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121.
M.G. Berthoud 《Icarus》2005,175(2):382-389
An increasing number of objects discovered in the Solar System have irregular shapes which require unconventional mapping techniques. Here we present a technique that produces equivalent maps of such objects. As such maps preserve surface area they are especially useful for mapping the distribution of geological features on irregular objects. Maps of blocks and craters on the Asteroid 433 Eros are used to illustrate the potential use of the technique. Two equal-area maps are adequate to cover the entire asteroid and convincingly demonstrate variations in surface density of mapped features. Similar coverage by orthographic views requires 4 to 6 plots. The distortion of the maps are comparable to the distortions of maps created by other techniques. 相似文献
122.
苏定强 《紫金山天文台台刊》2003,(1)
目前 ,已有 1 0架口径 8~ 1 0m的地面大望远镜建成并投入科学观测。在近红外波段 ,自适应光学和干涉术已在大望远镜上获得成功。Hubble空间望远镜发射至今已逾 1 2年。为了研究早期宇宙 ,探测类地行星等 ,2 0 0 2年 9月NASA已与TWR公司签约 ,研制口径≥ 6m的下一代空间望远镜JWST ,计划2 0 1 0年发射。许多口径 30~ 1 0 0m的地面未来巨型望远镜FGT项目已经提出。本报告 ,也介绍了我国正在研制或预研中的三个大项目 :LAMOST、FAST和SST ,这些项目虽较小 ,但完成后都会对天文学的一个方面作出有份量的贡献。最后 ,报告人建议我国参与到与国外合作研制FGT或NGST的工作中 ,特别强调要有天文学家和工程专家参与进去 相似文献
123.
124.
H. Rickman G. B. Valsecchi Cl. Froeschlé 《Monthly notices of the Royal Astronomical Society》2001,325(4):1303-1311
We investigate the first stage of the dynamical evolution of Oort cloud comets entering the planetary region for the first time. To this purpose, we integrate numerically the motions of a large number of fictitious comets pertaining to two samples, both with perihelion distances up to 5.7 au and random inclinations; the first sample is composed of comets whose orbits have at least one node close to 5.2 au, while the second is not subject to this constraint. We examine the orbits when the comets come to aphelion after their first perihelion passage within the planetary region, and find that there is a clear statistical dependence of the energy perturbations on the Tisserand parameter. There appear to be two main processes, of comparable importance, governing the shortening of semimajor axes to values of less than 1000 au, i.e. planetary close encounters, especially with Jupiter, and indirect perturbations due to the shifting of the motion from barycentric to heliocentric and back; the former process mostly affects comets crossing the ecliptic at about 5.2 au, or on low-inclination orbits, while the latter mostly affects comets of small perihelion distance. This last result may help to understand the relative paucity of Halley-type comets with perihelion distances larger than about 1.5 au. 相似文献
125.
P. Nurmi M.J. Valtonen J.Q. Zheng 《Monthly notices of the Royal Astronomical Society》2001,327(4):1367-1376
Time variation in impact probability is studied by assuming that the periodic flux of the Oort Cloud comets within 15 au arises from the motion of the Sun with respect to the Galactic mid-plane. The periodic flux clearly shows up in the impact rate of the captured Oort Cloud cometary population, with a phase shift caused by the orbital evolution. Depending on the assumed flux of comets and the size distribution of comets, the impact rate of the Oort Cloud comets of 1 km in diameter or greater is from 5 to 700 impacts Myr−1 on the Earth and from 0.5 to 70 impacts per 1000 yr on Jupiter. The relative fractions of impacts are 0.09, 0.11, 0.26 and 0.54 for long-period comets, Halley type comets, Jupiter family comets and near-Earth objects, respectively. For Jupiter, the corresponding fractions in the first three categories are 0.18, 0.31 and 0.51. If we consider physical fading of comet activity that is compatible with the observations, then the impact rates of active comets are two orders of magnitude smaller than the total impact rates by all kinds of comets and cometary asteroids of size 1 km or greater. 相似文献
126.
