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1.
The measured sky twilight brightness of a site is believed to be connected with main factors such as geographical latitude, elevation of the site above sea level, the season of observations and the aerosol pollution. These factors may decrease the sky twilight brightness and thus improve the crescent visibility limits. The effect of these factors on the visibility conditions to see the new Moon are investigated in the present work. The results show that the visibility conditions has improved at sites situated at higher northern geographical latitudes and higher elevation above sea level. The conditions to see the new Moon in winter season is better than the summer season. The aerosol pollution has a great effect on the visibility of the new Moon at sun's depression 5°, while for sun's depression greater than 5° the aerosol pollution has a small effect. 相似文献
2.
Amir Hasanzadeh 《Astrophysics and Space Science》2012,339(2):211-221
About 70 years ago “André Danjon” a French astrophysicist showed that as elongation of the moon decreases the arc length of
crescent gets less too. By studying the recent observational data, he concluded that at 7 degree elongation, the length of
arc (cusp to cusp) will reach zero degree. Today, this value is named as Danjon limit, which points to the limit at which
the moon crescent is formed. Danjon believed that the effective factor for occurring this limit was the shadows of moon’s
mountains. Later researchers have obtained different values for this limit. In this research based on the new data, the decreasing
dependence of length of arc versus elongation was obtained. The results show that the Danjon limit is about 5 degrees. The
effective factors to form the Danjon limit are then given and discussed. By considering the effects of astronomical seeing
and shadows of lunar features, the values of the arc length were calculated and compared with the observational data curve.
The results of this study show good agreement with the observational data. The present research shows that the above-mentioned
effects can reduce the length of arc. The effect of libration and roughness of the lunar terrain of the moon in forming the
moon crescent were also considered, and the possibility of observing thinner crescents by photometric model and breaking the
Danjon limit were given. 相似文献
3.
Giovanni Federico Gronchi 《Celestial Mechanics and Dynamical Astronomy》2009,103(4):301-326
Charlier’s theory (1910) provides a geometric interpretation of the occurrence of multiple solutions in Laplace’s method of
preliminary orbit determination, assuming geocentric observations. We introduce a generalization of this theory allowing to
take into account topocentric observations, that is observations made from the surface of the rotating Earth. The generalized
theory works for both Laplace’s and Gauss’ methods. We also provide a geometric definition of a curve that generalizes Charlier’s
limiting curve, separating regions with a different number of solutions. The results are generically different from Charlier’s:
they may change according to the value of a parameter that depends on the observations. 相似文献
4.
N. G. Rizvanov 《Earth, Moon, and Planets》1977,16(3):335-337
Aberrational displacement of the observed topocentric positions of the Moon differ from the aberrational effect in its apparent
ephemeris geocentric coordinates. The differential aberrational corrections due to the mutual positions of the observer and
the Moon, may account to 0
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″
3. The reduction method of astrometric observations of the Moon, which takes into account this effect, is proposed. 相似文献
5.
A technique for the fast identification of detected asteroids directly after terminating their observations on a short topocentric
arch is briefly described. 相似文献
6.
A. N. Opanasenko N. V. Opanasenko Yu. G. Shkuratov V. G. Kaidash Yu. I. Velikodskii V. V. Korokhin 《Kinematics and Physics of Celestial Bodies》2011,27(1):38-41
Polarimetric observations of the moon have been carried out at λeff = 0.48 and 0.63 μm using the 50 cm telescope of the Maidanak (Middle Asia) observatory. Imaging has been performed using
a Canon-350D camera with a CMOS array and rotating polaroid. The investigation covered the north-western part of the lunar
disk comprising the northern part of Ocean Procellarum and obtained the images representing the albedo, polarization degree, color index, and polarimetric color ratio at a phase
angle of 96°. It is the first time that the latter parameter has been imaged with a resolution of approximately 1 km. Its
pattern has proved to resemble that of the color index, although some important differences can be seen. This shows that spectropolarimetric
observations of the moon can give new information on the composition and optical properties of the lunar regolith. 相似文献
7.
