Center Of Moon Research Articles

The design of the Moon Center based on the female perspective

With the opening of China's three child policy and the continuous development of social economy, China's industrial structure has changed constantly. As a new economic growth point, the maternity and infant industry has become a hot industry in recent years. New service industries such as Moon Sister and Moon Center have developed rapidly. The scientific and comfortable modern moon center is increasingly favored by young women. It is undeniable that the emergence of maternity care institutions has timely met the needs of women for puerperal care today. However, there are always many imperfections in the development of emerging industries at the time of their inception, and the Moon Club entered the mainland market late and is in the initial stage of industrial development. From the actual situation of the few existing Moon Centers, it only meets the immediate needs and hasty response, and fails to fundamentally improve and enhance the reasonable, humanized, scientific planning, design and research of Moon Centers. The space function and design style are not mature enough, and there is no deep concept to support it. It is a superficial form, so women's demand for the existing indoor space of postpartum care center has not been met. Therefore, the interior design of postpartum care center must start to change the original design thinking, no longer simply pursue the excessive exaggeration and blandness in style and decoration, but should design a warm and comfortable interior space that conforms to the consumption psychology and aesthetic psychology of newborn mothers based on emotional needs, especially for the functional care of related nursing spaces and its feasible humanized and emotional design.

Forced Keplerian orbits in the Earth–Moon system

Motivated by the fact that the mass of the Moon is about one percent of the Earth mass we consider in this paper Keplerian orbits of satellites (or spacecrafts) in the Earth–Moon system. These orbits represent approximate solutions of the basic equations of motion. As a result a satellite in one of these orbits will require some thrust to stay in orbit. In spite of this issue these orbits might be of interest when satellites orbits have to satisfy some practical constraints. In this paper we explore two types of such orbits. The first is around the Earth–Moon center of mass. The second consists of orbits whose center is along the line from Earth to the Moon but at some distance from Earth–Moon center of mass. As examples we consider briefly orbits for an Earth observation station and an Earth–Moon cycler (Casoliva et al., 2008). (In the following we use the term “Earth–Moon shuttle” to mean “Earth–Moon cycler”). Throughout this paper we use symbiosis between analytical and numerical methods to derive the desired results.

Cislunar Navigation Accuracy Using Optical Observations of Natural and Artificial Targets

Onboard optical-based autonomous navigation (autonav) has the potential to significantly reduce reliance on ground-based assets, and it can provide a robust backup system for unexpected ground outages. An investigation of autonav across the solar system is continued here by assessing optical-only navigation performance in cislunar space using simulated observations of the center of the moon, lunar landmarks, artificial satellites, and asteroids. It is shown that autonav in cislunar space is feasible and effective within current technological capabilities, and that artificial satellites, the moon center, and lunar landmarks are effective targets for navigation in this region.

Determining the angular resolution of an air shower array including five scintillation detectors using two methods: Shadow of the moon and the CORSIKA simulation

Abstract An array including five scintillation detectors at Sharif University of Technology in Tehran ( 35 ° 4 3 ′ N, 51 ° 2 0 ′ E, 1200m a.s.l= 897 gcm−2), over a year from October 2016 to October 2017, collected more than 5 . 6 × 1 0 5 extensive air shower ( EAS) events in the energy range between 0.03PeV and 3PeV. Data from the array were used to examine the cosmic ray shadow of the Moon in the energy range mentioned. The observation of a deficit of cosmic rays in the direction of the moon can be an estimate of the accuracy of the measurement of the primary particles of the air showers. The deficit of cosmic rays from the direction of the moon, in fact, is due to the presence of the moon in the early direction of the cosmic rays which prevents them from reaching the earth, and is interpreted as the shadow of the moon. A preliminary analysis of the directions of cosmic rays has been done in a two-dimensional sky map (zenith and azimuth angles) to compare the deficit of cosmic rays in terms of the angular radius from the moving moon center with the centers randomly selected in the sky. In this method, a two-dimensional Gaussian distribution for shadowed events is considered, which the standard deviation of this distribution is interpreted as the angular resolution of the array. Also, using the CORSIKA simulation data, the angular resolution of this array is obtained for different energies and different zenith angles and its mean value is calculated by considering the probability of detecting different energies by the array. The angular resolutions obtained with these two methods are comparable.

