Ch 1 The Sun

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(1). Ch 1 The Sun. Ch4 Upper Atmosphere and Ionosphere . .

(2). Ch 3 Magnetosphere . .

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(8) * ,+-. Ch 2 Interplanetary Space. Mar. 1. 2006. Ch 5 Space Surrounding and Probing & Space Science and Technology. . Space 50km Geospace

(9) Geo- . . . . 1- 4Re.

(10) . Mar. 1. 2006. Chapter1 The Sun, Solar 1-1 Introduction 1. One of the 1011 stars in our galaxy absolute visual magnitude 4.72 at the middle of main sequence(. ./. http://www.geocities.com/chokseng02/chokseng/t 7.htm).. 2. Life ~4.6x109 ~50 Radius ~100RE RE6370 Mass ~3.3×105 ME ME5.971027g Density ~1.4 g/ 3 . g ~2.7×102 m/s2 1A.U.mean distance between the earth and the Sun ~ 2 RE Power Output3.9×1033 ergs/s Rotation period: differential rotation

(11) . (Sunspot

(12). . ). 0: 24d16h 30: 27d4h 75: 33d. near pole: 35d . Sunspot . . . . . . . . . . . !. ". #. $. %. . 27 .

(13) 1-2 Cross Section of the Sun & ' physical condition/process/state. 1. Core0.3R. 0. energy source 7. (i) T ~ 1.5×10 K P ~ 150 atm. (ii) main: H+, small amount of He++ (~1%), heavy elements (iii) energy sourcethermal nuclear fussion ( ) 2. Radiative Interior . 0. thickness ~ 0.5 R. Energy transport by radiation process * + , - . % 3. Convective zone . 0. thickness ~ 0.2 R Energy transport by convection 4. Photosphere thickness~ 0.1% R. 0. depend on . (i)effective temperature. i.e. best fit blackbody radiation. T~5750K Energy source: from inside Transfer process: radiation (ii)Limb Dark effect visible disc physical picture. TA/TC I0T4. 5. Chromosphere thickness ~ 10000 (i) H Line 1 2 3 4. =>IB/ID. ~65635Å. (ii) temperature variation 6 Chromosphere 7 8 9 500 5000 :10000 . ~5500 °K 4500 °K 10000 °K~50000 °K 500000 °K. Mar. 1. 2006.

(14) . Mar. 1. 2006. 6. Corona T1.5×106 °K Corona size(thickness) depend on sunspots. Density variation Ne 0 1/;2 for ;/5 5 . !. " <. 8. =. >. ?. @. . . A. B. CD. where;=r/R . E. F. G. 0. H. 1-3 Sunspot and Solar cycle 1. Sunspot characteristics: (i) Low temperature: 3900°K (ii) Intense magnetic field: 200gauss (Zeeman effect) (iii). Pair . (iv). Cycle~11.25 years (minimum minimum). . K. L. (I J. 0.3gauss). H. P. CQ 4.6 H. F. M. N. O. R. S. N. Q 6.7 H.

(15) . Mar. 1. 2006. 2. Wolf Sunspot number (Solar activity index, SSN,R) Wolf number: Rk(10gTf) f: number of individual spot g: number of group k: comparison constant ~1 Solar min R 0 Solar max R 200 U5 Butterfly diagrams(V W. X. ): Sunspot YZ [. \. ]. F.

(16). &. ^. http://science.msfc.nasa.gov/ssl/pad/solar/images/bfly.gif 3. 1st cycle: 1755~1766 Now: 23rd cycle 1996~2007 The Maunder Minimum: 1645~1715 Little ice age, No tree ring, Sun-weather relation: cold! Quiet Time: sunspot number minimum solar Active Time: sunspot number maxmum.

(17) 1-4 Solar flare # $. Mar. 1. 2006. and Prominence % &. 1. Solar flare: sudden enhancement _=6563Å5`a e f ! " I J X-raygEUVgUV 2. Mechanism: Magnetic field merging. h i. j. k. N. b. c. d. l. http://www.c-science.com/txt/tc/un/990310un.htm 3. Characteristics rise time ~ a few minutes decay time ~1~3 hours 4. Prominence(m n ): oY solar flare p q. r. s. t. u. K. r. v. w. Gigantic luminous arch structure when viewed at the limb of the Sun and long dark filments when projected on the solar disc..

(18) . Mar. 1. 2006. 1-5 Solar radiation( ' !!) Solar energy radiation Steady energy radiation ( ) * + EM wave---Control ionospheric structure/dynamics. Formation of the ionosphere Solar wind (300-800km/s)--- Formation of the magnetosphere Transient energy radiation EM wave(flare) Plasma cloud(high energy particle). anomalous ionization magnetic storm ionospheric storm.

