共查询到19条相似文献，搜索用时 140 毫秒
1.
哈雷彗星在日彗距较大时出现长而直的主彗尾（尾流），这是很有趣的。尾流一般是指等离子体尾流；但是，当地球接近彗星轨道面时，尘埃尾流可能叠加到主彗尾上。在一般感光波段宽的彗星底片上很难区分这两种尾流。本文选取哈雷彗星在不同日彗距的5条主尾流，作了光度测量和比较分析。得出沿各尾轴及其垂直方向几个截面的亮度分布、亮度半极大全宽、尾轴的视风差角和真风差角及彗尾长度。在所分析的蓝敏底片上，过近日点前的2个尾流肯定是等离子体尾流，而5个尾流的相似性以及其他证据说明它们主要都是等离子体尾流，尘埃彗尾的污染是次要的。 相似文献
2.
哈雷彗星1984年9月到1986年4月的观测期,对彗星科学研究来说是一次极好的机会。在此期间,人类第一次用现代科学技术记录下彗发形成和消失的整个过程。 在哈雷彗星接近太阳和地球时,天文学家观测 相似文献
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5月6日室瓶座η流星雨极盛宝瓶座η流星雨是与哈雷彗星有关的流星雨。哈雷彗星在运行到太阳附近时在其运行轨道上撒落大量流星体粒子。宝瓶座η流星群是哈雷彗星的流星群中的一个,每年4月下旬到5月下旬期间,宝瓶座流星群粒子进入地球大气 相似文献
4.
第一次观看哈雷彗星追记１９８５年１０月２８日，对我来说，是一个值得纪念的日子。这一天过去快十年了，但那天晚上的一切，我还记忆犹新。那年暑假参加省天文夏令营时，我就得知了一些关于哈雷彗星的信息，得以及时汇款邮购了《哈雷彗星观测手册》；开学后，我又作了一... 相似文献
5.
哈雷彗星的轨道演变的趋势和它的古代历史 总被引：4，自引：1，他引：3
本文讨论了哈雷彗星三千多年中轨道演变的趋势。所根据的资料是利用TQ-6型电子计算机,计及大行星摄动而求得的在这三千多年中的运动轨道。本文的中心内容是将我国历史上各次可能是哈雷彗星的纪录,加以分析考证,以断定其是否果属哈雷彗星。对于几个有关年代学的问题,也提供了解决的线索。 相似文献
6.
王益萍 《紫金山天文台台刊》1996,15(1):24-30
本文介绍了国际哈雷彗星联测组织收集并整理发行的25张哈雷彗星光盘资料库。着重说明了它的内容、资料库结构以及资料的查询和使用方法。 相似文献
7.
风靡全球的世纪大明星────哈雷彗星彗星是浪迹太阳系的漂泊者，有的穿梭于行星之间，以极短的周期围绕太阳运动，有的则从行星领域的最远处直奔太阳而来，随即扬长而去。谈到彗星，历史上大概没有比哈雷彗星更引人注目了。７６年才出现一次的哈雷彗星，由于外观壮丽、... 相似文献
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一九八五年十一月十三日和十六日在国际哈雷彗星射电联测时段内,由加州大学贝克利分校I.D.Pater、芝加哥大学P.Palmer、伊利诺斯州立大学L.E.Snyder组成的观测小组,用设在新墨西哥州的美国国家射电天文台(NRAO)甚大阵(VLA)观测哈雷彗星的羟基(OH)谱线发射,得到了羟基最低能态(2II_3/2,J_5/3)F=2→2跃迁谱线(频率为 相似文献
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Yu. V. Sizonenko 《Kinematics and Physics of Celestial Bodies》2007,23(5):207-213
The plasma tails of comets C/2001 Q4 (NEAT) and C/2004 Q2 (Machholz) are investigated. For each comet we calculate the aberration angle, i.e., the angle between the cometary tail axis and the prolonged radius vector of the comet. The aberration angles are used to estimate the radial velocity of the solar wind in May 2004 and January–February 2005. The calculated velocities are compared to the solar wind velocities measured by space apparatuses in the circumterrestrial space. Possible causes of disagreement between these data are discussed 相似文献
12.
