The passage of cosmic ray particles and energetic solar particles through interplanetary space is illustrated with a number of idealized examples. The formal examples are worked out from the condition that energetic particles in interplanetary space random walk in the irregularities in the large-scale interplanetary magnetic field. The irregularities move with approximately the velocity of the solar wind. The classical probability distribution is describable by a Fokker-Planck equation. A general expression for the particle diffusion coefficient kij is worked out, including both scattering in magnetic irregularities and systematic pressure drifts. Magnetometer data from Explorer XVIII is presented to show the close average adherence of the quiet-day interplanetary magnetic field to the theoretical spiral angle, and to show the tendency for particles to move more freely along the field than across, k∥ >k⊥. The observed fields show that the diffusion coefficient is of the order of 1021–1022 cm2/sec, as had been estimated from earlier cosmic ray studies. A middle value of 3 × 1021 cm2/sec suggests a cosmic ray density gradient of about 10 per cent per a.u. across the orbit of Earth. Direct observations of the interplanetary magnetic field afford the possibility for quantitative estimate of Kij as a function of particle energy.The first example to be considered is isotropic diffusion in a spherical region r < R with uniform radial wind velocity v for the purpose of illustrating the general nature and duration of the passage of a cosmic ray particle through the solar system. It is shown that the cosmic ray density reduction is of the order of exp (−vR/k), and, hence, that during the years of solar activity vR/k is not less than about 1 for protons of one BeV or so. It follows from this that the galactic cosmic ray particles will generally have spent several days in the solar system by the time they are observed. During this time they are in the expanding magnetic fields carried in the solar wind and are adiabatically decelerated, losing 15 per cent or more of their energy by the time they are observed. The energy distribution is shown for particles starting all with the same energy T0 from interstellar space. The incoming probability wave of a single particle is computed as a function of time, showing how the particle is swept back by the wind.The converse problem of energetic solar particles is illustrated. The solar particles may typically lose half their initial energy before escaping into interstellar space. The outward motion of the wind displaces their probability distribution outward so that ultimately the maximum solar particle intensity may lie beyond the orbit of Earth. The outward motion of the wind steepens the decline of the solar particle intensity.The steady-state cosmic ray intensity is calculated throughout the spherical region r < R supposing a uniform cosmic ray density N0 to obtain in interstellar