共查询到20条相似文献,搜索用时 31 毫秒
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WenBin Shen Jinsheng Ning Dingbo Chao Jinnan Liu 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
We propose a test of the gravitational time dilation in general relativity by long term clock comparison between two stations separated in height. The geopotential difference between the two National time keeping centers in China, Lintong (A) and Beijing (B) is around 4000 geopotential unit, which corresponds to the height difference of 400 m. Two clocks CA and CB are fixed at stations A and B, respectively, which are synchronized at beginning by a portable clock C in a short time period with go-back synchronization approach. After one month, the clock C is again transported between A and B , comparing the records of the keeping time by clocks CA and CB, respectively. Calculations show that, after one month, the difference of the time durations between the clocks CA and CB is around 121 ns, if general relativity is correct. 相似文献
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Maria S. Pulinets Elizaveta E. Antonova Maria O. Riazantseva Svetlana S. Znatkova Igor P. Kirpichev 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
Crossings of the magnetopause near the subsolar point are analyzed using data of THEMIS mission. Variations of the magnetic field near magnetopause measured by one of THEMIS satellites are studied and compared with simultaneous measurements in the solar wind by another THEMIS satellite. The time delay of the solar wind arrival at the subsolar point of the magnetopause is taken into account. 30 and 90 s averaging of the magnetic field in the magnetosheath is produced. The results of averaging are compared with the results of measurements in the solar wind before the bow shock and foreshock. It is shown, that Bx component of the magnetic field near magnetopause is near to zero, which supports the possibility to consider the magnetopause as the tangential discontinuity. Comparatively good correlation of By component in the solar wind and near the magnetopause is observed. The correlation of Bz component near the magnetopause and IMF is practically absent, the sign of the Bz near the subsolar point does not coincide with the sign of IMF Bz in ∼30% cases. 相似文献
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L.H. Chao W.H. Bian K.L. Huang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
Using the bulge data from AGN image decomposition with ground-based observations, we calculate the ratios of the central supermassive black hole mass(SMBH) to the Bulge mass (Mbh/Mbulge) in a sample of X-ray selected AGNs, including 15 Narrow-line Seyfert 1 galaxies (NLS1s) and 18 broad-line Seyfert 1 galaxies (BLS1s). We found that the mean value of log(Mbh/Mbulge) is -3.81±0.11 for 15 NLS1s, and -2.91±0.13 for 18 BLS1s, showing the lower Mbh/Mbulge in NLS1s relative to BLS1s. The calculation shows that the Bulge mass from the host image decomposition in NLS1s is statistically smaller than that from Hubble-type correction method, and a linear mass relation is suggested for NLS1s and a nonlinear mass relation for BLS1s. The studying of host galaxies with ground-based observations strongly limited by the atmospheric seeing. We need to do the decomposition of host images for NLS1s with Hubble Space Telescope observation in the future. 相似文献
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F.J.T. Salazar J.J. Masdemont G. Gómez E.E. Macau O.C. Winter 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
Assume a constellation of satellites is flying near a given nominal trajectory around L4 or L5 in the Earth–Moon system in such a way that there is some freedom in the selection of the geometry of the constellation. We are interested in avoiding large variations of the mutual distances between spacecraft. In this case, the existence of regions of zero and minimum relative radial acceleration with respect to the nominal trajectory will prevent from the expansion or contraction of the constellation. In the other case, the existence of regions of maximum relative radial acceleration with respect to the nominal trajectory will produce a larger expansion and contraction of the constellation. The goal of this paper is to study these regions in the scenario of the Circular Restricted Three Body Problem by means of a linearization of the equations of motion relative to the periodic orbits around L4 or L5. This study corresponds to a preliminar planar formation flight dynamics about triangular libration points in the Earth–Moon system. Additionally, the cost estimate to maintain the constellation in the regions of zero and minimum relative radial acceleration or keeping a rigid configuration is computed with the use of the residual acceleration concept. At the end, the results are compared with the dynamical behavior of the deviation of the constellation from a periodic orbit. 相似文献
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Huynh Anh Nguyen Le Soojong Pak Myungshin Im Minjin Kim Chae Kyung Sim Luis C. Ho 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
We present medium resolution near-infrared host galaxy spectra of low redshift quasars, PG 0844+349 (z = 0.064), PG 1226+023 (z = 0.158), and PG 1426+015 (z = 0.086). The observations were done by using the Infrared Camera and Spectrograph (IRCS) at the Subaru 8.2 m telescope. The full width at half maximum of the point spread function was about 0.3 arcsec by operations of an adaptive optics system, which can effectively resolve the quasar spectra from the host galaxy spectra. We spent up to several hours per target and developed data reduction methods to reduce the systematic noises of the telluric emissions and absorptions. From the obtained spectra, we identified absorption features of Mg I (1.503 μm), Si I (1.589 μm) and CO (6-3) (1.619 μm), and measured the velocity dispersions of PG 0844+349 to be 132 ± 110 km s−1 and PG 1426+015 to be 264 ± 215 km s−1. By using an MBH–σ relation of elliptical galaxies, we derived the black hole (BH) mass of PG 0844+349, log(MBH/M⊙)=7.7±5.5 and PG 1426+015,log(MBH/M⊙)=9.0±7.5. These values are consistent with the BH mass values from broad emission lines with an assumption of a virial factor of 5.5. 相似文献
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A.P. Kropotkin V.I. Domrin 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
