Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.mao.kiev.ua/images/postbyemail/GERS%20S%20AKR.%20REL.%2016p.pdf Дата изменения: Fri Nov 20 13:30:02 2015 Дата индексирования: Mon Apr 11 01:47:50 2016 Кодировка: Поисковые слова: aurora

- , . ., . ., . . - (GERS) 202.97 (theauroralkilometricradiation -AKR) , , , , , , . - . 202.97 , . , , , - , - . [1,2,3,4,5,6,7,8,9] , AKR (during magnetospheric substorms), : (gyromagneticresonance) 1 ( ) (electronswithenergies 1 keV) (aroundthemagneticfieldlinesoftheplanets) (cyclotron) , , 1 3 ; (solarwind). AKR: , , 106 107 (W) [3]; (Spectrum): 30 ­ 800 , 10 1500 40 , 1.2 ­1.3 , 850 , 20 ( ) 600 ( ); (circular); AKR [7]. - , AKR [10,11] " ". , , m, , S ( S - ) tdm. m, S tdm [10,11]: mp mp lp lp tp tp m S; m tdm ; S tdm ; S m; tdm S ; tdm m, (1) lp tp tp mp lp mp lp, mp, tp ­ , ­ , . m, S tdm :


E mc2 Fp S hetdm , (2)
he

E t

p

­ , Ep ­ : E p m p c 2 ,Fp-

p

: Fp m p a p , a p - : a p S 1 S 2 , t , [10,11]:

l t

p 2 p

, m1 m2 ,
dm2

dm1

t

, R

F G

t tdm m1m2 SS Fp 1 2 2 F pc 2 dm1 2 2 . (3) 2 R R R

[12] (1) : , , , , , , , : , 5.9722 x 1024 7.3477 x 1022 4.8673 x 1024 6.4169 x 1023 1.8981 x 1027 5.6832 x 1026 1.989 x 1030 8.68 x 1025 1.02 x 1026 , 0.00443474 0.000054547302 0.0036143131 0.00047451718 1.40948454472 0.42201429314 1477.036 0.0645 0.0757 , 67.6 5495.94 82.95 631.78 0.2127 0.7104 2,0297 x 10 4.65 3.958

-4

- (GERE) 67.6 [10,11]. . 1 [10,11] , - 67.6 .

Fig. 1.­ GraphGERE. The dependence of signal power on frequency in the
frequency range from 65.7 GHz to 68.6 GHz with 0.1 GHz at the output of the measuringchannel. The signal power at the output of the generator is 4,5mW. [10,11].

1 (areinjectedfromtheplasmasheetregionintotheauroralregion) (andtherestarereflectedbecauseofthemirroreffectoftheconvergentgeomagneticfield)


[4]. ( ), 1.5. - 202.97 . , - , , 202.97 . , - . , , () , . , [13] , , , AKR (AKR ­ SKR) (DataobtainedbythreedifferentexperimentsonboardtheCassinispacecraft). These three experimentsare the Radio and PlasmaWave Science experiment (RPWS)[14], the Dual Technique Magnetometer(MAG) [15] and the Cassini PlasmaSpectrometer (CAPS) [16]. . 2 ( Cassini ­ RPWS 19/8/2004 ­ 21/8/2004, dayofyearDOY232.5-234.0) . 3 (DOY 224.0-240.0) [13] , Cassini ­ RPWS. 202.97 . . . 2b Cassini ­ RPWS (StokesparameterS = totalintensity), 2c 2d , 2c 2d. - .

Fig.2.Cassini-RPWS dynamic spectra for (a) the Stokes parameter S (= total intensity),
(b) the degree of circular polarization dc, (c) thedegree of polarization d and (d) the degree of linear polarization dLas a result of the Direction-Finding computations for the time period DOY 232.5­234.0, 2004. [13].


Fig. 3.(a) The RPWS dynamic spectrum, (b) the integrated SKR intensity
profile,(c) profiles for the SW ram pressure (solid) and bulk velocity (dotted), (d) profiles for the interplanetary magnetic field strength (solid) and its y-component (dotted) in KSM-coordinates and (e)the profile of the reconnection voltage at the dayside magnetopause of Saturn during DOY 224 ­240, 2004.[13].

- AKR . AKR 5 . 4 [7], AKR .

Fig. 4.Comparative spectra of auroral radio emissionsof 5 planets.[7] AKR , .4 . , GERS , GERS AKR . . GERS AKR, , AKR (. . 4). , AKR , , AKR AKR .


- (GERJ) 212.7 , (synchrotronradiation), JSR. 100 4 JSR [17]. (DIM) . (Inthefrequencyrangefromabout 100 MHztoabout 4 GHz, Joviansynchrotron radiation (hereafter referred as JSR) is emitted from the relativistic electrons, which is a non-thermal and incoherent radiation. JSR has a flat spectrum which is mainly in the decimeter (DIM) range). . 5 [17] ( AKR ), DIM (JSR) 212.7 . , 212.7 JSR.

Fig. 5.Spectra of Jovian magnetospheric radiations. The power flux is
normalizedto constant distance. The spectrum of the Earth's is also shown asacomparisonwithJupiter.[17].

JSR . 6 [18].

Fig. 6.JSR spectrum from 74 MHz to 8 GHz measured in July 1994 (blue
circles) and September 1998 (red circles). The red and blue solid lines are the results of a model simulation.[18].

. 6, . 5,, GERJ JSR. , GERJ JSR.