A great deal of attention has been given to the production and spatial distribution of sodium in comets after the discovery
of the sodium tail, by Cremonese et al. (1997a), on Hale-Bopp. The sodium has been observed in several comets in the past,
but the Hale-Bopp represent the first time where it will be deeply analyzed considering the several data and scientists working
on that. The sodium tail stimulated different studies trying to explain the mechanism source and provided the new lifetime
for photoionization of the neutral sodium atom. We took into account other sodium observations performed in this century and
we focalized our attention to comet Hale-Bopp to understand the main sources responsible for the sodium features observed.
We analyzed the sodium tail observations performed by Cremonese et al. (1997b) and Wilson et al. (1998) finding that the Hale-Bopp
had four different tails. The wide field images and the high resolution spectroscopy performed along the sodium tail provided
very important clues to distinguish the two sodium tails observed and their possible sources. Considering most of the data
reported in several papers has been possible to draw a real sketch on what has occurred to the comet during March and April
1997. We are going to demonstrate that the sodium tail observed by Wilson et al. (1998) was not the same reportedby Cremonese
et al. (1997a) and in the images taken by the European Hale-Bopp Team there were two distinct sodium tails. The observations
allowed us to define “narrow sodium tail” the tail reported by Cremonese et al. (1997a), and “diffuse sodium tail” the tail
overimposed to the dust tail. We suggest that the narrow sodium tail was due to a molecular process instead of the diffuse
one due to the release of sodium atoms by the dust particles. Such a conclusion is supported by the spatial distribution of
sodium on the nucleus and in the coma as reported from other authors.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
13.
Yu. V. Sizonenko 《Kinematics and Physics of Celestial Bodies》2012,28(1):9-14
We studied variations in the structure of plasma and dust tails of the C/2006 M4 (SWAN) comet during a long observation period
(September–December 2006). We found sizes of grains ejected by the comet from the synchronic-syndynamic analysis of comet
images. We calculated solar wind speed for high heliographic latitudes from calculations of the aberration angle of the comet
plasma tail. Rapid changes in the calculated values of the solar wind speed are caused by its variable transversal component. 相似文献
14.
We present the results of our analysis of the geometrical tidal tail characteristics for nearby and distant interacting galaxies. The sample includes more than two hundred nearby galaxies and about seven hundred distant ones. The distant galaxies have been selected in several deep fields of the Hubble Space Telescope (HDF-N, HDF-S, HUDF, GOODS, GEMS) and they are at mean redshift 〈z〉 = 0.65. We analyze the distributions of lengths and thicknesses for the tidal structures and show that the tails in distant galaxies appear shorter than those in nearby ones. This effect can be partly attributed to observational selection, but, on the other hand, it may result from the general evolution of the sizes of spiral galaxies with z. The positions of interacting galaxies on the galaxy luminosity (L)-tidal tail length (l) plane are shown to be explained by a simple geometrical model, with the upper envelope of the observed distribution being \(l \propto \sqrt L\). We have solved the problem on the relationship between the observed distribution of tail flatting and the tail length in angular measure by assuming the tidal tails to be arcs of circumferences visible at arbitrary angles to the line of sight. We conclude that the angular length of the tidal tails visually distinguished in nearby and distant galaxies, on average, exceeds 180°. 相似文献
15.
The comparison of data obtained in laboratory experiments on the solar wind interaction with a body endowed with a plasma shell, the observations of comet type I tails and the direct measurements near Venus show that an induced magnetosphere is formed with an extended magnetic tail. This magnetosphere appears due to currents associated with unipolar induction. The distribution of electrodynamical forces associated with the formation of the induced magnetosphere makes it possible to explain the acceleration of matter towards the tail as in the motion across the tail observed in comets and Venus. The analysis of the condensation motion in Halley's comet yields an estimate of tail magnetic field of 30 to 50. A three-dimensional model of the induced magnetospheres of Venus and comets is developed. 相似文献
16.
Eighty MHz observations of the occultation of the radio source Culgoora-1 0300 + 16 by the plasma tail of Comet Kohoutek (1973f) were made in February/March 1974 with the Culgoora radioheliograph. No detectable source broadening or change in flux density was observed, but the results showed a 2' arc anomaly in the observed position. This is greater than can be attributed to ionospheric refraction or experimental error. We suggest that it arose from refraction in the plasma tail of the comet. Similar observations of the occulation of the radio source Culgoora-1 2313-14 by the plasma tail of Comet West (1975n) were made at Culgoora in February 1976. These results were inconclusive but did suggest that the cometary plasma may have had some influence on the observed source position. The results are used to derive, from simple models, the distribution of electron density in comet tails. Peak electron densities of approximately 2 to 5 × 104 cm?3 and density gradients of ～0.05 cm?3 km?1 are indicated. 相似文献
17.