Dynamics of the magnetotail involves elementary processes of magnetic field merging (reconnection layer formation) occurring on medium spatial scales. Every such process features two different stages, a fast one and a subsequent slower one. The corresponding short time scale T1 is associated with disturbances propagating in the tail lobes. The longer time scale T2 is associated with plasma motions in the plasma sheet. A disturbance appearing in the magnetotail on the time scale T1 results in a loss of equilibrium in the plasma sheet. By means of theoretical argument and numerical simulation, it is shown that the relaxation process which follows on the time scale T2, produces extremely thin embedded current sheets, along with generation of fast plasma flows. The process provides an effective mechanism for transformation of magnetic energy accumulated in the magnetotail, into energy of plasma flows. The fast flows may drive turbulent motions on shorter spatial scales. In their turn, those motions can locally produce very thin current sheets; after that, nonlinear tearing process leads to generation of neutral lines, and reconnection. The latter produces new fast disturbances on the time scale T1 closing the feedback loop. 相似文献
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C. Alenka Negrete Deborah Dultzin Paola Marziani Jack W. Sulentic 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
We describe an alternate way to estimate Broad Line Region (BLR) radii for type-1 AGN based on determination of physical conditions in the BLR under the assumption that the line emitting gas is photoionized by a central continuum source. We derive “diagnostic” intensity ratios involving UV lines Aliiiλ1860, Siiii]λ1892 and Civλ1549 which enable us to compute the ionizing photon flux, and hence BLR radius from the ionization parameter definition. We compare our estimates of BLR radii with values independently obtained from reverberation monitoring of Hβ and, in a few cases, of C ivλ1549. We analyze the interpretation of the photoionization estimates in the 4D eigenvector 1 context, and discuss in some detail the case of 3C 390.3. For this object we are able to provide not only the ionizing photon flux, but also an estimate of density and ionization parameter from the measured diagnostic ratios. We also compare black hole masses obtained from this method with values derived from widely-applied correlations between mass, line broadening and luminosity. Good agreement is found for both radius and black hole mass comparisons. 相似文献
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Holger Winkler Justus Notholt 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
An ion chemistry model is used to investigate the negative chlorine ion chemistry of the mesosphere for quiet ionospheric conditions. Model results are presented for high latitudes in February as well as for the equator in Summer. For nighttime, Cl-, Cl-(HCl), and NO3−(HCl) are the most abundant chlorine anions in the mesosphere. The concentration of ClO3− depends significantly on its stability against collision-induced dissociation. In contrast to previous model predictions, the abundance of Cl-(H2O) is small. For daytime, photoelectron detachment and photodissociation have pronounced impact on the negative chlorine ion chemistry in the mesosphere. The abundance of all anion cluster is considerably smaller than at night. While Cl- decreases in the upper mesosphere, its abundance increases at lower altitudes. 相似文献
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Manuel Arriagada Carolina Cipagauta Alberto Foppiano 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
A simple semi-empirical model to determine the maximum electron concentration in the ionosphere (NmF2) for South American locations is used to calculate NmF2 for a northern hemisphere station in the same longitude sector. NmF2 is determined as the sum of two terms, one related to photochemical and diffusive processes and the other one to transport mechanisms. The model gives diurnal variations of NmF2 representative for winter, summer and equinox conditions, during intervals of high and low solar activity. Model NmF2 results are compared with ionosonde observations made at Toluca-México (19.3°N; 260°E). Differences between model results and observations are similar to those corresponding to comparisons with South American observations. It seems that further improvement of the model could be made by refining the latitude dependencies of coefficients used for the transport term. 相似文献
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Emirant Bertillas Amabayo Jurua Edward Pierre J. Cilliers John Bosco Habarulema 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
This study presents results on the investigation of the diurnal, monthly and seasonal variability of Total Electron Content (TEC), phase (σΦ) and amplitude (S4) scintillation indices over Ugandan (Low latitude) region. Scintillation Network Decision Aid (SCINDA) data was obtained from Makerere (0.34°N, 32.57°E) station, Uganda for two years (2011 and 2012). Data from two dual frequency GPS receivers at Mbarara (0.60°S, 30.74°E) and Entebbe (0.04°N, 32.44°E) was used to study TEC climatology during the same period of scintillation study. The results show that peak TEC values were recorded during the months of October–November, and the lowest values during the months of July–August. The diurnal peak of TEC occurs between 10:00 and 14:00 UT hours. Seasonally, the ascending and descending phases of TEC were observed during the equinoxes (March and September) and solstice (June and December), respectively. The scintillations observed during the study were classified as weak (0.1≤S4,σΦ≤0.3) and strong (0.3<S4,σΦ≤1.0). The diurnal scintillation pattern showed peaks between 17:00 and 22:00 UT hour, while the seasonal pattern follows the TEC pattern mentioned above. Amplitude scintillation was more dominant than phase scintillation during the two years of the study. Scintillation peaks occur during the months of March–April and September–October, while the least scintillations occur during the months of June–July. Therefore, the contribution of this study is filling the gap in the current documentation of amplitude scintillation without phase scintillation over the Ugandan region. The scintillations observed have been attributed to wave-like structures which have periods of about 2–3 h, in the range of that of large scale travelling ionospheric disturbances (LSTIDs). 相似文献