A Study on the Semiotics and Poetic Meaning of Literature Content - at the Center of Moon Sam­seok's Children's Poetry -

A Study on the Semiotics and Poetic Meaning of Literature Content - at the Center of Moon Sam­seok's Children's Poetry -

Multifrequency model of Earth tidal deformations within framework of three-body problem

The Earth tidal deformation is studied. Earth is considered as a visco-elastic axially symmetrical body with a solid core. For the description of the visco-elastic Earth part the linear theory of visco-elasticity is used. It is assumed that the Earth - Moon center of mass moves on the constant elliptic orbit around the Sun, that is considered as attractive center. From the d’Alembert - Lagrange principle the system of motion equations is obtained. Then the displacement vector is expanded in series of Earth’s oscillation modes. The system of ordinary differential equations for modal variables is obtained. This system describes process of oscillations, but in real situation we can consider these deformations as quasi-stationary ones. Hence, we can discard inertial members in equations. We can expand right parts of equations in series by orbit’s eccentricities of the Earth - Moon center of mass and of the Earth (Moon). Then we can look, that the right parts of the equations are the series with coefficients depending of angles combinations, hence modal variables can be represented also as the similar series. From these conditions we can find approximately of Sun - Moon’s tidal frequencies. We find well known frequencies, corresponding periods as year, half year, month, half month, day, half day, frequencies combinations, near above mentioned and large quantity of other combinations.

Interactive visualization of 3D lunar model with texture and labels, using Chang’E-1 data

A lunar model with real texture can be obtained by mapping texture onto the lunar mesh, but the convergence in the polar regions of lunar model is a problem. In this paper, we build a 3D lunar model and solve this problem by texture partitioning and transforming. The whole lunar map is divided into four images and the polar images are transformed to circular textures before mapped to the semi-regular (SR) lunar mesh which is obtained through denoising, triangulating, subdividing and resampling the laser altimetry (LAM) data. Hundreds of lunar labels are classed into three levels and added gradually to the lunar model considering the distance between the viewpoint and the moon center. Through some techniques such as mip-map and view-dependent, the lunar model with textures and labels can be interactively browsed on a personal computer (PC) in real time.

3D visualization of solar wind ion data from the Chang'E-1 exploration

Chang'E-1 (abbreviation CE-1), China's first Moon-orbiting spacecraft launched in 2007, carried equipment called the Solar Wind Ion Detector (abbreviation SWID), which sent back tens of gigabytes of solar wind ion differential number flux data. These data are essential for furthering our understanding of the cislunar space environment. However, to fully comprehend and analyze these data presents considerable difficulties, not only because of their huge size (57 GB), but also because of their complexity. Therefore, a new 3D visualization method is developed to give a more intuitive representation than traditional 1D and 2D visualizations, and in particular to offer a better indication of the direction of the incident ion differential number flux and the relative spatial position of CE-1 with respect to the Sun, the Earth, and the Moon. First, a coordinate system named Selenocentric Solar Ecliptic (SSE) which is more suitable for our goal is chosen, and solar wind ion differential number flux vectors in SSE are calculated from Geocentric Solar Ecliptic System (GSE) and Moon Center Coordinate (MCC) coordinates of the spacecraft, and then the ion differential number flux distribution in SSE is visualized in 3D space. This visualization method is integrated into an interactive visualization analysis software tool named vtSWIDs, developed in MATLAB, which enables researchers to browse through numerous records and manipulate the visualization results in real time. The tool also provides some useful statistical analysis functions, and can be easily expanded.