In our previous papers, we showed that at the final phases of the dynamical evolution of an open cluster, an extended population of stars elongated along its Galactic orbit, the stellar tail of the cluster, is formed. The tail stars that escaped from the cluster at different times move in a common orbit with low relative velocities. Experiencing a weak interaction with Galactic field stars, these objects, the relics of open clusters, can exist for a fairly long time. In this paper, we investigate the structures of such stellar tails in the nearest open clusters: Hyades, Pleiades, Praesepe, Alpha Persei, Coma, IC 2391, and IC 2602. To this end, we performed several numerical simulations of the dynamical evolution of these clusters in the tidal field of the Galaxy. Our computations of the dynamical evolution were based on known cluster age estimates and real Galactic orbits. The initial conditions were chosen in such a way that the parameters of the simulated clusters corresponded to their observed parameters. As a result, we obtained models of the stellar tails for the nearest open clusters and estimated such parameters of the tails as their sizes, densities, locations relative to the solar neighborhood, and others. 相似文献
18.
A unique short‐period (P = 0.65356(1) d) Mercury‐size Kepler exoplanet candidate KIC012557548b has been discovered recently by Rappaport et al. (2012). This object is a transiting disintegrating exoplanet with a circum‐planetary material–comet‐like tail. Close‐in exoplanets, like KIC012557548b, are subjected to the greatest planet‐star interactions. This interaction may have various forms. In certain cases it may cause formation of the comet‐like tail. Strong interaction with the host star, and/or presence of an additional planet may lead to variations in the orbital period of the planet. Our main aim is to search for comet‐like tails similar to KIC012557548b and for long‐term orbital period variations. We are curious about frequency of comet‐like tail formation among short‐period Kepler exoplanet candidates. We concentrate on a sample of 20 close‐in candidates with a period similar to KIC012557548b from the Kepler mission. We first improved the preliminary orbital periods and obtained the transit light curves. Subsequently we searched for the signatures of a circum‐planetary material in these light curves. For this purpose the final transit light curve of each planet was fitted with a theoretical light curve, and the residuals were examined for abnormalities. We then searched for possible long‐term changes of the orbital periods using the method of phase dispersion minimization. In 8 cases out of 20 we found some interesting peculiarities, but none of the exoplanet candidates showed signs of a comet‐like tail. It seems that the frequency of comet‐like tail formation among short‐period Kepler exoplanet candidates is very low. We searched for comet‐like tails based on the period criterion. Based on our results we can conclude that the short‐period criterion is not enough to cause comet‐like tail formation. This result is in agreement with the theory of the thermal wind and planet evaporation (Perez‐Becker & Chiang 2013). We also found 3 cases of candidates which showed some changes of the orbital period. Based on our results we can see that orbital period changes are not caused by comet‐like tail disintegration processes, but rather by possible massive outer companions. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
19.
Scott Gordon Bärbel Koribalski Keith Jones 《Monthly notices of the Royal Astronomical Society》2001,326(2):578-596
We present the results of new radio interferometer H i line observations for the merging galaxy pair NGC 4038/9 ('The Antennae'), obtained using the Australia Telescope Compact Array. The results improve substantially with respect to those of van der Hulst and show in detail the two merging galactic discs and the two tidal tails produced by their interaction. The small edge-on spiral dwarf galaxy ESO 572–G045 is also seen near the tip of the southern tail, but distinct from it. It shows no signs of tidal interaction. The northern tidal tail of the Antennae shows no H i connection to the discs and has an extension towards the west. The southern tidal tail is continuous, with a prominent H i concentration at its tip, roughly at the location of the tidal dwarf galaxy observed optically by Mirabel, Dottori & Lutz. Clear velocity structure is seen along the tidal tails and in the galactic discs. Radio continuum images at 20 and 13 cm are also presented, showing the discs in detail. 相似文献