PROBLEMS OF GEOCOSMOS

More documents

Recommendations

Info

Proceedings of the 7th International Conference "Problems of Geocosmos" (St. Petersburg, Russia, 26-30 May 2008) r ∂M G r ∂M G r A = μ ( x − y ) , μ 0 ∂Y 0 ∂X 0 2 2 2 2 r ∂ MG r ∂ MG ∂ MG r ∂ MG r Aτ =τ 0( x0 + ( + ) y0 − z0) . 2 2 ∂X∂Y ∂X ∂Z ∂Z∂Y The outer “dipole part” of the field Aμ r is related to the magnetopause/mantle field provided by the “two wire” current structure with two ± opposite currents. The inner “toroidal” part τ is provided by “ Ar θ ” type cylindrical toroid current structure in the magnetotail. Generation of the potential field ϕ by moving magnetization, which is equivalent here to the moving electric dipole polarization is not considered here. These components are expressed via derivatives of the characteristic function M r 4π ( X , r0 , v') = ( 2π ) ∫ r r r 2 2 exp[( −k r0 / 2) + ikX ] dk r r , 2 k D ( k , kv' ) G 3 r T r 2 2 2 where DT ( ω, k) = 1− ( ω / c k ) εt ( ω, k) and ε t ( ω, k ) is the transversal part of the dielectric r r permittivity tensor ε ( ω, k ) . When ( ω , k ) = 0 we have e.m. field modes in plasma and get ij D T plasma resonance. r The real part of the complex value ε t ( ω, k ) is related to diamagnetic properties of the flow r r and forms the current jd , and the imaginary part of ε t ( ω, k ) is related to resistive properties of the r r r flow and forms the resistive current jr . Vectors jd and jr are collinear in an isotropic plasma, but have different spatial distribution and differently depend on e.m. field. In the kinetic approach to the CFP, there are three physically different “regimes” of flow. We have the “subsonic regime”, which is realized for the solar streamer generation v '< c > v >> c which describes the plasma as an MHD medium [3]. For the first two cases [1,2], the characteristic function can be represented as I x e s ∞ 2 2 1 ξ ⊥ Re m M G ( χ, ρ ⊥ , Re m , GV ) = dξ ⊥ξ ⊥ J 0 ( ξ ⊥ρ ⊥ ) exp( − ) I x ( ξ ⊥ , χ, Re m ) πr ∫ , 2 0 G 0 ∞ 2 2 2 2 ξ x Re m ( ξ ⊥ + ξ x ) ( ξ ⊥ , χ, Re m , GV ) = 2Re∫ dξ x exp( iξ x χ − ) , 2 2 ( ξ + ξ ) − i | ξ | ξ + G ξ where χ = x / rG , ρ ⊥ = r ⊥ / rG are dimensionless cylindrical coordinates and krG is a dimensionless wave vector with the cylindrical components r r ξ = ξ ⊥ and ξ x . Here, Rem = r 0 / rG is the r magnetic Reynolds number and r = r is the anomalous skin depth expresed via f (| v |) [1]. skin G From the expression given above we see the key role of the parameter GV called “quality” which r determined by form factor of the VDF f (| v |) . Parameter GV governs the 3d topology due to the variable character of the dispersion in the denominator of the characteristic function M G ( X , GV ) . We have a transition from the “resistive” state with a long ray structured magnetic tail to the diamagnetic r G > 1, which explains in the nonadiabatic transition the effects of the magnetic V substorm and the effect of coronal mass ejection (CME). The parameter G ≈ κ / κ V V D 89 G 2 ⊥ s 2 x s e x e V 2 x
Proceedings of the 7th International Conference "Problems of Geocosmos" (St. Petersburg, Russia, 26-30 May 2008) as the ratio of diamagnetic to resistive current is determined in a hot collisionless isotropic plasma by the ratio of the “momentum anisotropy” κ ≈ v'πf ( v') provided by the “resonant” particles to the “energy ∫ G 2 2 anisotropy” κ ≈ −2v' du( ∂f / ∂u ) of the “nonresonant” particles of the flow providing the flow D dynamical pressure. For the Maxwellian plasma f = f we have G v' / v
Page 1 and 2:
Saint-Petersburg State University P
Page 3 and 4:
Proc. of the 7th Intern. Conf. "Pro
Page 5 and 6:
Page 7 and 8:
Page 9 and 10:
Page 11 and 12:
Î�ÒÙ×�ØØ��Ñ��Ò
Page 13 and 14:
Proceedings of the 7th Internationa
Page 15 and 16:
��ÒÓÛÐ��Ñ�ÒØ
Page 17 and 18:
Page 19 and 20:
Page 21 and 22:
Page 23 and 24:
Page 25 and 26:
