. The solar wind provides the energy that largely determines conditions within the space environment surrounding the Earth. The solar wind consists of a stream of plasma, and also carries the magnetic field of the solar corona into interplanetary space. The magnetic field is called the interplanetary magnetic field (IMF).
22 IV. Solar wind (interplanetary space) Magnetic field: Bt, Bz (nt) Magnetic field: Phi (degree) Density: (/cm3) Speed: (km/s) Temperature: (k) Solar wind 2 Jun. 2008
23 IV. Solar wind (interplanetary space) Solar wind Bt, Bz (nt) Phi (degree) Density: (/cm3) Speed: (km/s) Temp. (k) 2 Jun UT We take particular note of variation of Bz, density(n), and speed(v). Bz Storm, substomrs N formation of the magnetosphere V formation of the magnetosphere Near the Earth, typical values are as follows; V=450km/s, n=5/cc, T=10 5 k and B=5nT
24 IV. Solar wind (interplanetary space) Effect of coronal holes 18 Apr.- 15 May.- 11 Jun.- 8 Jul.- Solar wind velocity (18 Apr Aug. 2011) The period of the sun s rotates is 27 days, therefore the solar wind shows 27-day variations. Thus High-speed solar wind (from coronal holes) is observable periodically.
25 CME causes a increase of Bt, N, and V. CME-type variation 6/12-14 CME 6/16 21:15UT- 6/17 13:00UT CME-type variation is characterized by simultaneous increase of Bt, N, and V
26 CME causes a increase of Bt, N, and V. 6/12-14 CME 6/16 21:15UT- 6/17 13:00UT CME-type variation is characterized by simultaneous increase of Bt, N, and V -71nT
27 CIR-type variation is caused by high-speed solar wind which is radiated from coronal holes. In the case of CIR-type, Bt and N increases before high-speed flow arrives. CIR-type variation 05/07-13
28 CIR-type variation is caused by high-speed solar wind which is radiated from coronal holes. 05/07-13 In the case of CIR-type, Bt and N increases before high-speed flow arrives. -41nT
29 V. magnetosphere The magnetosphere is surrounded by solar wind, therefore the magnetosphere is controlled by the sun. IMF Bow shock Solar Wind Lobe Plasmasheet Sun Solar Wind Magnetosphere Here we show two famous index; Dst index and AE index. They are useful for the space whether to know Storm and Substorm (aurora).
30 V. magnetosphere Dst index Dst commonly uses as index of the magnetic disturbances. Especially we cans see magnetic storms because DST index reflects effect of the ring current. Magnetic storm started on 5 Aug. with negative DST index of less than -100 nt
31 V. magnetosphere AE index is for substorms. When substorms occur, AE enhances because of auroral electro jet. AE index
32 VI. Recent Space Weather Recent Sunspot number [Noaa Sunspot Number] Hinode XRT White:0, Skyblue: less than 40, Green: 40-80, Yellow: , Red: greater than 120
33 Recent Sunspot number
34 Recent Solar Surface Solar Dynamics Observatory/ Atmospheric Imaging Assembly Apr., 2012 Sept.,
35 Recent Solar Surface SDO MHI Magnetograms Apr., 2012 Sept., 2012
36 Recent X-ray Activity X5.4 Apr., 2012 Sept., 2012 X1.1 X1.4
37 Recent Solar Proton Activity 6530 PFU 469 Apr., 2012 Sept.,
38 Recent Solar Proton Activity halo halo Apr., 2012 Sept., 2012 partial halo(farside) halo halo halo partial partial(farside)
39 Recent Solar Proton Activity X5.4 M7.9 Apr., 2012 Sept., 2012 M5.1 (farside) M1.9 X1.1 X1.4 M1.7 (farside)
40 Recent Solar Wind Velocity by ACE Apr., 2012 Sept., 2012
41 Recent Interplanetary Field Activity Apr., 2012 Sept., 2012
42 Recent Dst Index Apr., 2012 Sept.,
43 Recent Space Weather Event 2012 March /02-16 Flare List 3/4 M2.0/1N LDE CME 3/5 X1.1/2B LDE CME 3/7 X5.4/3B CME X1.3/SF CME 3/9 M6.3 CME 3/10 M8.4 LDE CME Proton Event: 3/7 05:00UT- 3/12 21:00UT (max PFU at 3/8 11:15UT)
44 Recent Space Weather Event 2012 March /02-16 Flare List 3/4 M2.0/1N LDE CME 3/5 X1.1/2B LDE CME 3/7 X5.4/3B CME X1.3/SF CME 3/9 M6.3 CME 3/10 M8.4 LDE CME
45 Recent Space Weather Event 2012 March /02-16 Flare List 3/4 M2.0/1N LDE CME 3/5 X1.1/2B LDE CME 3/7 X5.4/3B CME X1.3/SF CME 3/9 M6.3 CME 3/10 M8.4 LDE CME
46 Recent Space Weather Event 2012 March /02-16 Flare List 3/4 M2.0/1N LDE CME 3/5 X1.1/2B LDE CME 3/7 X5.4/3B CME X1.3/SF CME 3/9 M6.3 CME 3/10 M8.4 LDE CME
47 Recent Space Weather Event 2012 March /02-16 IMF and Geosynchronous Orbit
48 Recent Space Weather Event 2012 March / /7 04:19UT- 3/8 00:00UT 3/8 11:03UT- 3/10 19:00UT 3/12 09:14UT- 3/13 00:00UT -75nT -133nT -50nT
49 Recent Space Weather Event Space disasters by this space weather event 2012/03/07 Dellinger phenomenon(communication failure) with the X class flare 2012/03/07 Venus Express satellite trouble 2012/03/07 SkyTerra1 satellite trouble 2012/03/08-09 Some aircrafts changed the route from via polar region to via lower region 2012/03/12 HughesNet Spaceway 3 satellite trouble Based on
50 Recent Space Weather Event
51 Recent Space Weather Event
52 Recent Space Weather Event First GLE(Ground Level Event/Ground Level Enhancement)of Solar cycle 24(2012/05/17) Because of the energy emission from the Sun, the radiation levels on Earth's surface rises to the degree that they are readily detected by neutron monitors. Gopalswamy et al., 2008
53 Recent Space Weather Event First GLE(Ground Level Event/Ground Level Enhancement)Solar cycle 24(2012/05/17)
54 Recent Space Weather Event First GLE(Ground Level Event/Ground Level Enhancement)Solar cycle 24(2012/05/17)
55 Recent Space Weather Event First GLE(Ground Level Event/Ground Level Enhancement) Solar cycle 24(2012/05/17)
56 Recent Space Weather Event First GLE(Ground Level Event/Ground Level Enhancement)Solar cycle 24(2012/05/17)
57 Recent Space Weather Event 4) First GLE(Ground Level Event/Ground Level Enhancement)Solar cycle 24(2012/05/17)
58 Recent Space Weather Event
59 Summary The Sun controls the Erath s magnetosphere. Summary of the space weather system is as follows. Sun Solar wind Magnetosphere Corona Solar wind substorm Coronal hole CME Flare High-speed solar wind Storm Proton event Intense X-ray Let s check daily space weather. You can meet more interesting space weather events!
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