35 research outputs found
Results of experiments for the detection of lunar ionosphere carried out on the first moon's artificial satellite /Luna-10/
Lunik X experiments to detect lunar ionospher
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Noble gases from the interstellar medium trapped on the MIR space station and analyzed by in vacuo etching
Introduction: The composition of the present interstellar medium (ISM) provides an important benchmark in cosmochemistry. It serves as a reference for galactic chemical evolution (GCE) models, solar mixing predictions and provides information for understanding Big Bang nucleosynthesis. The present-day ISM 3He abundance allows, combined with the protosolar 3He, deduced from the Jovian atmosphere or meteorites [1,2], tracing the GCE over the past 4.56 Ga. 3He/4He = (2.5 0.6) x 10-4 has been determined for the local ISM [3]. However, the uncertainty is too large to better constrain GCE models and - in combination with the present-day solar wind value - the protosolar D/H [4]
Geosynchronous magnetic field responses to fast solar wind dynamic pressure enhancements: MHD field model
Intershock observations during STIP intervals 17 and 18
The Prognoz-10/Intercosmos satellite (Intershock Project) carried out observations from Earth orbit from 26 April 1985 until 11 November 1985, covering STIP Intervals XVII and XVIII. Data obtained during the systematic measurements in the course of STIP Interval XVII and part of XVIII are presented; i.e., hourly averages of the solar wind velocity, temperature and ion concentration, ion flux changes (10 to the -1 to 10 to the -3 Hz), plasma wave parameters, energetic particles flux, magnetic fields, etc. Special attention is paid to solar wind distrubances causing abrupt and large effects on the shape of the bow shock (i.e., on 2 May 1985 and 14 September 1985). Generally, the observation period was very close to a minimum of solar activity and was quiet without significant interplanetary shocks
Sharp changes of solar wind ion flux and density within and outside current sheets
Analysis of the Interball-1 spacecraft data (1995-2000) has shown that the
solar wind ion flux sometimes increases or decreases abruptly by more than 20%
over a time period of several seconds or minutes. Typically, the amplitude of
such sharp changes in the solar wind ion flux (SCIFs) is larger than 0.5x10^8