Cudnik Brian M. Dunham David W. Palmer David M. Cook Anthony Venable Roger Gural Peter S. 《Earth, Moon, and Planets》2003,93(3):145-161
The occurrence and visibility of meteoroid impacts on the moon as seen from the earth were little more than speculation prior to November 1999. The best evidence of present-day impact activity came from the seismic experiments left on the Moon during the Apollo era. Past systematic attempts at earth-based observations to document lunar impacts revealed nothing conclusive. However, during the Leonid storms of 1999 and 2001, lunar impact events were for the first time confirmed by multiple independent observers. A total of 15 meteoritic impact flash events have been verified during these storms, with an additional 12 unconfirmed but likely events awaiting confirmation. Estimates of the mass of these meteoroids range from less than one gram for the faintest flashes to more than 10 kg for the brightest observed flash. The fraction of visible light to total energy produced by these events, a quantity known as luminous efficiency, averages about 0.001 for the established events. The confirmation of lunar meteoritic events on the Moon opens a new avenue in lunar and planetary research, one which could help bridge the gap between atmospheric sampling of the smallest components of meteoroid streams and interplanetary debris to the larger scale objects accessible to ground-based telescopes. 相似文献
8.
Roberto Armellin Pierluigi Di Lizia Michele Lavagna 《Celestial Mechanics and Dynamical Astronomy》2012,112(3):331-352
A method for high-order treatment of uncertainties in preliminary orbit determination is presented. The observations consist
in three couples of topocentric right ascensions and declinations at three observation epochs. The goal of preliminary orbit
determination is to compute a trajectory that fits with the observations in two-body dynamics. The uncertainties of the observations
are usually mapped to the phase space only when additional observations are available and a least squares fitting problem
is set up. A method based on Taylor differential algebra for the analytical treatment of observation uncertainties is implemented.
Taylor differential algebra allows for the efficient computation of the arbitrary order Taylor expansion of a sufficiently
continuous multivariate function. This enables the mapping of the uncertainties from the observation space to the phase space
as high-order multivariate Taylor polynomials. These maps can then be propagated forward in time to predict the observable
set at successive epochs. This method can be suitably used to recover newly discovered objects when a scarce number of measurements
is available. Simulated topocentric observations of asteroids on realistic orbits are used to assess the performances of the
method. 相似文献
9.
The process of calculating a good orbit from astrometric observations of the same object involves three main steps: preliminary orbit determination, least squares orbit fitting, and quality control assessing the orbit's uncertainty and reliability. For the next generation sky surveys, with much larger number density of observations, new algorithms, or at least substantial revisions of the classical ones, are needed. The classical theory of preliminary orbit algorithms was incomplete in that the consequences of the topocentric correction had not been fully studied. We show that it is possible to rigorously account for topocentric observations and that this correction may increase the number of alternate preliminary orbits without impairing the overall performance. We have developed modified least squares algorithms including the capability of fitting the orbit to a reduced number of parameters. The restricted fitting techniques can be used to improve the reliability of the orbit computing procedure when the observed arcs have small curvature. False identification (where observations of different objects are incorrectly linked together) can be discarded with a quality control on the residuals and a ‘normalization’ procedure removing duplications and contradictions. We have tested our algorithms on two simulations based on the expected performance of Pan-STARRS—one of the next generation all-sky surveys. The results confirm that large sets of discoveries can be handled very efficiently resulting in good quality orbits. In these tests we lost only 0.6 to 1.3% of the possible objects, with a false identification rate in the range 0.02 to 0.06%. 相似文献
10.
The optimum conditions to see the crescent of the new Moon have been obtained at Sacramento Peak and Maryland. We have used the data of the sky twilight brightness given by Koomenet al. (1952) for the two sites. The results show that the crescent can not be seen at the two sites for sun's depression less than 4° and 8° elongation between Sun, Moon and Earth confirming the results obtained before by Asaadet al. (1976). The visibility conditions at Maryland and Sacramento Peak are better than that obtained before for the three sites Misallat, Helwan and Daraw at Egypt. The reason is mainly due to the decrease in the sky twilight brightness at sites having higher geographical northern latitudes and high elevation above sea level. 相似文献
11.
Martin Šolc 《Astrophysics and Space Science》2005,296(1-4):43-54
Several important turning points appeared in the personal life and scientific career of Zdeněk Kopal, every time, when he
entered a new field of research. Four particular periods of his life will be commented in the present paper: the studies in
Prague and early observations in the variable star programme of the Czech Astronomical Society; the first lectures on close
binaries at Harvard; the intermezzo of lunar research; and the last period after 1989, when Zdeněk Kopal returned several
times to Prague University. 相似文献
12.
