標(biāo)題: Titlebook [打印本頁] 作者: bradycardia 時間: 2025-3-21 16:07 作者: Phonophobia 時間: 2025-3-21 22:43 作者: Infantry 時間: 2025-3-22 02:53
,Strong Coupling at Cardona’s Abteilung,stance of 2 10. km, then at distances of 1.2–1.5 10. km, and 5–7 10. km from the nucleus. These phenomena have been observed both on Vega-1 and Vega-2. The electric field measurements are compared with data obtained from dust and plasma experiments; possible mechanisms responsible for the existence of these boundaries are discussed.作者: ovation 時間: 2025-3-22 05:09 作者: 使成波狀 時間: 2025-3-22 11:25 作者: Adrenaline 時間: 2025-3-22 13:38 作者: Adrenaline 時間: 2025-3-22 18:19 作者: scotoma 時間: 2025-3-22 22:50
General features of comet P/Halley: solar wind interaction from plasma measurementsThe Giotto RPA-COPERNIC plasma experiment identified several regions in which the solar wind interaction with the cometary plasma displayed characteristic features:.The detailed plasma features associated with these regions are successively described.作者: BRIDE 時間: 2025-3-23 05:18 作者: GUEER 時間: 2025-3-23 08:12 作者: MOTTO 時間: 2025-3-23 13:37 作者: 聯(lián)想記憶 時間: 2025-3-23 16:34 作者: Limpid 時間: 2025-3-23 20:40 作者: RODE 時間: 2025-3-23 22:17 作者: 先行 時間: 2025-3-24 03:36 作者: Amendment 時間: 2025-3-24 07:49
Sensorische Irritationen (WAS), the behaviour of the solar wind protons through the Giotto inbound shock crossing at comet P/Halley. A foreshock boundary is seen at ~ 1.4 10. km where the level of solar wind fluctuations increases substantially. The shock itself is seen some 2.5 10. km closer. It is a complex structure with high-作者: podiatrist 時間: 2025-3-24 14:09
https://doi.org/10.1007/978-3-642-66362-8alley the IMF showed quite a stable “away” polarity. Draping of magnetic field lines is clearly observed along the outbound leg of the trajectory. Inside the magnetic pile-up region the field reverses its polarity several times. A symmetry of oppositely magnetized sheets with respect to the nucleus 作者: Platelet 時間: 2025-3-24 16:07 作者: mastopexy 時間: 2025-3-24 21:39
https://doi.org/10.1007/978-88-470-5355-7 at times of a generally rather smooth rise or fall of the magnetic field. A maximum MFD magnitude of 40 nT and a maximum duration of 50 s were observed at distances of 50 ÷ 70 10. km. Most likely these events are due to spatial plasma irregularities inside the coma region and not to temporal field 作者: LAVE 時間: 2025-3-25 01:25
https://doi.org/10.1007/978-3-662-60781-7 the following results on the inner plasma boundaries in the magnetoplasma surrounding the comet:.The axis of symmetry had a transverse offset of about 80 000 km from the nucleus..The ionopause must be a tangential discontinuity thereby containing further evidence of the null magnitude of the cavity作者: Lice692 時間: 2025-3-25 03:46 作者: 會犯錯誤 時間: 2025-3-25 08:38 作者: Implicit 時間: 2025-3-25 15:33
https://doi.org/10.1007/978-3-658-28890-7except near the bow shock and that of alpha particle was almost constant (~ 7 cm.) in the cometosheath. Temperature of protons seems to decrease from bow shock to about 2 10. km, and increase thereafter slightly, but that of alpha particle seems to be almost constant. This decrease is likely caused 作者: obstinate 時間: 2025-3-25 18:38 作者: 撕裂皮肉 時間: 2025-3-25 22:29 作者: 建筑師 時間: 2025-3-26 03:23 作者: 反復(fù)無常 時間: 2025-3-26 06:37
New information on comet P/Halley as depicted by Giotto di Bondone and other Western artistsal evidence of comet P/Halley at several passages through that of 1301 and compare it with descriptions and modern images. Since it was first recognized that Giotto di Bondone painted a comet in place of the Star of Bethlehem and suggested that this was a portrait of the 1301 apparition of comet Hal作者: 問到了燒瓶 時間: 2025-3-26 08:59 作者: Observe 時間: 2025-3-26 14:33 作者: Gratulate 時間: 2025-3-26 17:33