(19) 2-2 Solar wind (r=1AU )e-H+ He++

(20) 300-800 /s . 5 pair/ 3. . 105K. Mar. 15. 2006. http://science.nasa.gov/ssl/pad/solar/images/DialPlot.jpg. Assumption: (1) uniform / viscosity (2) v v (3) ! (4) " # $. . . (5) % & % # (6) ' ( $ % ) * * % + , - . / % % ! ' 0 1 2. 3. 4. - 7 / " # $ 0 1 8. 5. 6. . 4. 5. 6 - 9 / : % ! 0 1 . − 1 dA v2 A (1 − 2 ) cs. dv = v. ;<. => ? % @ H. I. J. K. A

(21). H. I. J. C. => ? % @ G. B. N K. J. D. A. L.

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(23) E. F. . G. M. B.

(24). C J. D O.

(25) E. F. M. . U. r v2 v r − ln( ) 2 = 4 ln + 4 c − 3 P8 Q R S 4 5 2 cs rc r cs kT Q R D

(26) C sΘ = where T=1/2, mp= proton mass µm p V. W. I. GM M=Q R 2c s. rc =. rc = 4 − 7 r A C. D.

(27). . X. . GM=Q R. Y. (Z. H. I. [. \. ]. ^. _. )M.

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(29) `Q . 1. R. S. a. b. c. ]. d. e. Q. R. d. e. . f % + - . / % ' ? g $ + + h ! % - 7 / i 0 ! % # ? % . dr = Vs dt. dt =. dr j Vs. dφ = −(r − rc )Ω j dt. r. % % % - ;k /g r = rc φ = φ 0 B = B0 rˆ . r = Vs t + rc dφ − ΩV s t − Ω(r − rc )t = = dt r r rc Ω dφ = − [(1 − dr ] Vs r. V r r − 1 − ln = s (φ − φ s ) j

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(32) rc rc rc Ω l. m : ;k . 4πr 2 Br = 4πr02 B0 .

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(34) . Mar. 15. 2006. r Br = B0 ( c ) 2 j r . dr rdφ = Br dt Bφ dt Bφ = − B0. Ω rc 2 ( ) (r − rc ) j Vs r. . n . > 1 o 1 p 7 9 q 7 1. h ? # ? - % + # # r. s. t. u. v. w. /. . . x # y y . V r =− s φ rc rc Ω. 0 1 . r 1 Br = B0 ( c ) 2 ∝ 2 r r Ω rc 2 1 Bφ = − B0 ( ) r ∝ Vs r r . r Ω 2 r 2 12 BTotal = Br2 + Bφ2 = B0 ( c ) 2 (1 + ) r V s2 B rΩ θ = tan −1 φ = tan −1 Br Vs z. {. 2. |. }. ~. . 9 1. ? . β=. 1 2. ρVs 2 + 3nkT BT2. 8π. ; % ' % ' % % ' % ' .

(35) . Mar. 15. 2006. + + $ % - ? $ # # i + - d. Y. |. d . Y . | . . / . /. x + " % # ! % + + ? % # % % ' ? ' " % + % + ? ' 1 . . .

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(37) . Mar. 22. 2006. Chapter3 The Geomagnetic Field and Magnetosphere (Geospace) 3-1 The Earth’s Magnetic field The first order the earthquake’s magnetic field is that of a dipole whose axis is tilted with respect to the spin axis of the earth by 11.. http://www.tsjh.tc.edu.tw/t28/. /

(38) . .JPG. Dipole Model Earth’s dipole magnetic field. (unit: Gauss). ME (2 cos θrˆ + sin θθˆ) r2 = Br rˆ + Bθ θˆ B=−. 0.6 RE3 cos θ 0.3RE3 sin θ ˆ =− rˆ − θ r3 r3 θ = co − latitiude.

(39) . . . 10 . . . Mar. 22. 2006. ~14N . now~16N. . 65

(40). . . . . . mathematically Bx B y Bz = = dx dy dz for polar coordinate 2 cos θ sin θ = dr rdθ. B Br = θ dr rdθ. dr 2 cos θdθ 2d (sin θ ) = = r sin θ sin θ. ln r = ln(sin θ ) 2 + k ' r = k sin 2 θ when =90 r = re = k r = re sin 2 θ , re : let. r =l RE. L=. re RE. .