Page 27 and 28:
Page 29 and 30:
Page 31 and 32:
Page 33 and 34:
Page 35 and 36:
(the first number), two three-lette
Page 37 and 38:
Page 39 and 40:
Page 41 and 42:
Page 43 and 44:
Page 45 and 46:
Page 47 and 48: vertical fields. The vertical field
Page 49 and 50: Proceedings of the 7th Internationa
Page 97: Proceedings of the 7th Internationa
Page 149 and 150:
Page 151 and 152:
Page 153 and 154:
Page 155 and 156:
Page 157 and 158:
Page 159 and 160:
Page 161 and 162:
Page 163 and 164:
Page 165 and 166:
Page 167 and 168:
Page 169 and 170:
Page 171 and 172:
90 60 30 0 -30 -60 Proceedings of t
Page 173 and 174:
Page 175 and 176:
Page 177 and 178:
Page 179 and 180:
Page 181 and 182:
Page 183 and 184:
Page 185 and 186:
Page 187 and 188:
Page 189 and 190:
Page 191 and 192:
Page 193 and 194:
Page 195 and 196:
Page 197 and 198:
Page 199 and 200:
Page 201 and 202:
Page 203 and 204:
Page 205 and 206:
Page 207 and 208:
Page 209 and 210:
Page 211 and 212:
Page 213 and 214:
Page 215 and 216:
Page 217 and 218:
Page 219 and 220:
Page 221 and 222:
Page 223 and 224:
Page 225 and 226:
Page 227 and 228:
Page 229 and 230:
Page 231 and 232:
Page 233 and 234:
Page 235 and 236:
Page 237 and 238:
Page 239 and 240:
Page 241 and 242:
a Proceedings of the 7th Internatio
Page 243 and 244:
Page 245 and 246:
Page 247 and 248:
Page 249 and 250:
Page 251 and 252:
Page 253 and 254:
Page 255 and 256:
Page 257 and 258:
Page 259 and 260:
Page 261 and 262:
Page 263 and 264:
Page 265 and 266:
Page 267 and 268:
Page 269 and 270:
Page 271 and 272:
Page 273 and 274:
Page 275 and 276:
Introduction ON THE NATURE OF PLASM
Page 277 and 278:
Page 279 and 280:
Page 281 and 282:
Page 283 and 284:
Page 285 and 286:
Page 287 and 288:
Page 289 and 290:
Page 291 and 292:
Page 293 and 294:
Page 295 and 296:
Page 297 and 298:
Page 299 and 300:
Page 301 and 302:
Page 303 and 304:
Page 305 and 306:
Page 307 and 308:
Page 309 and 310:
Vy Here index j =1,2 characterizes,
Page 311 and 312:
Jy Proceedings of the 7th Internati
Page 313 and 314:
Page 315 and 316:
Page 317 and 318:
Page 319 and 320:
Page 321 and 322:
Page 323 and 324:
Page 325 and 326:
Page 327 and 328:
Page 329 and 330:
Page 331 and 332:
Page 333 and 334:
Page 335 and 336:
Page 337 and 338:
Fig. 3. Dependence of 1D interpreta
Page 339 and 340:
Page 341 and 342:
Page 343 and 344:
Page 345 and 346:
Page 347 and 348:
Page 349 and 350:
Page 351 and 352:
Page 353 and 354:
Page 355 and 356:
Page 357 and 358:
Page 359 and 360:
Page 361 and 362:
Page 363 and 364:
Page 365 and 366:
Page 367 and 368:
Page 369 and 370:
Page 371 and 372:
Page 373 and 374:
Page 375 and 376:
Page 377 and 378:
Page 379 and 380:
Page 381 and 382:
Page 383 and 384:
Page 385 and 386:
Page 387 and 388:
Page 389 and 390:
Page 391 and 392:
Page 393 and 394:
Page 395 and 396:
Page 397 and 398:
Page 399 and 400:
Page 401 and 402:
Page 403 and 404:
Page 405 and 406:
Page 407 and 408:
Page 409 and 410:
Page 411 and 412:
Page 413 and 414:
Page 415 and 416:
Page 417 and 418:
Page 419 and 420:
Page 421 and 422:
Page 423 and 424:
Page 425 and 426:
Page 427 and 428:
Page 429 and 430:
Page 431 and 432:
Page 433 and 434:
Page 435 and 436:
Page 437 and 438:
Page 439 and 440:
Page 441 and 442:
Page 443 and 444:
Page 445 and 446:
Page 447 and 448:
Page 449 and 450:
Page 451 and 452:
Page 453 and 454:
Page 455 and 456:
Page 457 and 458:
Page 459 and 460:
Page 461 and 462:
Page 463 and 464:
Page 465 and 466:
Page 467 and 468:
Page 469:
Page 476 and 477:
Page 478 and 479:
Page 480 and 481:
Page 482 and 483:
Page 484 and 485:
Page 486 and 487:
Page 488 and 489:
Page 490 and 491:
Page 492 and 493:
Page 494 and 495:
2. Burlaga & Klein method. The main
Page 496 and 497:
Page 498 and 499:
Page 500 and 501:
Page 502 and 503:
Page 504 and 505:
show all

PROBLEMS OF GEOCOSMOS

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?