Alfvénic turbulence in the solar wind flow during the approach to comet P/Halleyde observations of the proton and alpha particle distributions in the solar wind with 8 seconds time resolution. As the comet was approached, fluctuations were observed in all the primary bulk parameters, i.e. density, temperature and flow velocity, of both distributions at levels above the usual so作者: 莎草 時間: 2025-3-26 22:44 作者: chondromalacia 時間: 2025-3-27 04:17 作者: 截斷 時間: 2025-3-27 05:28 作者: Common-Migraine 時間: 2025-3-27 10:26
Macroscopic perturbations of the IMF by P/Halley as seen by the Giotto magnetometeralley the IMF showed quite a stable “away” polarity. Draping of magnetic field lines is clearly observed along the outbound leg of the trajectory. Inside the magnetic pile-up region the field reverses its polarity several times. A symmetry of oppositely magnetized sheets with respect to the nucleus 作者: 博識 時間: 2025-3-27 17:00 作者: fidelity 時間: 2025-3-27 20:23 作者: 泥沼 時間: 2025-3-28 00:20 作者: Invigorate 時間: 2025-3-28 05:22 作者: 奇怪 時間: 2025-3-28 07:15 作者: enfeeble 時間: 2025-3-28 13:57
Plasma flow in the cometosheath of P/Halley during the encounter of Suiseiexcept near the bow shock and that of alpha particle was almost constant (~ 7 cm.) in the cometosheath. Temperature of protons seems to decrease from bow shock to about 2 10. km, and increase thereafter slightly, but that of alpha particle seems to be almost constant. This decrease is likely caused 作者: 細(xì)菌等 時間: 2025-3-28 15:21 作者: KIN 時間: 2025-3-28 19:28
Plasma-tail activity at the time of the Vega encountersments obtained by the Vega spacecraft. Emphasis is placed on Disconnection Events (DE’s) and on testing the sector boundary/frontside magnetic reconnection model (Niedner and Brandt, 1978) of their origin. Strong support for the model comes from the spectacular DE whose onset, on 1986 March 7–8, is 作者: Paraplegia 時間: 2025-3-29 00:22 作者: 催眠藥 時間: 2025-3-29 05:21 作者: MUTED 時間: 2025-3-29 10:48 作者: 脖子 時間: 2025-3-29 14:58
https://doi.org/10.1007/978-3-642-66362-8ide the magnetic pile-up region the field reverses its polarity several times. A symmetry of oppositely magnetized sheets with respect to the nucleus is found and can be explained in terms of convected IMF features.作者: Rejuvenate 時間: 2025-3-29 18:02
https://doi.org/10.1007/978-88-470-5355-7ed at distances of 50 ÷ 70 10. km. Most likely these events are due to spatial plasma irregularities inside the coma region and not to temporal field variations. The observed effects may be caused by cometary plasma rays.作者: happiness 時間: 2025-3-29 21:06 作者: spondylosis 時間: 2025-3-30 01:00 作者: faculty 時間: 2025-3-30 08:07 作者: GUISE 時間: 2025-3-30 11:20
,Brustwirbels?ule (BWS) und Rippen,ely, and with an IMF sector boundary observed by Vega-1 on March 7.9 UT. Additional work is needed to determine the possible role of solarwind plasma effects in producing the DE. Relationships between other occurrences of plasma-tail activity and Halley Armada spacecraft measurements remain to be explored.作者: nitric-oxide 時間: 2025-3-30 15:47
Encounters with comets: discoveries and puzzles in cometary plasma physicsmation of these structures and boundaries. The paper reviews the observations of these phenomena from spacecraft and the kinetic theories of cometary plasma that were developed recently and that are able to provide a natural explanation of observed puzzling phenomena.作者: Medicaid 時間: 2025-3-30 17:02
Solar wind flow through the comet P/Halley bow shock km. There is evidence for a further excursion back into the cometary ion foot after the initial shock crossing. The cometary ion density is inferred from the solar wind speed changes and is compared with measurements.作者: Alienated 時間: 2025-3-30 21:14