GERS AKR (AKR terrestrialKR, TKR) AKR ­ SKR. , TKR , , [1,2,7,19,20,21]. [19] TKR, JIKIKEN (EXOS-B). , TKR 100 300 , , , 1.5 2.15 (Existenceofthespectrumpeakaround 100 kHzto 300 kHz, then, indicatesthatastrongwaveparticleinteractionistakingplaceinarangefrom 1.5R, to 2.15R,suggestingtheauroralparticleaccelerationinthisregion.). EnergySpectrumofParticles (ESP) (Energyspectrumofparticlescanbeanalyzedusingchanneltronmultiplier, inanenergyrangefrom 10 eVto 20 keV, bothfortheelectronandprotons.) 10 eV 20 keV. . 7 [19] TKR, ESP.

Fig.7.The energetic particle spectrum measured by ESP.[19]. . 7 , 200 , , , , 150 - 175 , 120 , 80 , 40 . . 8 [19] TKR.

Fig.8.Dynamic spectra of the terrestrial kilometric radiation.[19]. TKR .8 TKR 202.97 . TKR , , . 202.97


. . 7 . 8 , - TKR. 202.97 - , ­ 202.97 ( ). [21]Imager forMagnetopause-to-Aurora Glob Exploration (IMAGE) Polar spacecraft (Several year's worth of observations from the plasma wave instruments on both Magnetopause-to-Aurora Global Exploration (IMAGE) and Polar spacecraft are used to study the seasonal and solar cycle variations in the spectrum of auroral kilometric radiation (AKR)) AKR. (the average spectra of AKR as a function of dipole tilt angle) AKR. , . 9[21] .

Fig. 9.The average spectra of AKR as a function ofdipole tilt
angle from observations by the IMAGE/RPIinstrument.[21]

AKR : 80 500 260 , 60 250 150 . (-16 -16.5 ) AKR 200 . , AKR ­ 16 , 200 , 0 ­ (27-28) ­ 200 . , ­ - . . 10 [21] AKR , IMAGE Polar.


Fig.10.Comparison of the average spectra over the same dipole tilt ranges
where the emission peak isapproximately constant for both Polar/PWI (blue) andIMAGE/RPI (red) for positive (top) and negative (bottom)dipole tilt angle. [21].

. 10, AKR 202.97 , Polar - . [20] MF/HF 4 7 , Wind. (We present observations of MF/HF ionospheric radio emission observed between 4-7 Re in the terrestrial magnetosphere by the Wind spacecraft.). 1.8 , (moresteadyandweakeremission) 4.4 . . 11 [20] AKR MF/HF, Wind.

Fig. 11.Power spectra during the MF (top) and HF(bottom) events from the RAD1
(0.02-1.04MHz) andRAD2(1.075-14MHz) receivers. TheMF emission in the top panel peaked at f 1.8 MHz has bandwidth f/f 0.14 HFemission is peaked near fHF 4.5 MHz and has a similarFWHM bandwidth.[20].


. 11, AKR , 202.97 . AKR 400 , 500 , 600 800 . 500 , , AKR, GERS 202.97 , : 2, 3, 4. MF HF: 1.8 ­ 9 ­ GERS 4.4 ­ 4.6 ­ 22 23 GERS. . 12 [22]AKR, MEMO Interball 2.

Fig. 12.AKR event recordedby MEMO on January 28, 1997, with an electricsensor.The
spectrogramstartsat 1952:20 UTandendsat 2124:58 UT.[22].

. 12 202.64 AKR 202.97 GERS. POLRAD Interball 2 AKR 4 ­ 1 . . 13 [23] 202.97 GERS 406 609 .

Fig.13.AnexampleoftheAKRrecordedwith Interball 2 bythePOLRADradio-spectro-polarimeter.[23].


GERS AKR , GERS AKR. AKR [24,25] 1.2 - 1.3 200 . :GERS AKR 202.97 . - (GERS) 202.97 AKR , , , . - (GERJ) 212.7 JSR. , " " . [1] Gurnett, D. A.,:The Earth as a radio source: Terrestrial kilometricradiation, J. Geophys. Res., 79(28), 4227­4238, doi:10.1029/JA079i028p04227, 1974. [2] Kurth, W. S., M. M. Baumback, and D. A. Gurnett,: Direction-findingmeasurements of auroral kilometric radiation, J. Geophys. Res.,80, 2764 - 2770, 1975. [3] Kaiser, M. L., and Alexander, J. K.,: Terrestrial kilometric radiation. III - Average spectral properties, J. Geophys. Res., 82, 3273-3280, 1977. [4] Wu, C. S. and Lee, L. C.,: A theory of terrestrial kilometric radiation,Astrophys. J.,230, 1979. [5] Benson, R.F.,Auroral kilometric radiation:Wave modes, harmonics, and source region electron density structures., J. Geophys. Res., 90, 2753-_2784, 1985. [6]Hayes, L. M. and D. B. Melrose,: Generation of ordinary mode auroral kilometric radiation from extraordinary mode waves., J. Geophys. Res., 91, A1, 1986. [7] Zarka, P.,: Auroral radio emission at the outer planets:Observations and theories, J. Geophys. Res., 103, 20159,1998. [8] Louarn, P., and D. Le QuИau,:Generation of the auroral kilometric radiation in plasma cavities ­ I. Experimental study, Planet.Space Sci., 44(3),1996. [9] Morioka, A. et al.,: Fundamental characteristics of field ­ alignedauroral acceleration derived from AKR spectra, J.Geophys. Res., 117, doi:10.1029/2011JA017137, 2012. [10]Timkov, V. F., Timkov, S. V., Zhukov, V. A.,:Planck universal proportions. Gravitational electromagnetic resonance., Fifth InternationalScientific Conference:"Metrology, technical regulationsandquality assurance.",Collection of scientific papers., p.p. 72 ­ 78, 2015.
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