space. The calculation is carried out for isotropic Kij, which would obtain if the magnetic irregularities were of large amplitude and of a scale not exceeding the radius of gyration of the cosmic ray particles, and for anisotropic kij with k∥ ⪢ k⊥, which obtains when the field is relatively smooth. (The observations at sunspot minimum suggest k∥ ⪢ k⊥ at the orbit of Earth.) The particles diffuse only along the spiral lines of force when k∥ ⪢ k⊥, so their path in and out of the solar system is much longer than when Kij is isotropic. The result is a much greater reduction of the cosmic ray intensity for a given vR/|Kij|.There is no direct observational information on Kij beyond the orbit of Earth, where the intensity reduction takes place. Indirect information is available, however. There is the fact that the intensity of energetic solar particles at Earth often decays as t−g with g = 1·5–2·0. It is shown that in order for this to follow, it is necessary that |Kij| ∞ rs with s = 0·0–0·5 if kij is isotropic, and s = 2·0–2·5 if k∥ ⪢ k⊥. That is to say, if Kij should continue to be as anisotropic beyond Earth as it is observed to be near Earth, then the diffusion must increase rapidly with distance from the Sun. These qualitative features should be easily detectable with particle, field, and plasma observations beyond the orbit of Earth.РефератДaeтcя пoяcHeHиe, coпpoBoздaeмoe pядoм идeaлизиpoBa HHыч пpимepoB, пpoчoдa чacтиц кocмичecкич лyчeй чepeз мeзплaHeтHoe пpocтpaHcтBo. ФopмaльHыe пpимepы paзpaбoтaHы Ha пpeдпoлoзeHии, чтo эHepгeтичe cкиe чacтицы B мeзплaHeтHoм пpocтpaHcтBe блyздaют B HeoдHopoдHocтя ч B пpocтpaHHoм мeзплaHeтHoм мaгHитHoм пoлe. HeoдHopoдHocти пpoдBигaютcя co cкopo cтью пpиблизитeльHoй coлHeчHoмy Beтpy. BepoятHoe клaccичecкoe pacпpeдeлe Hиe мoзeт быть пoдBeдeHo пoд ypaBHeHиe Фoккep-ПлaHкa. paзpaбoтa Ho BыpaзeHиe oбщeгo чapaктepa для кoзффициeHтa Kij. pacceяHия чacтиц, Bкл ючaющee кaк pacceяHиe B мaгHитHыч HeoдHopoдHocтяч, тaк и дpeйфы cиcтeмaтичec кoгo дaBлeHия. Дaютcя мaгHитoмeтpoBыe дaHHыe, пoлyчeHHыe иccлeдoBaтeлeм Чy Ш, чтoбы пoкaзaть Hacкoлькo тecHo—B cpeдHeм—мeзплaHeтHoe мaгHитHoe пo лe, B cпoкoйHый дeиь, coглacyeтcя c тeopeтичecким cпиpaльHым yглoм, a тaкзe yкaзaть Ha тo, чтo чacтицы пpиBычHo пepeдBигaютcя cBoбoдHee Bдoль пoля, Heзeли пoпepeк Heгo, K∥,K⊥. Haблюдaeмыe пoля oбHapyзиBaют, чтo кoэффици eHт pacceяHия пpиHaдлeзит пopядкy B 1021–1022 CM2 ceк, cooтBeтcтByющeмy пpeзHим кaл ькyляцим B изyчeHии кocмичecкич лyчeй. cpeдHee зHaчeHиe B 3 × 1021 CM2 ceк, зacтaBляeт пpeдпoлaгaть, чтo гpaдиeHт плoтHocти кocмичecкич лyч eй пpибл. 10% Ha a.e. пoпepeк opбиты зeмли.HeпocpeдcтBeHHыe HaблюдeHия мeзплaHeтHoгo qmaгHитHoг o пoля пpeдocтaBляют BoзмoзHocть кoличecтBeHHoгo BычиcлeHия Kij, B кaчecт Be фyHкции эHepгии чacтиц. ПepBым пpимepoм, пoдлeзaщим paccмoтpeHию, яBляeтcя из oтpoпHoe pacceяHиe B cфepичecкoй oблacти r < R c paBHoмepHoй paдиaльHoй c кopocтью Beтpa v, и oH дaeтcя B дeляч иллюcтpaции oбщeгo чapaктepa пpoдoлзи тeльHocти пpoчoдa чacтицы кocмичecкoгo лyчa чepeз coлHeчHyю cиcтeмy. yк aзыBaeтcя, чтo плoтHocть кocмичecкич лyчeй coкpaщaeтcя B пopядкe eчp (−vR/K) и ч тo cлeдoBaтeльHo B гoды coлHeчHoй aктиBHocти vR>/K He мeHee чeм пpибл. 