Initial observations from the Lunar Orbiter Laser Altimeter (LOLA)

As of June 19, 2010, the Lunar Orbiter Laser Altimeter, an instrument on the Lunar Reconnaissance Orbiter, has collected over 2.0 × 109 measurements of elevation that collectively represent the highest resolution global model of lunar topography yet produced. These altimetric observations have been used to improve the lunar geodetic grid to ∼10 m radial and ∼100 m spatial accuracy with respect to the Moon's center of mass. LOLA has also provided the highest resolution global maps yet produced of slopes, roughness and the 1064‐nm reflectance of the lunar surface. Regional topography of the lunar polar regions allows precise characterization of present and past illumination conditions. LOLA's initial global data sets as well as the first high‐resolution digital elevation models (DEMs) of polar topography are described herein.

The Lunar Orbiter Laser Altimeter Investigation on the Lunar Reconnaissance Orbiter Mission

The Lunar Orbiter Laser Altimeter (LOLA) is an instrument on the payload of NASA's Lunar Reconnaissance Orbiter spacecraft (LRO) (Chin et al., in Space Sci. Rev. 129:391-419, 2007). The instrument is designed to measure the shape of the Moon by mea- suring precisely the range from the spacecraft to the lunar surface, and incorporating preci- sion orbit determination of LRO, referencing surface ranges to the Moon's center of mass. LOLA has 5 beams and operates at 28 Hz, with a nominal accuracy of 10 cm. Its primary objective is to produce a global geodetic grid for the Moon to which all other observations can be precisely referenced.

Research of Circuit System in CCD Ultraviolet Sensor for Probing Moon

介绍了我国探月工程之嫦娥一号卫星的紫外CCD敏感器系统的CCD电路的软硬件的开发研究.紫外CCD敏感器由光学结构、CCD及处理线路、数据处理单元及其软件组成.入射光经光学系统后,照射在CCD敏感元件,经视频处理电路处理后形成数字图像信号.数字图像信号保存在数据存储器中,由数据处理器进行分析处理.计算得到月球的中心并转换为探测器对月姿态角,其中紫外CCD敏感器头部电路包括CCD电路、时序电路、驱动电路、视频处理电路和电源电路.核心器件CCD采用E2V公司的CCD48-20芯片,文中重点介绍该CCD的时序、驱动和Smear等难点问题.

Polarization and Physical Properties of the August 11, 1999 White-Light Corona

Four series of coronal images have been obtained by the expedition of Abastumani Astrophysical Observatory during the August 11, 1999 total solar eclipse with the help of a photographic mirror–lens polarimeter (D = 100 mm, F = 1000 mm). Each series include three images corresponding to three positions of the polarization analyzer. The position of the solar disk center relative to the Moon's center has been determined beforehand. In addition, the background skylight polarization and intensity are calculated. All measurements are absolute given in units of the Sun's average surface brightness. A new technique for separation of the F- and K-coronae is used. It was found that in the equatorial regions the model of hydrostatic distribution of the density with T = constant is not quite accurate for the August 11, 1999 corona and there is a temperature gradient in this region. For r1 = 1.3R⊙ and r2 = 1.8R⊙ we derived T1 = 1.25×106 K and T2 = 1.07×106 K, respectively. The average polarization degree in the equatorial regions changes from 10 to 40%, while in the polar regions the maximum value reaches only 10%. The values of electron densities Ne(r) vary from 1.32×108 cm−3 (r = 1.1R⊙) to 2.0×106 cm−3 (r = 2.0R⊙). Our data are compared with previous measurements.

