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101.
J. L. Kohl S. Fineschi R. Esser A. Ciaravella S. R. Cranmer L. D. Gardner R. Suleiman G. Noci A. Modigliani 《Space Science Reviews》1999,87(1-2):233-236
Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI. 相似文献
102.
Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models
of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation
of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending
on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies
with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum
between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is
rapid, even for minor ions like O5+, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This
indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
103.
Balázs Zábori Attila Hirn Pál Bencze 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
The main point of the paper is to use the simultaneous measurements of the energetic particle flux by TriTel and those of electron density by a Langmuir probe to study the question of to what extent solar electromagnetic and corpuscular radiation (galactic cosmic rays, particle precipitation from the radiation belts) are responsible for the ionization of the atmosphere. The electron density measured by the Langmuir probe is the sum of the ionization produced by the solar electromagnetic radiation and that due to the corpuscular radiation. The ionization produced by the solar electromagnetic radiation may be computed. The flux of energetic particles in an energy range may be determined by taking the difference between the threshold energy of the TriTel telescopes and the energy corresponding to the local cut-off rigidity. As the ESEO satellite will have a quasi-polar and circular orbit, the cut-off rigidity will change from low to high latitudes, thus enabling the assignment of different energy bands for the telescopes. Thus, it will be possible to determine which energy bands of particle produce ionization at different latitudes. 相似文献
104.
Richard N. Grugel 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
In view of potential application as a construction material on the lunar surface the mechanical integrity of sulfur concrete was evaluated after being subjected to simulated temperature cycles. Here, small cubes of sulfur concrete were repeatedly cycled between room (20 °C) and liquid nitrogen (−191 °C) temperatures after which they, and non-cycled cubes, were evaluated by compression testing. The compression strength of the non-cycled samples averaged ∼35 MPa (5076 psi) before failing whereas the cycled samples fractured at about 7 MPa (1015 psi). Microscopic examination of the fracture surfaces from the cycled samples showed clear de-bonding of the sulfur from the aggregate whereas it was seen adhering in those non-cycled. Based on a simple analysis it was concluded that the large strength discrepancy between cycled and non-cycled samples is due to differences between the coefficients of thermal expansion of the materials constituting the concrete. 相似文献
105.
106.
107.
介绍了中国新一代宇航试验舱的温控系统。该温控系统设计思想先进、结构新颖。在直径2.3m,长2m的封闭舱体控温面上,实现了0℃~50℃的任意温度定点控制及90min内的正弦波、梯形波、三角波的周期变化;在整个控温面上温度非均匀性(均方根偏差)小于0.3℃,远远超过了非均匀度±1℃、控制精度±2℃的原设计指标。 相似文献
108.
提出了一种建立在TEEN协议基础之上反应式网络的应用.反应式网络是一种对适时性要求较高的网络,用三角定位法对传感器节点进行定位,在定位的基础上,使得簇首节点的选定更为容易,在一定程度上能节省节点能源、延长网络寿命. 相似文献
109.
任爱珍 《北华航天工业学院学报》2007,17(3):54-55
"语言习得"与"语言学习"是外语教学理论研究中的两个重要概念,克拉申认为只有"习得"来的语言才能成为流利的口头表达,而"学习"只能起"监查"作用.在"学习"的条件下,通过营造人为目的语习得环境,以用为本,立足实践,学习者同样可以达到习得外语的目标. 相似文献
110.
S. W. Kahler 《Space Science Reviews》2007,129(4):359-390
Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several
acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks
driven by coronal mass ejections (CMEs) with speeds ≳1000 km s−1. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with
CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the
sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known
several decades ago, but recent observations have presented a more complex picture. We review early and recent observational
results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus
flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from
flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic
proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events;
electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks
are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares.
Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions
for future work are given. 相似文献