(41). . . . . . . . re =L RE. at Taiwan, L=1.2 or 1.3. L-valueThe radius of the equatorial crossing point of the field line. L-shell Example. L. . . . . . . . 60 . sol.. θ = 30 o r = RE 1 1 RE = re sin 2 θ = re ( ) 2 = re 2 4 re = 4 RE L=4 3R E. h = 3RE = 3 × 6400 = 19200(km). . . . . . . . !. ". #. . $. #. %. &.

(42) 3-2 The Magnetosphere ' ( ) * + , -. .. . /. 0. Solar wind at 1AU n~5 #/cm3 v~500 km/s T~1.61105K B~5nT Cs~50 km/s 2(flow energy)~1keV Vhm = MA=. B 4πρ. ~ 60 km/s. V ~8 Vhm. 3.2.1 Collisionless Bow shock and Magnetosphere Bow shock 1. Bow shock 3 4 Jump condition. v1 n2 = ≅4 v 2 n1 1<. 5. . 6plasma density. B2 <4 7 B1. T2 ≅ 20 8 T1. supersonic. subsonic. . . Mar. 22. 2006.

(43) . Quasi-parallel shock. Mar. 22. 2006. perpendicular shock.

(44) . 2. . Mar. 22. 2006. 9. In physical parameter, such U, T, n, B, are pretty much defined by “jump” condition. 3. Magnetopause( ' :. ). Solar wind pressure is balanced by the magnetic pressure. Chapman and Ferraro’s model B 2 (2 B0 ) 2 B02 = = 8π 2π 2π Kinetic pressure = F∆P = nv(2m p v) = 2nm p v 2.

(45) 2nm p v 2 =. Mar. 22. 2006. B02 2π. B2 1 nm p v 2 = 0 2 8π. ;< .

(46). M. P. N. g. O. D. h. A. J J. }. A . R. S. `. x K. . Q. 6i. I I. = h. y L. B 6. T . z. . . F . g. . . X. l }. . 8. W. k. | D. J. V. j. {. &\ I. U. R. m. . \ . D. o. . I . A \. p. . @ [. n. . ?. Y 6Z. @ . >. D m. J <. . B. . . q. [ r. K. C ] s. . . . D. E. F. < 6^ t. L 6\ . . . C. &< u. D . O. P. h. z. . \ h. A `. w >. R. H _. v =. 6Q. G. \ D. B a. O. &. J. b. O D. I >. ] . B. } r. <. ¡ ¢ ¢ £ ¤ ¥ ¦ § ¥ ¨ © § ¥ ª ¢ « ¬ ¨ ¦ ¬ ¨ ¢ « ® ª « ¢ « § ¦ ¯ ¦ ¨ ° ® °¢ ¦ © ¨ ± ¥ ¤ ² < ¡ ¢ ¢ ª ª ª ¥ ³ « ¥ ¦ ¬ ´ § ¥ ¨ © § ¥ ª ¢ µ ¶ « °® ² ¶ · ¢ ¨ ¯ · ® ® ´ ¢ « § ¦ ¢ « § ¦ ¥ ¤ ² ¸ ¹ ¨ ² ® « ¨ « ¤ ® ² ® º ³ <. . B. O . . A. N. &. . E ~. M. L. f. D F. 6A . K. c d e. P [. . . . s. .

(47) ;< ;. . ^. . À $. . . . #. Á. '. :. . . ». ¼. ½. ¾. &<. ¿<. 0.6 R E3 cos θ 0.3R E3 sin θ ˆ B=− rˆ − θ< r3 r3 ¿ Ã ¶ § « « 6Ä ¿ Å Æ Ç È É Ê d d ´ ¤ 6 ¿ Ë. . A . $. Â. % &Î. Õ . . B . Ï. $. . 5. Ö. Mar. 22. 2006. . ×. ¿ Ð d d ´ ¤ ¢ « 6Ñ. . C. $. . . Ò c \. Ó. ÔØ Ñ. Ò. . . !. ' C. :. . #. 6° Ì Í. Ù Ú c µ Ø $. # $. Í #. . Û. %. Ô Ü &<. < Ý « ® ²Þ <. B2 1 nm p v 2 = 0 2 8π. c <. − 0.3(6400) 3 2 ( ) 1 r3 (10)(1.6 × 10 − 27 )(500) 2 = 2 8π (2) r = LR E sin 2 θ r = L(6400)(1). . ä. L=?. : 6400 = L(6400) sin 2 θ ' θ '= ? θ '

(48) , ~. (3) Φ = ;ã. r = ? (Ò ß à á × g â ). 3 RE RE. . B ⋅ da < . '. K. L. å. The Schematic of the Earth’s magnetosphere æ ç http:// space.rice.edu/IMAGE/livefrom/sunearth.html.