Broadband submillimeter measurements of the full Moon center brightness temperature and application to a lunar eclipse

We report on observations of the full Moon brightness temperature covering the frequency range of 300–950 GHz, and also on observations of the lunar eclipse of July 16, 2000, though only covering the frequency range of 165–365 GHz due to poor atmospheric transmission at higher frequencies. All observations were performed from the summit of Mauna Kea (HI) using a Fourier Transform Spectrometer mounted on the Caltech Submillimeter Observatory and supplemented by measurements of the atmospheric opacity using a 183 GHz Water Vapor Monitor. The telescope was pointed to the center of the lunar disk (with a footprint of ∼45–15 km on the Moon at 300 through 900 GHz). In order to obtain the correct values of the Moon brightness temperatures at all frequencies we carefully corrected for the atmospheric absorption, which varies across the submillimeter domain. This correction is fully described. The measured pre-eclipse brightness temperature is around 337 K in the 165–365 GHz range. This temperature slightly increases with frequency to reach ∼353 K at 950 GHz, according to previous broader band data. The magnitude of the temperature drop observed during the eclipse at 265 GHz (central frequency of the band covered) was about ∼70 K, in very good agreement with previous millimeter-wave measurements of other lunar eclipses. We detected, in addition, a clear frequency trend in the temperature drop that has been compared to a thermal and microwave emission model of the lunar regolith, with the result of a good match of the relative flux drop at different frequencies between model and measurements.

Polarization and intensity studies of the August 11, 1999 solar corona

Four series of coronal images have been obtained by the expedition of Abastumani Astrophysical Observatory during the August 11, 1999 total solar eclipse with the help of the photographic mirror-lens polarimeter (D=150 mm, F=1000 mm). Each series includes three images corresponding to three positions of the polarization analyzer. The position of the solar disk center relative to the Moon's center has been determined beforehand. In addition, the background skylight polarization and intensity are calculated. All measurements are absolute given in units of the sun's average surface brightness. Equatorial electron densities and temperatures are determined. Our data are compared with previous absolute measurements. To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Development of a filter for operation of atmospheric Cherenkov telescopes close to the Moon

A filter has been developed and tested for the ARTEMIS experiment with solar-blind photomultiplier tubes. The filter consists of CoSO 4, NiSO 4, and 2,7-dimethyl-3,6-diazacyclohepta-2,6-diene perchlorate solutions in water. The filter transmission is about 65% in the wavelength range 230–270 nm. The NiCo solution allows a factor of 10 reduction in the background light from the Moon and the dye introduces another factor of 20. This reduction reduces significantly the systematics due to the position of the Moon. The new arrangement allows the center of the camera to be as close as 2° from the Moon center without any bias to a specific direction from the moon at any phase.

Medicare reform: nibbling at catastrophic costs.

Prologue: The 1980s have produced virtually no new federal health programs and few new benefits in existing programs. Congress has been largely consumed by efforts to constrain the growth of health entitlement programs created in an earlier era when tax revenues were easier to come by. Nevertheless, health and medical issues have remained popular subjects for politicians to address. And in the few instances where President Reagan actually proposed a liberalization of a federal program. Congress reacted with enthusiasm. In this paper, Judith Feder, Marilyn Moon, and William Scanlon explore the limits of health care reform—1980s style—pointing out that the Medicare catastrophic benefit under discussion on Capitol Hill is less than meets the eye or fits the rhetoric. Feder, who holds a doctorate in political science from Harvard University, and Scanlon, who has a similar degree in economics from the University of Wisconsin, are codirectors of Georgetown University's Center for Health Policy Studies. The center, which also is codirected by economist Jack Hadley, devotes the bulk of its analytic time to health financing issues, with a heavy emphasis on hospital and nursing home payment. The center also provides support to The Robert Wood Johnson Foundation in its development of program demonstrations and other projects. Moon, who holds a doctorate in economics from the University of Wisconsin, is director of the American Association of Retired Persons' (AARP) Public Policy Institute. Before joining the association, she worked as an analyst at the Congressional Budget Office and as a researcher at the Urban Institute. Moon's center is a recent creation of the AARP, a powerful influence on federal social policy by virtue of its diverse membership of 28 million people over age fifty. Moon's professional staff of eighteen concentrates its analytic efforts on issues that run the gamut of domestic policy. Seven analysts devote themselves to health issues, including long-term care, the quality of medical care, and physician-related issues.