Henry Florence Bockelée-Morvan Dominique Crovisier Jacques Wink Jörn 《Earth, Moon, and Planets》2002,90(1-4):57-60
CO was observed on March 11, 1997 in comet Hale–Bopp with theIRAM Plateau de Bure interferometer. The maps show evidence for
asymmetrical patterns, due to the Existence of CO jets. Analysis of the spectra and their velocity shifts shows that there
is a spiral CO jet rotating in a plane almost perpendicular to the sky plane.This is the first time that rotating jets are
observed for parent molecules.We have developed a 3-D model simulating rotating spiral jets of CO gas.We present here the
comparison between the observations and our model. 相似文献
127.
The investigation of fragmented comets provides information on the physical properties and internal structure of cometary nuclei, as well as insights into the mechanisms responsible for cometary breakups. The Jupiter-family Comet 73P/Schwassmann-Wachmann 3 (73P/SW3) fragmented non-tidally into at least four components, and probably more, in the autumn of 1995. Fragment C was detected with the Wide Field Planetary Camera 2 (WFPC2) of the Hubble Space Telescope (HST) on 26 November 2001 when it was 3.26 AU from the Sun and 2.34 AU from the Earth. The high spatial resolution of the HST allowed us to separate the signal of the fragment from that of its coma, and to determine its R magnitude in the Johnson-Kron-Cousins photometric system from four images taken with the F675W filter. Assuming a spherical body with a geometric albedo of 0.04 and a linear phase coefficient of 0.04 mag deg−1 for the R band, we derived an effective radius of . The pre-breakup radius of the original nucleus was estimated to be 1.1 km, which implies that the volume of fragment C is ∼25% of the total volume of the pre-breakup nucleus. The limited temporal coverage of our observations preclude deriving an accurate shape or rotational period; our measurements are consistent with a rather spherical body but an elongated shape cannot be excluded. Fragment C was very active despite its rather large heliocentric distance, with an estimated dust production rate of (∼130 metric tons day−1). A very large fraction of the surface area of fragment C must have been sublimating to sustain such a high level of activity. Fragment C may be recovered at its next return in 2006, if it does not experience further fragmentation. 相似文献
128.
Infrared observations of comets C/1996 B2 (Hyakutake) and C/1995 O1 (Hale-Bopp) benefited from the high spectral resolution
and sensitivity of échelle spectrometers now equipping ground-based telescopes and from the availability of the Infrared Space
Observatory (ISO).
From the ground, several hydrocarbons were unambiguously detected for the first time: CH4, C2H2, C2H6. Water was observed through several of its hot vibrational bands, escaping telluric absorption. CO, HCN, NH3 and OCS were also observed, as well as several radicals. This permitted the evaluation of molecular production rates, of
rotational temperature, and — taking advantage of the 1-D imaging of long-slit spectroscopy — of the space distribution of
these species. With ISO, carbon dioxide was directly observed for the second time in a comet (after its detection from the
Vega probes in P/Halley). The spectrum of water was investigated in detail (several bands of vibration and far-infrared rotational
lines), permitting the evaluation of the rotational temperature of water, and of it spin temperature from the ortho-to-para
ratio. Water ice was identified in the grains of Hale-Bopp as far as 7 AU from the ground and possibly at 3 AU with ISO. The
composition of cometary volatiles appears to be strikingly similar to that of interstellar ices.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
129.
130.
Weaver H. A. Brooke T. Y. Chin G. Kim S. J. Bockelée-Morvan D. Davies J. K. 《Earth, Moon, and Planets》1997,78(1-3):71-80
High resolution (λ/δλ ∼ 20,000) spectra of comet C/1995 O1 (Hale-Bopp) in the 2–5 μm region were obtained during UT 2–5 March
1997 using CSHELL at the NASA Infrared Telescope Facility (IRTF) on Mauna Kea. The heliocentric and geocentric distances of
the comet were ∼1.1 AU and ∼1.5 AU,respectively. We detected emission lines of the gas-phase molecules H2O, 4, C2H6, C2H2, HCN, and CO and derived absolute production rates and relative abundances for all species. We also used the 2-dimensional
nature of the CSHELL data to investigate the spatial distribution of the molecules and find evidence that CO was derived at
least partly from an extended source in the coma.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献