cm^-2 s^-1. These sudden changes of the ion flux were also observed by the
Solar Wind Experiment (SWE), on board the WIND spacecraft, as the solar wind
density increases and decreases with negligible changes in the solar wind
velocity. SCIFs occur irregularly at 1 AU, when plasma flows with specific
properties come to the Earth's orbit. SCIFs are usually observed in slow,
turbulent solar wind with increased density and interplanetary magnetic field
strength. The number of times SCIFs occur during a day is simulated using the
solar wind density, magnetic field, and their standard deviations as input
parameters for a period of 5 years. A correlation coefficient of ~0.7 is
obtained between the modelled and the experimental data. It is found that SCIFs
are not associated with coronal mass ejections (CMEs), corotating interaction
regions (CIRs), or interplanetary shocks; however, 85% of the sector boundaries
are surrounded by SCIFs. The properties of the solar wind plasma for days with
5 or more SCIF observations are the same as those of the solar wind plasma at
the sector boundaries. One possible explanation for the occurrence of SCIFs
(near sector boundaries) is magnetic reconnection at the heliospheric current
sheet or local current sheets. Other probable causes of SCIFs (inside sectors)
are turbulent processes in the slow solar wind and at the crossings of flux
tubes.Comment: 33 pages, 8 figures, 6 tables, Solar Physics 2011, in pres
ΠΠΠΠ‘Π’Π Π£ΠΠ¦ΠΠ― ΠΠΠ’Π§ΠΠΠΠ ΠΠΠ’ΠΠΠΠ ΠΠΠ‘ΠΠΠ§ΠΠ‘ΠΠΠ ΠΠΠΠΠΠ« ΠΠ ΠΠ‘ΠΠΠΠ Π¦ΠΠΠΠΠΠ Π Π€ΠΠ ΠΠΠΠ―
Important tasks of modern space research are the study and continuous observations of the processes of cosmic and meteorological Β«weatherΒ». One of the electronic devices for carrying out such researches is a plasma sensor based on Faraday cup. The purpose of the work was to develop a constructive variant of the Faraday cup with precision sensitive (selective) elements in the form of metal grid microstructures and a four-sector collector, which has no analogues in the world technology.For the formation of grid nickel microstructures, a process has been developed for creating a matrix of nanoporous anodic aluminum oxide by photolithography as a precision shape (template) for depositing nanostructured metal layers. Methods for conducting testing for mechanical (vibrational) and thermocyclic impact that satisfies the requirements for space instruments have been