Equivalence of active and passive gravitational mass using the moon.

Based on an asymmetry in the composition of the moon, a limit is established for the violation of the equity of passive and active gravitational mass. It is suggested that the 2-km offset between the moon's center of figure and center of mass imply an asymmetry in the distribution of Fe and Al, and that the Fe on one side and the Al on the other must attract another with equal force in order for the moon to follow the orbit predicted by classical mechanics. Based on laser ranging data and a model for the moon's interior, the ratios of active to passive mass for Fe and Al are found to be equal to a precision of 4 x 10 to the -12th.

Mascons and the moon's orientation

This letter reports the discovery of a relation between the moments of inertia of the mascons (taken about the moon's center) and the moon's moments of inertia. It is found that the principal axes of the mascons alone are nearly parallel to those of the moon. Possible explanations of this parallelism are discussed. If the mascons are associated with a layer of uncompensated basalt on the moon's nearside, then the parallelism can be adequately explained on the grounds that the mascons and basalts together determined the moon's orientation. On the other hand, the third-order harmonics of the moon's gravity field indicate that the excess mass controlling the moon's orientation is on the farside. It thus appears that the mascons have been emplaced in special sites whose position was controlled by the processes which produced the farside highlands.

The great-circle pattern of large circular maria: product of an earth-moon encounter

The circular maria - Orientale, Imbrium, Serenitatis, Crisium, Smythii, and Tsiolkovsky -lie nearly on a lunar great circle. This pattern can be considered the result of a very close, non-capture encounter between Moon and Earth early in solar-system history. Of critical importance in analyzing the effects of such an encounter is the position of the weightlessness limit of the Earth-Moon System which is located at about 1.63R e, measured from the center of Earth to center of Moon. Within this weightlessness limit, material can be pulled from the lunar surface and interior by Earth's gravity and either escape from the Moon or be redistributed onto the lunar surface. In the case of an encounter with a non-spinning Moon, backfalling materials would be distributed along a lunar great circle. However, if the Moon is rotating during the encounter, the backfall pattern will deviate from the great circle, the amount depending on the rate and direction of spin. Such a close encounter model may be related to the pattern of circular maria if materials departing from the source region are visualized as spheroids of molten lunar upper mantle basalt. These spheroids, then, would impact onto the lunar surface to form a pattern of lava lakes. Radiometric dates from mare rocks are consistent with this model of mare formation if the older mare rock dates are considered to date the encounter and younger dates are considered to date subsequent volcanic eruptions on a structurally weakened Moon.

An operational theory of laser-radar selenodesy

A theory of the utilization of laser techniques for ranging from the Earth to the Moon for the purpose of providing control points on the lunar surface at which the figure of the Moon is measured to an accuracy at least an order of magnitude better than that of the present astrometric measurements is presented. This, in turn, increases the accuracy of the horizontal selenocentric coordinates of topographical features measured by present astrometric methods. The improvement in the vertical and horizontal coordinates of control points in the Apollo landing zone will aid in the analysis of Unmanned Lunar Orbiter photographs for the selection of Apollo landing sites. The present discussion proposes the means of obtaining the ground control upon which the Orbiter photogrammetry is to be fastened. In addition, a technique of combining Goldstone tracking data to show where the resulting lunar figure is positioned relative to the Moon's center of mass is presented. If corner reflectors are placed on the lunar surface, as suggested by many members of the scientific community, or on a lunar orbiting vehicle, one or more Earth-based laser ranging systems are essential. These reflectors will give enough enhancement in return signal to allow for an additional increase in range accuracy of one to two orders of magnitude. In addition to the primary data on the figure of the Moon, a number of other measurements of scientific importance are then readily obtainable. As far as the measurement of control points is concerned, however, the use of corner reflectors is not essential for the success of this project. Questions regarding the influence on the present shape of the Moon of the frozen tide, isostasy, and past impacts of large asteroids appear in large part answerable through the data which are indicated to be obtainable under the present theory.