(49) Chap 4 Th Earth’s Atmosphere and Ionosphere 4.1 Structure of the Atmosphere. (a) Classified by neutral temperature. http://www.ux1.eiu.edu/~cfjps/1400/FIG01_019.JPG. (b) Classified by mix equilibrium and dynamic process. http://apollo.lsc.vsc.edu/classes/met130/notes/chapter1/vert_comp.html.

(50) (c) Classified by ionization. http://gbailey.staff.shef.ac.uk/researchoverview_images/ionosphere_01.JPG. Definition of Ionosphere: . . . . . . . ∂N = Q − L − ∇ • ( Nν ) ∂t Q"# $ % L"& ' % ∇ • ( Nν ) " (. ). . . . . . !. .

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(52) 4.2 Formation of Ionosphere 4.2.1 Production. Chapman Layer: The explanation of ionospheric electrons number density production. It combines different species in different altitude (Fig. 2.19) and the radiation from the Sun with different zenith angle(*) that I = I ∞ e. −. s. τ. different height and different * (Fig. 2.20). +I", 0",. 1. 2. then gets the production rate in -. .I/"*=0 . ,. -. ..

(53) What is zenith angle?. Solar zenith"The angle between the local zenith and the line of sight to the sun. View zenith"The angle between the local zenith and the line of sight to the satellite. 3. 4. http://asd-www.larc.nasa.gov/SCOOL/definition.html.

(54) 5. 6. ". 1. 7 8. 9. :. . ;. ". <. =. 2. 7 8. 9. :. . <. "A. B. CD. 3. . L. M. N. O. L. P. Q. . <. ]. U^. \. _. . `. a. L. . *> "R. b. . @. FG. H. I. I. S. T. E. ?. c. . Ud. e. f. . J. . . . 2. CA. UV. R. I. . W. X. Y. . . L. R. I. . M. N. O. / D. B. K. UZ. [. L. @. \. R. E I. K. F @. . . . hm ( χ ) = hm ( χ = 0) + H ln sec χ H"scale height.hm"The peak height (where the number density is the max.) in Chapman’s layer. q m ( χ ) = q m ( χ = 0) cos χ qm"The peak production rate in Chapman’s layer. . . L. . #. $. ). >. g. h. $. . i. 1. ". jklmnj o .lm"pqr s t uv w x yz. {. . ~ r q # r # r #. $. #. $. $. . . . qr . . e. ,. $. . . " t . |. }. @. "v w x 4. e. ,. . . . . }. s s t r s t . "pqr s t . U£. . . . K. ¤. ! yK. UQ ¥. ¦. §. ¨. qr , ©. ª. «. ¬. . ! O. ®. . \ @. . ¡. ¢.

(55) 4.2.2 Loss. (1) Dissociative recombination"p¯ o n po ¯ . O2+ + e − → O + O + 6.96eV L = αN 2 USquare LossU°. Ex" N 2+ + e − → N + N + 5.82eV. ±. ². L. . . NO + + e − → N + O + 2.76eV . L. @. (2) Charge transfer or atom-ion exchange reactions or charge exchange recombination X + YZ n p¯ o ³. O + + O2 → O2+ + O + 1.53eV. Ex" . . . L. (3) X + e + M n X + M ´ T. ±. Y. L. (F2 region@. -. (4) ¹. L = β N ULinear LossU°. O + + N 2 → NO + + N + 1.09eV. Loss . . L. º. ¹. O. i L. 1 . Q. µ . ¶ ». R. ·. ¸. D. U£. R. ·. h. $. @. ¼. Night time: The higher ionosphere exists linear loss (the species is O+) and transport but without production.. Night time: The lower ionosphere only exists square loss (the species is NO+) without production and transport..

(56) 4.2.3 Transport (Movement) . (½) Conjugate ¾ 8. Â. ¾. ¿À. ¿"I. (. Á. . Ã. J. Ä. Å. Æ. }. Ç. . È. É. Ê. U7. Ë. Ì. Å. Æ. }. . È. Ê. Í. . ¾. ¿@. 3. http://www.kurasc.kyoto-u.ac.jp/~epic/activities/COPEX.html 4. K. Conjugate Effect. !. . Î. . É. . . . Ï. Ð. . . . . ¾. ¿. . K. ¤. @.

(57) (Ñ) Neutral wind effect Ó. ×. Ø. Air Draft . Ò. . . Ô. àUÚ. Ù. f. â. . . Ú. &. (hmF2). Ô. f. '. . ). . Ö. . . Ï. ç @è. Ô. Õ. . Ué. . ß. Ç. ó. È. í. J. É. î. ô. Q. . Uù . ú. Ô. L. Y æ. ë U´.