Modern asteroid surveys produce an increasingly large number of observations, which are grouped into very short arcs (VSAs) each containing a few observations of the same object in one single night. To decide whether two VSAs collected in different nights correspond to the same observed object we can attempt to compute an orbit with the observations of both arcs: this is called the linkage problem. Since the number of linkages to be attempted is very large, we need efficient methods of orbit determination. Using the first integrals of Kepler’s motion we can write algebraic equations for the linkage problem, which can be put in polynomial form. In Gronchi et al. (Celest Mech Dyn Astron 123(2):105–122, 2015) these equations are reduced to a polynomial equation of degree 9: the unknown is the topocentric distance of the observed body at the mean epoch of one VSA. Here we derive the same equations in a more concise way, and show that the degree 9 is optimal in a sense that will be specified in Sect. 3.3. We also introduce a procedure to join three VSAs: from the conservation of angular momentum we obtain a polynomial equation of degree 8 in the topocentric distance at the mean epoch of the second VSA. For both identification methods, with two and three VSAs, we discuss how to discard solutions. Finally, we present some numerical tests showing that the new methods give satisfactory results and can be used also when the time separation between the VSAs is large. The low polynomial degree of the new methods makes them well suited to deal with the very large number of asteroid observations collected by the modern surveys. 相似文献
13.
The distributions of sunspot longitude at first appearance and at disappearance display an east-west asymmetry that results
from a reduction in visibility as one moves from disk centre to the limb. To first order, this is explicable in terms of simple
geometrical foreshortening. However, the centre-to-limb visibility variation is much larger than that predicted by foreshortening.
Sunspot visibility is also known to be affected by the Wilson effect: the apparent ‘dish’ shape of the sunspot photosphere
caused by the temperature-dependent variation of the geometrical position of the τ=1 layer. In this article we investigate the role of the Wilson effect on the sunspot appearance distributions, deducing a
mean depth for the umbral τ=1 layer of 500 – 1500 km. This is based on the comparison of observations of sunspot longitude distribution and Monte Carlo
simulations of sunspot appearance using different models for spot growth rate, growth time and depth of Wilson depression. 相似文献
14.
Lunar meteoroid impact flashes provide a method to estimate the flux of the large meteoroid flux and thus their hazard to
spacecraft. Although meteoroid impacts on the Moon have been detected using video methods for over a decade, the difficulty
of manually searching hours of video for the rare, extremely brief impact flashes has discouraged the technique’s systematic
implementation. A prototype has been developed for the purpose of automatically searching lunar video records for impact flashes,
eliminating false detections, editing the returned possible flashes, and archiving and documenting the results. Several utilities
for measurement, analysis, and location of the flashes on the moon included in the program are demonstrated. Application of
the program to a year’s worth of lunar observations is discussed along with examples of impact flashes. 相似文献
15.
Michael R. Line E.J. Mierkiewicz R.J. Oliversen J.K. Wilson L.M. Haffner F.L. Roesler 《Icarus》2012,219(2):609-617
The lunar sodium tail extends long distances due to radiation pressure on sodium atoms in the lunar exosphere. Our earlier observations measured the average radial velocity of sodium atoms moving down the lunar tail beyond Earth (i.e., near the anti-lunar point) to be ～12.5 km/s. Here we use the Wisconsin H-alpha Mapper to obtain the first kinematically resolved maps of the intensity and velocity distribution of this emission over a 15° × 15 ° region on the sky near the anti-lunar point. We present both spatially and spectrally resolved observations obtained over four nights bracketing new Moon in October 2007. The spatial distribution of the sodium atoms is elongated along the ecliptic with the location of the peak intensity drifting 3° east along the ecliptic per night. Preliminary modeling results suggest the spatial and velocity distributions in the sodium exotail are sensitive to the near surface lunar sodium velocity distribution. Future observations of this sort along with detailed modeling offer new opportunities to describe the time history of lunar surface sputtering over several days. 相似文献
16.
对北京天文台动态频谱仪1996～1999年观测到的68群Ⅲ型爆发作了统计分析,并对这些事件的频率漂移、持续时间、偏振和带宽的基本特性作了定性分析. 相似文献
17.
