Muon density measurements with the KASCADE central detector     

《Astroparticle Physics》2002,16(4):183-386

Frequency distributions of local muon densities in high-energy extensive air showers (EAS) are presented as signature of the primary cosmic ray energy spectrum in the knee region. Together with the gross shower variables like shower core position, angle of incidence, and the shower sizes, the KASCADE experiment is able to measure local muon densities for two different muon energy thresholds. The spectra have been reconstructed for various core distances, as well as for particular subsamples, classified on the basis of the shower size ratio N_μ/N_e. The measured density spectra of the total sample exhibit clear kinks reflecting the knee of the primary energy spectrum. While relatively sharp changes of the slopes are observed in the spectrum of EAS with small values of the shower size ratio, no such feature is detected at EAS of large N_μ/N_e ratio in the energy range of 1–10 PeV. Comparing the spectra for various thresholds and core distances with detailed Monte Carlo simulations the validity of EAS simulations is discussed.  相似文献   

流星暴的航天定义     

马月华  徐品新  李广宇  包纲 《天文学报》2005,46(2):158-164

定义ZHR^*以每小时穿过1000平方公里天顶截面的，能在铝质表面打出直径不小于1厘米的弹坑的流星体数，作为流星群对航天安全威胁强度的定量标志，给出了从ZHR到ZHR^*的换算公式．用ZHR^*取代ZHR来评价20世纪90年代以来的一些强流星雨，发现1998年的贾可比尼(天龙座)流星雨对航天安全来说，是比公认的1999、2001、2002年3次狮子座流星暴强数倍的更强流星暴．  相似文献   

PREDICTING MARTIAN AND VENUSIAN METEOR SHOWER ACTIVITY     

Apostolos A. Christou 《Earth, Moon, and Planets》2004,95(1-4):425-431

Based on the number of planet-approaching cometary orbits at Mars and Venus relative to the Earth, there should be ample opportunities for observing meteor activity at those two planets. The ratio of planet-approaching Jupiter family comets (JFCs) at Mars, Earth, and Venus is 4:2:1 indicating that JFC-related outbursts would be more frequent at Mars than the Earth. The relative numbers of planet-approaching Halley-type comets (HTCs) implies that the respective levels of annual meteor activity at those three planets are similar. We identify several instances where near-comet outbursts (Jenniskens, P.: 1995, Astron. Astrophys. 295, 206–235) may occur. A possible double outburst of this type at Venus related to 45P/Honda-Mrkos-Padjusakova may be observable by the ESA Venus Express spacecraft in the summer of 2006. Similarly, the Japanese Planet-C Venus orbiter may observe an outburst related to 27P/Crommelin’s perihelion passage in July 2011. Several additional opportunities exist to observe such outbursts at Mars from 2019 to 2026 associated with comets 38P/Stephan-Oterma, 13P/Olbers and 114P/Wiseman-Skiff.  相似文献   

Evolution of short period meteoroid streams     

P. B. Babadzhanov  Yu. V. Obrubov 《Celestial Mechanics and Dynamical Astronomy》1992,54(1-3):111-127

The dynamical evolution of meteoroid streams associated with cornets Encke, Halley, Machholz 1986 VIII and asteroid Phaethon is discussed. It is shown that the planetary perturbations can greatly increase the streams thickness and each stream may produce several couples of meteor showers active in different seasons of the year. The theoretical and observed data are in a satisfactory accordance.  相似文献   

A note on the determination of ozone concentrations from radio-meteor duration distributions.     

J. Jones  M. Simek 《Earth, Moon, and Planets》1995,68(1-3):329-338

Hajduk, et al (1992) have drawn attention to a possible source of error in our earlier analysis of visual and radar observations of shower meteors from which we calculated the ozone concentration at meteor heights. We have considered their main criticism that the features of our data which we used to calculate the ozone concentration may have been due to the constraint that our meteors had to be observed by both methods. We have shown that observations collected from radar-only systems show very similar characteristics and that these can be analysed without recourse to visual data to produce very similar results to those from our original analysis. Presented at theInternational Conference on Meteoroids 23 – 31 August 1994 in Bratislava.Submitted to Earth, Moon and Planets  相似文献   

Statistics on the vertical structure of rainshowers     

R. R. Rogers  K. J. Keen  M. Blaskovic 《Pure and Applied Geophysics》1983,121(1):167-184

A large sample of summertime data from the McGill Radar Weather Observatory was analyzed to determine the variation with altitude of the horizontal extent of individual rainshowers. For echoes defined by a reflectivity factor of 39 dBz (equivalent to a rainfall rate of about 10 mm/h) it was found that the mean area of the total population of echoes decreases linearly with altitude from approximately 20 km² at 2 km to 11 km² at 8 km. Subsets of the total population were investigated, consisting of only the echoes penetrating the altitudes of 6, 7, and 8 km. On the average these relatively tall echoes are much greater in horizontal extent than the total population. Whereas the sizes of the total population of echoes at any altitude are distributed approximately exponentially in terms of the square root of area, the sizes of the “survivors” that extend to high altitudes may be described by the gamma distribution with a mean value decreasing approximately linearly with height above 3 km and a dispersion of 0.55. Some characteristics are also reported for echoes defined by reflectivities of 31 dBz and 47 dBz. Estimates are given of the fraction of the total area in a horizontal plane that contains echoes in each of these categories.  相似文献   

Distributions of secondary muons at sea level from cosmic gamma rays below 10 TeV     

J. Poirier  S. Roesler  A. Fass 《Astroparticle Physics》2002,17(4):1247-458

The Monte Carlo program is used to predict the distributions of the muons which originate from primary cosmic gamma rays and reach sea level. The main result is the angular distribution of muons produced by vertical gamma rays which is necessary to predict the inherent angular resolution of any instrument utilizing muons to infer properties of gamma ray primaries. Furthermore, various physical effects are discussed which affect these distributions in differing proportions.  相似文献   

Multi-station electro-optical observations of the 1999 Leonid meteor storm     

P. Brown  M.D. CampbellR.L. Hawkes  C. TheijsmeijerJ. Jones 《Planetary and Space Science》2002,50(1):45-55

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Visual Observations Of The Leonid Meteors 1998 In Yunnan     

Wu  Guang-jie  Zhang  Zhou-sheng 《Earth, Moon, and Planets》1998,81(3):193-200

The 1998 Leonid meteor shower was observed at the Gaomeigu station of Yunnan Observatory during five successive days in November. The visual records indicate that the number of meteors increased suddenly, from a ZHR of about 140 to over 400, in the early morning of November 17th, Beijing time. But it decreased slowly in the following two days. During the maximum there was a high proportion – about 10 percent – of very bright fireballs with enduring trains. The brightest one was about -10 magnitude with a smoke train fading about three minutes after. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

RADAR MEASUREMENTS OF MACRO FRAGMENTATION IN METEOROIDS     

W. J. BAGGALEY  J. GRANT 《Earth, Moon, and Planets》2004,95(1-4):655-662

Fragmentation of an ablating meteoroid is a process that depends on the physical constitution of the body and the internal structure. These parameters are thought to control temperature gradients within the body. Phase signatures from the University of Canterbury’s AMOR facility are shown to be able to resolve instances in which meteors are subject to gross macro-fragmentation where the meteoroid body disrupts into a few discrete components.  相似文献