1 д ля пpoтoHoB oдHoгo Be V, или oкoлo этoгo. Из этoгo cлeдyeт, чтo гaлaктичecкиe чa cтицы кocмичecкич лyчeй, кo BpeмeHи HaблюдeHия ич, yзe oбычHo пpoBeли Hecкoлькo дHeй B coлHeчHoй cиcтeмe. B тeчeHиe этoгo пepиoдa oHи Haчoдятcя B pacши pяющичcя мaгHитHыч пoляч, Hecoмыe coлHeчHым Beтpoм, c aдиaбaтичecки зaмeд лeHHoй cкopocтью, yтpaчиBaя 15 или бoлee пpoцeHтoB cBoeй эHepгии к тoмy Bp eмeHи, чтo oHи пoдBepгaютcя HaблyдeHиям. pacпpeдeлeHиe эHepгии yкaзaHo длH чacти ц c oдиHaкoBoй иcчoдHoй зHepгиeй T0 oт мeззBeздHoгo пpocтpaHcтBa. H acтyпaющaя BepoятHaя BoлHa eдиHoй чacтицы иcчиcляeтcя B кaчecтBe фyHкции B peмeHи, yкaзыBaя кaк чacтицa oтHocитcя Beтpoм.Дaeтcя иллюcтpaция oбpaтHoй пpoблeмы эHHpгeтичecкич coлHeчHыч чacтиц. coлHeчHыe чacтицы мoгyт чapaктepHым oбpaзoм yтepять 50% cBoeй пepBoHaчaльHoй эHepгии дo тoгo, кaк ycкoльзHyть B мeззBeздHoe пpocтpa HcтBo. ДBизeHиe Beтpa, HaпpaBлeHHoe Hapyзy, пepeмeщaeт ич BepoятHoe pa cпpeдeлeHиe Hapyзy тaким oбpaзoм, чтo B кoHeчHoм cчeтe мaкcимaльHaя иHтeH cиBиocть coлHeчHoй чacтицы мoзeт Haчoдитьcя зa пpeдeлaми opбиты зeмли. Ha пpaBлeHHoe Hapyзy дBизeHиe Beтpa ycкopяeт пoHизeHиe иHтeHcиBHocти coлH eчHoй чacтицы. ycтoйчиBoe cocтoяHиe иHтeHcиBHocти кocмичecкич лyчe й Bычиcляeтcя пo Bceй cфepичecкoй oблacти r < R пpи ycлopии paBHoмepHocти плoтHocти No кocмичecкич лyчeй, пoлyчaeмoй B мeззBeздHoм пpocтpaHcтBe. pacчeт пpoизBoдитcя для изoтpoпHoгo Kij и oH пoлyчaeтcя пpи ycлoBии, чтo мaгHи тHыe HeoдHopoдHocти бoльшoй aмплитyды и мacштaбoм HeпpeBышaющим paдиyc B paщeHия чacтиц кocмичecкич лyчeй, a тaкзe для aHизoтpoпHoгo Kij, пpи K∥ ⪢ K⊥, пoлyчaeмoгo, кoгдa пoлe oтHocитeльHo cпoкoиHo. (HaблюдeHия пpи миHи мyмe coлиeчHыч пятeH зacтaBлHют пpeдпoлaгaть, чтo K∥ ⪢ K⊥ Haчoдитcя y o pбиты зeмли.) чacтицы pacceиBayтcя лишь Bдoль cпиpaльHыч лиHий cилы, кoгдa K∥ ⪢ K⊥ и тaким oбpaзoм ич пyть B и из coлHeчHoй cиcтeмы гopaздo длиHee, чeм B т oм cлyчae, кoгдa Kij изoтpoпHo. B paзyльтaтe, иHтeHcиBHocть кocмичecкич лy чeй пoHизaeтcя гopaздo бoльшe для дaHHoгo vR/kij.oтHocитeльHo Kij He имeeтcя HeпocpeдcтBeHHoй oбcepB aциoHHoй иHфopмaции зa пpeдeлoм opбиты зeмли, гдe пpoиcчoдит пoHизeHиe иHтeH cиBHocти. oдHaкo, B pacпopязeHии имeeтcя кocBeHHaя иHфopмaция, кaк тoт фa кт, чтo иHтeHcиBHocть эHepгeтичecкич coлHeчHыч чacтиц Hepeдкo зaтyчaeт, кa к t−g, пpи g = 1,5 – 2,0. yкaзыBaeтcя, чтo для тoгo, чтoбы зтo cлyчилocь, Heoбчoд имo, чтoбы |Kij| αrs пpи S = 0,0 – 0,5, ecли Kij изoтpoпHo, пpoдoлзaлo быть тaк зe aHи зoтpoпHo зa пpeдeлoм зeмли, кaк oHo Haблюдaлocь Bблизи зeмли, и тoг дa pacceяHиe дoлзHo быcтpo yBeличиBaтьcя c paccтoяHиeм oт coлHцa. Эти кoли чecтBeHHыe чapaктepиcтики мoгyт быть лeгкo oбHapyзeHы пpи HaблюдeHияч чacтиц, пo лeй и плaзмы зa пpeдeлoм opбиты зeмли.