排序方式: 共有102条查询结果,搜索用时 15 毫秒
1.
Karl-Heinz Glassmeier Ingo Richter Andrea Diedrich Günter Musmann Uli Auster Uwe Motschmann Andre Balogh Chris Carr Emanuele Cupido Andrew Coates Martin Rother Konrad Schwingenschuh Karoly Szegö Bruce Tsurutani 《Space Science Reviews》2007,128(1-4):649-670
The fluxgate magnetometer experiment onboard the ROSETTA spacecraft aims to measure the magnetic field in the interaction
region of the solar wind plasma with comet 67P/Churyumov-Gerasimenko. It consists of a system of two ultra light (about 28
g each ) triaxial fluxgate magnetometer sensors, mounted on the 1.5 m long spacecraft boom. The measurement range of each
sensor is ±16384 nT with quantization steps of 31 pT. The magnetometer sensors are operated with a time resolution of up to
0.05 s, corresponding to a bandwidth of 0–10 Hz. This performance of the RPC-MAG sensors allows detailed analyses of magnetic
field variations in the cometary environment. RPC-MAG furthermore is designed to study possible remnant magnetic fields of
the nucleus, measurements which will be done in close cooperation with the ROSETTA lander magnetometer experiment ROMAP. 相似文献
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3.
近地磁尾准无碰撞磁重联事件 总被引:2,自引:2,他引:2
综合分析了ClusterⅡ-C1飞船在2001年9月15日飞越地球磁尾等离子体片区的热离子和磁场观测资料。结果表明,约在0340-0440UT时间期间,资料多次呈现出较强的尾向离子流(VXGSM<0),明显的南向磁场分量(BZGSM<0),以及明显的晨-昏向磁场分量BYGSM等特征。由此可以推断,在磁尾等离子体片中,在径向方向XGSE>-18.6Re范围内,可能发生了多次磁重联事件,整个事件持续期约1h。磁重联事件的观测特征与准无(或半)碰撞磁重联理论的基本图像符合一致,因此这些事件应当是准无碰撞磁重联事件。 相似文献
4.
E. J. Smith M. Neugebauer A. Balogh S. J. Bame R. P. Lepping B. T. Tsurutani 《Space Science Reviews》1995,72(1-2):165-170
The radial component of the magnetic field at Ulysses, over latitudes from –10° to –45° and distances from 5.3 to 3.8 AU, compares very well with corresponding measurements being made by IMP-8 in the ecliptic at 1AU. There is little, if any, evidence of a latitude gradient. Variances in the field, normalized to the square of the field magnitude, show little change with latitude in variations in the magnitude but a large increase in the transverse field variations. The latter are shown to be caused by the presence of large amplitude, long period Alfvénic fluctuations. This identification is based on the close relation between the magnetic field and velocity perturbations including the effect of anisotropy in the solar wind pressure. The waves are propagating outward from the Sun, as in the ecliptic, but variance analysis indicates that the direction of propagation is radial rather than field-aligned. A significant long-period component of 10 hours is present. 相似文献
5.
We report the discovery that for latitudes above 40°S, the observed recurring modulation of cosmic rays and anomalous nuclei occurs without the detection byUlysses of the solar wind velocity and magnetic field recurring enhancements that have, heretofore at lower latitudes, defined corotating interaction regions—i.e., the mechanism producing the recurring intensity variations >40°S appears to be located beyond the radial range ofUlysses. 相似文献
6.
A. Balogh J. A. Gonzalez-Esparza R. J. Forsyth M. E. Burton B. E. Goldstein E. J. Smith S. J. Bame 《Space Science Reviews》1995,72(1-2):171-180
Between its launch in October 1990 and the end of 1993, approximately 160 fast collisionless shock waves were observed in the solar wind by the Ulysses space probe. During the in-ecliptic part of the mission, to February 1992, the observed shock waves were first caused mainly by solar transient events following the solar maximum and the reorganisation of the large scale coronal fields. With the decay in solar activity, relatively stable Corotating Interaction Regions (CIRs) were observed betwen 3 and 5.4 AU, each associated with at least one forwardreverse shock pair. During the out-of-ecliptic phase of the orbit, from February 1992 onwards, CIRs and shock pairs associated with them continued to dominate the observations. From July 1992, Ulysses encountered the fast solar wind flow from the newly developed southern polar coronal hole, and from May 1993 remained in the unipolar magnetic region associated with this coronal hole. At latitudes beyond 30°, CIRs were associated almost exclusively with reverse shocks only. A comprehensive list of shock waves identified in the magnetic field and solar wind plasma data from Ulysses is given in Table 1. The principal characteristics were determined mainly from the magnetic field data. General considerations concerning the determination of shock characteristics are outlined in the Introduction. 相似文献
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8.
We study the solar cycle, radial, and latitudinal dependence of the characteristics of magnetic field irregularities in the
Heliosphere. The frequency of magnetic field discontinuities is determined, using high time resolution magnetic field observations
by Ulysses, covering the time interval from 1992 to 2000. The quasi-linear scattering mean free path of particles is also calculated.
These investigations aim at understanding/exploring transport properties of energetic charged particles in the Heliosphere.
We find that the travel time of solar wind plasma from the Sun to the observer is the key parameter of the process, by controling
the decay of the irregularities.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
9.
At solar maximum, the large-scale structure of the heliospheric magnetic field (HMF) reflects the complexity of the Sun's
coronal magnetic fields. The corona is characterised by mostly closed magnetic structures and short-lived, small coronal holes.
The axis of the Sun's dipole field is close to the solar equator; there are also important contributions from the higher order
terms. This complex and variable coronal magnetic configuration leads to a much increased variability in the HMF on all time
scales, at all latitudes. The transition from solar minimum to solar maximum conditions, as reflected in the HMF, is described,
as observed by Ulysses during its passage to high southern heliolatitudes. The magnetic signatures associated with the interaction regions generated
by short-lived fast solar wind streams are presented, together with the highly disordered period in mid-1999 when there was
a considerable reorganisation in coronal structures. The magnetic sector structure at high heliolatitudes shows, from mid-1999,
a recognisable two-sector structure, corresponding to a highly inclined Heliospheric Current Sheet. A preliminary investigation
of the radial component of the magnetic field indicates that it remains, on average, constant as a function of heliolatitude.
Intervals of highly Alfvénic fluctuations in the rarefaction regions trailing the interaction regions have been, even if intermittently,
identified even close to solar maximum.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
10.
André Balogh Réjean Grard Sean C. Solomon Rita Schulz Yves Langevin Yasumasa Kasaba Masaki Fujimoto 《Space Science Reviews》2007,132(2-4):611-645
Mercury is a very difficult planet to observe from the Earth, and space missions that target Mercury are essential for a comprehensive
understanding of the planet. At the same time, it is also difficult to orbit because it is deep inside the Sun’s gravitational
well. Only one mission has visited Mercury; that was Mariner 10 in the 1970s. This paper provides a brief history of Mariner
10 and the numerous imaginative but unsuccessful mission proposals since the 1970s for another Mercury mission. In the late
1990s, two missions—MESSENGER and BepiColombo—received the go-ahead; MESSENGER is on its way to its first encounter with Mercury
in January 2008. The history, scientific objectives, mission designs, and payloads of both these missions are described in
detail. 相似文献