developed.The grid microstructures are formed in a unified technological cycle with the production of ring-holders along the perimeter of the grid, with a square 20 Γ 20 ΞΌm2Β section of the web and square cells with a size of 1 Γ 1 mm2. The transparency of each of the grids was more than 90 % for the normal incidence of light. Dimensions of holders and grid microstructures: internal diameters (34, 47, 60) Β± 0.1 mm, external diameters of rings (42, 55, 68) Β± 0.1 mm, respectively. The weight of one grid was less than 50 mg.The test results demonstrated the operability of the developed grid microstructures with multiple thermocyclic actions from β50 to +150 Β°C and vibrational and static overloads specific for space flights. Instruments for plasma measurements in the near of the Earth and in the interplanetary space will comprise six sensors with different angular orientations. This will make it possible to detect ions of cosmic plasma in a solid angle of about 180Β°.ΠΠ°ΠΆΠ½ΡΠΌΠΈ Π·Π°Π΄Π°ΡΠ°ΠΌΠΈ ΡΠΎΠ²ΡΠ΅ΠΌΠ΅Π½Π½ΡΡ
ΠΊΠΎΡΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠΉ ΡΠ²Π»ΡΡΡΡΡ ΠΈΠ·ΡΡΠ΅Π½ΠΈΠ΅ ΠΈ Π½Π΅ΠΏΡΠ΅ΡΡΠ²Π½ΡΠ΅ Π½Π°Π±Π»ΡΠ΄Π΅Π½ΠΈΡ ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ² ΠΊΠΎΡΠΌΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΈ ΠΌΠ΅ΡΠ΅ΠΎΡΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΎΠΉ Β«ΠΏΠΎΠ³ΠΎΠ΄ΡΒ». ΠΠ΄Π½ΠΈΠΌ ΠΈΠ· ΡΠ»Π΅ΠΊΡΡΠΎΠ½Π½ΡΡ
ΠΏΡΠΈΠ±ΠΎΡΠΎΠ² Π΄Π»Ρ ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ ΡΠ°ΠΊΠΈΡ
ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠΉ ΡΠ²Π»ΡΠ΅ΡΡΡ Π΄Π°ΡΡΠΈΠΊ ΠΏΠ»Π°Π·ΠΌΡ Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ ΡΠΈΠ»ΠΈΠ½Π΄ΡΠ° Π€Π°ΡΠ°Π΄Π΅Ρ. Π¦Π΅Π»Ρ ΡΠ°Π±ΠΎΡΡ ΡΠΎΡΡΠΎΡΠ»Π° Π² ΡΠ°Π·ΡΠ°Π±ΠΎΡΠΊΠ΅ ΠΊΠΎΠ½ΡΡΡΡΠΊΡΠΈΠ²Π½ΠΎΠ³ΠΎ Π²Π°ΡΠΈΠ°Π½ΡΠ° ΡΠΈΠ»ΠΈΠ½Π΄ΡΠ° Π€Π°ΡΠ°Π΄Π΅Ρ Ρ ΠΏΡΠ΅ΡΠΈΠ·ΠΈΠΎΠ½Π½ΡΠΌΠΈ ΡΡΠ²ΡΡΠ²ΠΈΡΠ΅Π»ΡΠ½ΡΠΌΠΈ (ΡΠ΅Π»Π΅ΠΊΡΠΈΡΡΡΡΠΈΠΌΠΈ) ΡΠ»Π΅ΠΌΠ΅Π½ΡΠ°ΠΌΠΈ Π² Π²ΠΈΠ΄Π΅ ΠΌΠ΅ΡΠ°Π»Π»ΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΠ΅ΡΠΎΡΠ½ΡΡ
ΠΌΠΈΠΊΡΠΎΡΡΡΡΠΊΡΡΡ ΠΈ ΡΠ΅ΡΡΡΠ΅Ρ
ΡΠ΅ΠΊΡΠΎΡΠ½ΡΠΌ ΠΊΠΎΠ»Π»Π΅ΠΊΡΠΎΡΠΎΠΌ, Π½Π΅ ΠΈΠΌΠ΅ΡΡΠ΅Π³ΠΎ Π°Π½Π°Π»ΠΎΠ³ΠΎΠ² Π² ΠΌΠΈΡΠΎΠ²ΠΎΠΉ ΡΠ΅Ρ
Π½ΠΈΠΊΠ΅.ΠΠ»Ρ ΡΠΎΡΠΌΠΈΡΠΎΠ²Π°Π½ΠΈΡ ΡΠ΅ΡΠΎΡΠ½ΡΡ
Π½ΠΈΠΊΠ΅Π»Π΅Π²ΡΡ
ΠΌΠΈΠΊΡΠΎΡΡΡΡΠΊΡΡΡ ΡΠ°Π·ΡΠ°Π±ΠΎΡΠ°Π½ ΠΏΡΠΎΡΠ΅ΡΡ ΡΠΎΠ·Π΄Π°Π½ΠΈΡ Ρ ΠΏΠΎΠΌΠΎΡΡΡ ΡΠΎΡΠΎΠ»ΠΈΡΠΎΠ³ΡΠ°ΡΠΈΠΈ ΠΌΠ°ΡΡΠΈΡΡ ΠΈΠ· Π½Π°Π½ΠΎΠΏΠΎΡΠΈΡΡΠΎΠ³ΠΎ Π°Π½ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΠΎΠΊΡΠΈΠ΄Π° Π°Π»ΡΠΌΠΈΠ½ΠΈΡ ΠΊΠ°ΠΊ ΠΏΡΠ΅ΡΠΈΠ·ΠΈΠΎΠ½Π½ΠΎΠΉ ΡΠΎΡΠΌΡ (ΡΠ°Π±Π»ΠΎΠ½Π°) Π΄Π»Ρ ΠΎΡΠ°ΠΆΠ΄Π΅Π½ΠΈΡ Π½Π°Π½ΠΎΡΡΡΡΠΊΡΡΡΠΈΡΠΎΠ²Π°Π½Π½ΡΡ