Low-frequency magnetic field fluctuations in comet P/Halley’s magnetosheath: Giotto observationsoard Vega-1 and as expected from quasilinear theory. The entrance into the cometary bow shock is furthermore characterized by an order of magnitude increase of the fluctuation level, both on the in- and outbound pass of Giotto.作者: 有機(jī)體 時間: 2025-3-31 03:36 作者: Mercantile 時間: 2025-3-31 07:02 作者: Eulogy 時間: 2025-3-31 09:23
MHD waves detected by ICE at distances ≥ 28 106 km from comet P/Halley: Cometary or solar wind origiar wind streams, presumably associated with stream-stream interactions. VLF electrostatic emissions are found to occur in field minima or at gradients of the drift mirror structures. Possible generation mechanisms of drift mirror mode waves, cyclotron waves and electrostatic waves are discussed.作者: 有權(quán) 時間: 2025-3-31 13:55 作者: vocation 時間: 2025-3-31 19:34
Manual to Veterinary Video-Oto-Endoscopypropagation for these waves to be separated. The magnetic component is predominantly transverse to the magnetic field and linearly polarised. The flow vector also has a substantial amount of power parallel to the magnetic field. A examination of the pressure variations shows that slow magnetosonic waves are more common than the fast mode.作者: G-spot 時間: 2025-3-31 23:20
https://doi.org/10.1007/978-3-658-28890-7by the cooling effect accompanying with the charge exchange process as well as with the mass addition of cold pickup ions. On the contrary, the observed temperature of alpha particles stayed almost constant throughout the cometosheath. This is because that there is no effective cooling process for alpha particles within the cometosheath.作者: 巧思 時間: 2025-4-1 05:34
übersichtsuntersuchung des K?rperstammes those sampled by Vega and Sakigake, it is important to compare observations from the three missions that carried dedicated wave instruments. Here we summarize ICE plasma wave measurements associated with both comet encounters and relate the very high sensitivity ICE observations to corresponding measurements from the other Halley spacecraft.作者: SAGE 時間: 2025-4-1 07:14
New information on comet P/Halley as depicted by Giotto di Bondone and other Western artistsley (Olson, 1979), a great deal of new information has come to light. We present a synopsis of the textual, visual, and astronomical evidence to support the theory that when Giotto painted his comet in the Scrovegni Chapel he was reflecting his viewing of Comet Halley in 1301.作者: 土坯 時間: 2025-4-1 12:13
Waves in the magnetic field and solar wind flow outside the bow shock at comet P/Halleypropagation for these waves to be separated. The magnetic component is predominantly transverse to the magnetic field and linearly polarised. The flow vector also has a substantial amount of power parallel to the magnetic field. A examination of the pressure variations shows that slow magnetosonic waves are more common than the fast mode.作者: Provenance 時間: 2025-4-1 17:41
Plasma flow in the cometosheath of P/Halley during the encounter of Suiseiby the cooling effect accompanying with the charge exchange process as well as with the mass addition of cold pickup ions. On the contrary, the observed temperature of alpha particles stayed almost constant throughout the cometosheath. This is because that there is no effective cooling process for alpha particles within the cometosheath.作者: gratify 時間: 2025-4-1 19:10 作者: ciliary-body 時間: 2025-4-2 01:26
The pick-up of cometary protons by the solar windoidal trajectories such that they were nonuniformly distributed over a spherical shell in velocity space. The shell radius (relative to its expected radius) and thickness increased as the bow shock was approached. Down-stream of the shock, the cometary protons could not be distinguished from the heated solar wind protons.