Dmitry A. Pavlov James G. Williams Vladimir V. Suvorkin 《Celestial Mechanics and Dynamical Astronomy》2016,126(1-3):61-88
The aim of this work is to combine the model of orbital and rotational motion of the Moon developed for DE430 with up-to-date astronomical, geodynamical, and geo- and selenophysical models. The parameters of the orbit and physical libration are determined in this work from lunar laser ranging (LLR) observations made at different observatories in 1970–2013. Parameters of other models are taken from solutions that were obtained independently from LLR. A new implementation of the DE430 lunar model, including the liquid core equations, was done within the EPM ephemeris. The postfit residuals of LLR observations make evident that the terrestrial models and solutions recommended by the IERS Conventions are compatible with the lunar theory. That includes: EGM2008 gravitational potential with conventional corrections and variations from solid and ocean tides; displacement of stations due to solid and ocean loading tides; and precession-nutation model. Usage of these models in the solution for LLR observations has allowed us to reduce the number of parameters to be fit. The fixed model of tidal variations of the geopotential has resulted in a lesser value of Moon’s extra eccentricity rate, as compared to the original DE430 model with two fit parameters. A mixed model of lunar gravitational potential was used, with some coefficients determined from LLR observations, and other taken from the GL660b solution obtained from the GRAIL spacecraft mission. Solutions obtain accurate positions for the ranging stations and the five retroreflectors. Station motion is derived for sites with long data spans. Dissipation is detected at the lunar fluid core-solid mantle boundary demonstrating that a fluid core is present. Tidal dissipation is strong at both Earth and Moon. Consequently, the lunar semimajor axis is expanding by 38.20 mm/yr, the tidal acceleration in mean longitude is \(-25.90 {{}^{\prime \prime }}/\mathrm{cy}^2\), and the eccentricity is increasing by \(1.48\times 10^{-11}\) each year. 相似文献
18.
R. Yamada I. Yamada S. Tanaka N. Kobayashi Y. Ishihara K. Yomogida A. Fujimura 《Planetary and Space Science》2009,57(7):751-763
We developed a seismometer system for a hard landing “penetrator” probe in the course of the former Japanese LUNAR-A project to deploy new seismic stations on the Moon. The penetrator seismometer system (PSS) consists of two short-period sensor components, a two-axis gimbal mechanism for orientation, and measurement electronics. To carry out seismic observations on the Moon using the penetrator, the seismometer system has to function properly in a lunar environment after a hard landing (impact acceleration of about 8000 G), and requires a signal-to-noise ratio to detect lunar seismic events. We evaluated whether the PSS could satisfactorily observe seismic events on the Moon by investigating the frequency response, noise level, and response to ground motion of our instrument in a simulated lunar environment after a simulated impact test. Our results indicate that the newly developed seismometer system can function properly after impact and is sensitive enough to detect seismic events on the Moon. Using this PSS, new seismic data from the Moon can be obtained during future lunar missions. 相似文献
19.
Jeffrey L. Linsky 《Solar physics》1973,28(2):409-418
The solar millimeter continuum between 1 and 20 mm is recalibrated using observations of the average lunar brightness temperature at the center of lunar disk and new Moon brightness temperatures. The solar data are placed on a common scale according to the average lunar brightness temperature distribution proposed by Linsky. A least-squares parabolic regression curve is proposed for the solar millimeter continuum. A small departure from this regression curve near 8 mm may indicate the existence of an absorption feature.Staff member, Laboratory Astrophysics Division, National Bureau of Standards. 相似文献
20.
Robert M. Suggs William J. Cooke Ronnie J. Suggs Wesley R. Swift Nicholas Hollon 《Earth, Moon, and Planets》2008,102(1-4):293-298
NASA’s Meteoroid Environment Office has implemented a program to monitor the Moon for meteoroid impacts from the Marshall
Space Flight Center. Using off-the-shelf telescopes and video equipment, the Moon is monitored for as many as 10 nights per
month, depending on weather. Custom software automatically detects flashes which are confirmed by a second telescope, photometrically
calibrated using background stars, and published on a website for correlation with other observations. Hypervelocity impact
tests at the Ames Vertical Gun Range facility have begun to determine the luminous efficiency and ejecta characteristics.
The purpose of this research is to define the impact ejecta environment for use by lunar spacecraft designers of the Constellation
manned lunar program. The observational techniques and preliminary results will be discussed.
The U.S. Government's right to retain a non-exclusive, royalty-free license in and to any copyright is acknowledged. 相似文献