ΠΌΠ΅ΡΠ°Π»Π»ΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΠ»ΠΎΠ΅Π². Π Π°Π·ΡΠ°Π±ΠΎΡΠ°Π½Ρ ΠΌΠ΅ΡΠΎΠ΄Ρ ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ ΡΠ΅ΡΡΠΎΠ²ΡΡ
ΠΈΡΠΏΡΡΠ°Π½ΠΈΠΉ Π½Π° ΠΌΠ΅Ρ
Π°Π½ΠΈΡΠ΅ΡΠΊΠΈΠ΅ (Π²ΠΈΠ±ΡΠ°ΡΠΈΠΎΠ½Π½ΡΠ΅) ΠΈ ΡΠ΅ΡΠΌΠΎΡΠΈΠΊΠ»ΠΈΡΠ΅ΡΠΊΠΈΠ΅ Π²ΠΎΠ·Π΄Π΅ΠΉΡΡΠ²ΠΈΡ, ΡΠΎΠΎΡΠ²Π΅ΡΡΡΠ²ΡΡΡΠΈΠ΅ ΡΡΠ΅Π±ΠΎΠ²Π°Π½ΠΈΡΠΌ ΠΊ ΠΊΠΎΡΠΌΠΈΡΠ΅ΡΠΊΠΈΠΌ ΠΏΡΠΈΠ±ΠΎΡΠ°ΠΌ.Π‘Π΅ΡΠΎΡΠ½ΡΠ΅ ΠΌΠΈΠΊΡΠΎΡΡΡΡΠΊΡΡΡΡ ΡΡΠΎΡΠΌΠΈΡΠΎΠ²Π°Π½Ρ Π² Π΅Π΄ΠΈΠ½ΠΎΠΌ ΡΠ΅Ρ
Π½ΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΎΠΌ ΡΠΈΠΊΠ»Π΅ Ρ ΠΊΠΎΠ»ΡΡΠ°ΠΌΠΈ-Π΄Π΅ΡΠΆΠ°ΡΠ΅Π»ΡΠΌΠΈ ΠΏΠΎ ΠΏΠ΅ΡΠΈΠΌΠ΅ΡΡΡ ΡΠ΅ΡΠΊΠΈ, Ρ ΠΊΠ²Π°Π΄ΡΠ°ΡΠ½ΡΠΌ 20 Γ 20 ΠΌΠΊΠΌ2Β ΡΠ΅ΡΠ΅Π½ΠΈΠ΅ΠΌ ΠΏΠΎΠ»ΠΎΡΠ½Π° ΠΈ ΡΡΠ΅ΠΉΠΊΠ°ΠΌΠΈ ΡΠ°Π·ΠΌΠ΅ΡΠΎΠΌ 1 Γ 1 ΠΌΠΌ2. ΠΡΠΎΠ·ΡΠ°ΡΠ½ΠΎΡΡΡ ΠΊΠ°ΠΆΠ΄ΠΎΠΉ ΠΈΠ· ΡΠ΅ΡΠΎΠΊ ΠΏΡΠΈ Π½ΠΎΡΠΌΠ°Π»ΡΠ½ΠΎΠΌ ΠΏΠ°Π΄Π΅Π½ΠΈΠΈ ΡΠ²Π΅ΡΠ° ΡΠΎΡΡΠ°Π²ΠΈΠ»Π° Π±ΠΎΠ»Π΅Π΅ 90 %. ΠΠ°Π±Π°ΡΠΈΡΠ½ΡΠ΅ ΡΠ°Π·ΠΌΠ΅ΡΡ Π΄Π΅ΡΠΆΠ°ΡΠ΅Π»Π΅ΠΉ ΠΈ ΡΠ΅ΡΠΎΡΠ½ΡΡ
ΠΌΠΈΠΊΡΠΎΡΡΡΡΠΊΡΡΡ: Π²Π½ΡΡΡΠ΅Π½Π½ΠΈΠ΅ Π΄ΠΈΠ°ΠΌΠ΅ΡΡΡ (34, 47, 60) Β± 0,1 ΠΌΠΌ, Π²Π½Π΅ΡΠ½ΠΈΠ΅ Π΄ΠΈΠ°ΠΌΠ΅ΡΡΡ ΠΊΠΎΠ»Π΅Ρ (42, 55, 68) Β± 0,1 ΠΌΠΌ ΡΠΎΠΎΡΠ²Π΅ΡΡΡΠ²Π΅Π½Π½ΠΎ. ΠΠ°ΡΡΠ° ΠΎΠ΄Π½ΠΎΠΉ ΡΠ΅ΡΠΊΠΈ ΡΠΎΡΡΠ°Π²ΠΈΠ»Π° ΠΌΠ΅Π½Π΅Π΅ 50 ΠΌΠ³.Π Π΅Π·ΡΠ»ΡΡΠ°ΡΡ ΠΈΡΠΏΡΡΠ°Π½ΠΈΠΉ ΠΏΡΠΎΠ΄Π΅ΠΌΠΎΠ½ΡΡΡΠΈΡΠΎΠ²Π°Π»ΠΈ ΡΠ°Π±ΠΎΡΠΎΡΠΏΠΎΡΠΎΠ±Π½ΠΎΡΡΡ ΡΠ°Π·ΡΠ°Π±ΠΎΡΠ°Π½Π½ΡΡ
ΡΠ΅ΡΠΎΡΠ½ΡΡ
ΠΌΠΈΠΊΡΠΎΡΡΡΡΠΊΡΡΡ ΠΏΡΠΈ ΠΌΠ½ΠΎΠ³ΠΎΠΊΡΠ°ΡΠ½ΡΡ
ΡΠ΅ΡΠΌΠΎΡΠΈΠΊΠ»ΠΈΡΠ΅ΡΠΊΠΈΡ
Π²ΠΎΠ·Π΄Π΅ΠΉΡΡΠ²ΠΈΡΡ
ΠΎΡ β50 Π΄ΠΎ +150 Β°Π‘ ΠΈ Π²ΠΈΠ±ΡΠ°ΡΠΈΠΎΠ½Π½ΡΡ
ΠΈ ΡΡΠ°ΡΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΏΠ΅ΡΠ΅Π³ΡΡΠ·ΠΊΠ°Ρ
, Ρ
Π°ΡΠ°ΠΊΡΠ΅ΡΠ½ΡΡ
ΠΏΡΠΈ ΠΊΠΎΡΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΏΠΎΠ»Π΅ΡΠ°Ρ
. Π ΡΠΎΡΡΠ°Π²Π΅ ΠΏΡΠΈΠ±ΠΎΡΠΎΠ² Π΄Π»Ρ ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ ΠΏΠ»Π°Π·ΠΌΠ΅Π½Π½ΡΡ
ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΠΉ Π² ΠΎΠΊΡΠ΅ΡΡΠ½ΠΎΡΡΠΈ ΠΠ΅ΠΌΠ»ΠΈ ΠΈ Π² ΠΌΠ΅ΠΆΠΏΠ»Π°Π½Π΅ΡΠ½ΠΎΠΌ ΠΏΡΠΎΡΡΡΠ°Π½ΡΡΠ²Π΅ Π±ΡΠ΄ΡΡ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½Ρ ΡΠ΅ΡΡΡ Π΄Π°ΡΡΠΈΠΊΠΎΠ² Ρ ΡΠ°Π·Π»ΠΈΡΠ½ΠΎΠΉ ΡΠ³Π»ΠΎΠ²ΠΎΠΉ ΠΎΡΠΈΠ΅Π½ΡΠ°ΡΠΈΠ΅ΠΉ. ΠΡΠΎ ΠΎΠ±Π΅ΡΠΏΠ΅ΡΠΈΡ Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎΡΡΡ ΡΠΈΠΊΡΠΈΡΠΎΠ²Π°Π½ΠΈΡ ΠΈΠΎΠ½ΠΎΠ² ΠΊΠΎΡΠΌΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΏΠ»Π°Π·ΠΌΡ Π² ΡΠ΅Π»Π΅ΡΠ½ΠΎΠΌ ΡΠ³Π»Π΅ ΠΎΠΊΠΎΠ»ΠΎ 180Β°
Solar wind correlations: Statistical and case studies