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(59) @. . . ø. . Ô. . . K. UÏ ä. . Ð. å. Ù Uë. . . áü. L O. Ý. Uã. æ. $. . }. § ì. Ï. L. . æ. Ú. Ð. . . æ. . . Ô. S. Þ. O. (NmF2)áâ . . UL. . Y. . Û. Ç. Ü î. Å. Æ. . yL }. æ. í. ß Y. î Uá. @. Á. #. Q. Æ . Ø L. À. ö. Å . ê f. ñ. /õ. û. Ü . . àUÚ. Ù. Û. Uáâ. (ï) Fountain Effect ð ò. . . æ. ä ô. ð. ÷ ý. Ø. ñ. U. À. þ. Á. ø Æ. . ò. ä ó. . U. . ¥. Å. g. . ø ±. Q. ô. Uyò. E × B drift å. Å. ò. ó. È. Ê. Å. ê. §. . Ø. 1 ×. v s r s lr ó . g. ô. . Y. . O. ®. @.

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(61) 4.3 Morphology of the ionosphere CIonosondeF. . . L . . . ±. Y . CHFF. . . " . . . L. . . . %. C . . . "h. . . . . UZ. ^. \. ¹. . ". #. $. ". %. CfrequencyFv.s.!. %. . . . T. @ . / Y. . . . . F . f. Y. . . . ! Y !. Cvirtual heightU h '=. @ @. c∆t F 2 . . CIonogramF @ &". " . . L . . . 3. h. 1-30MHzU . 8KHz h '. . . . @. "http://www2.nict.go.jp/dk/c233-235/HOWTO.html 4. ωH qB ,ω H = 2π m. &"fxF2-foF2=1/2fH.Here fH is gyro frequency. f H =. Ionospheric Variation (½)Diurnal Variation f 0 E ∝ R12 (cos χ )1/ 2 Fig. 5.9 f 0 F1 ∝ R12 (cos χ )1/ 2 Fig. 5.10 E y F1 L. f 0 F2 ∝ F (cos χ ) F2 L. *U+ .. À. Á. NmF2 K . /. . å. §. @. U¡ !. ¢ . ý. . (. ). ). U. . . *U£. U1200-1800LT V. (. ú. *,. ý. . $. y&. '. È. ) ). @ 1999/9/17 ». . #. . . U. . 4. ±. ð. ñ. -.

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(63) ¹. O. L. . . . Daytime Region. Nighttime. Density(el/cm3). Density(el/cm3). 10. 10. F1. 10. 5. disappear!!!. 180~220 km. E. 104~105. <103(disappear). 90~110 km. D. 102~103. disappear!!!. 80 km. F2. C. 5. Peak height. 6. 250~500 km. 70 km.

(64) (Ñ) Seasonal Variation Seasonal Anomaly 0 < Ô S Þ 1 ú Y. Uå. §. < 0. . W. X. +. !. . Y. . è Ï. Á. @. Ð. U/ g. ú. è. Á. 7. . ". XY . . Y. Y 2. ± 3. UÐ 4. 5. & 6. '. ). . +. O + XY → XY + O. XY + + e − → X + Y Ï Ð UÐ 5 6 Ç 9. U7. 8. è. Á. . UQ. Loss Process.C´ . . g. W. X. . F. (ï) Solar Activity Variation foEufoF2 :. . . Ï. Ð. :. (. . B. § ;. < U+. )U´ . ù . :. . . 120 ù. Ç. saturation effect.. &"Solar Activity Index"SSN F10.7(C D. E. 5. ). ë =. >. ?. @. >. A UR. Z. .

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(67) (F) Latitudinal Variation (Geomagnetic Contral) 1. ð ñ. À. Á. å. §. . ò. ó . g. ô. 2. Temporal Variation a. Sporadic E Layer Occur over a range of heights from about 90 to 120 km or more. Es is transient, localized patches of relatively high electron density in the E region of the ionosphere which significantly affect radio wave propagation. Es is a comparatively strong and protracted transmission ‘returned’ from the E region of the ionosphere by some mechanism other than the normal reflection process from the daytime E layer..

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(69) Sporadic E can occur during daytime or nighttime, and it varies markedly with latitude. It can be associated with thunderstorms, meteor showers, solar activity, and geomagnetic activity.. b. Spread F Spread F is caused by the scattering of the signal from irregularities embedded in the ionosphere. Spread F is generally defined in terms of the appearance of an ionogram rather than in terms of the physical mechanism involved. This has led to a division into “range spread” and “frequency spread”..

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