Recent work on solar wind plasma correlations using data from several widely-separated spacecraft (IMP 8, INTERBALL-I, WIND, and ISEE-3) has shown that, for 6-hour periods, the average plasma correlation is 0.7. The focus of these studies has been directed toward a statistical understanding of gross solar wind correlation behavior. In all correlations examined, lower average correlations are caused by the presence of many points from the low correlation subpopulation; nevertheless, data points from the high correlation population are still present. No single organizational factor has yet been found which adequately separates low-correlation periods from high-correlation periods. Some of the spread in correlations is due to the spatial orientations and dimensions of solar wind structures, and thus to the locatiohal alignments of the spacecraft being correlated, but this does not adequately explain all the good or poor correlations since sometimes three nearby spacecraft show poor correlations, while sometimes three widely-separated spacecraft show good correlations. Thus, in order to understand the underlying physics, detailed investigation of individual cases has been undertaken. These results will be important in assigning quality measures to space weather predictions using satellite measurements taken at L1, for example
Correlation Dependencesdetermined By Simultaneous
Solar wind measurements on board several spacecraft were used to study the two-points correlations of the solar wind plasma structures. The factors having the most influence on the correlation level are the density variability and IMF cone angle. The characteristic length of large solar wind structures is estimated at 500--1000 R E
Geosynchronous magnetic field responses to fast solar wind dynamic pressure enhancements: MHD field model
We performed global MHD simulations of the geosynchronous magnetic
field in response to fast solar wind dynamic pressure (Pd)
enhancements. Taking three Pd enhancement events in 2000 as
examples, we found that the main features of the total field B
and the dominant component Bz can be efficiently predicted by the
MHD model. The predicted B and Bz varies with local time, with
the highest level near noon and a slightly lower level around
mid-night. However, it is more challenging to accurately predict the
responses of the smaller component at the geosynchronous orbit
(i.e., Bx and By). In contrast, the limitations of T01 model
in predicting responses to fast Pd enhancements are presented