Despite Pluto’s demotion to dwarf planet status,people are still attached to it.Scientists combined observations of Pluto from NASA’s New Horizons probe with observations of comet Churyumov-Gerasimenko from the Euro...Despite Pluto’s demotion to dwarf planet status,people are still attached to it.Scientists combined observations of Pluto from NASA’s New Horizons probe with observations of comet Churyumov-Gerasimenko from the European Space Agency’s Rosetta probe and found that Pluto’s nitrogen abundance matched the pattern of about a billion comets,which led to the theory that Pluto is made of about a billion comets.Yet they don’t know exactly when or where these comets originated.By studying the origin and orbit of comets,the author of this paper found that the material that condensed Pluto was mainly comets and dust ejected by Neptune,and the Kuiper Belt objects were condensed by material ejected by Neptune toward the outer side of its orbit.展开更多
We intend to study a modified version of the planar Circular Restricted Three-Body Problem(CRTBP) by incorporating several perturbing parameters. We consider the bigger primary as an oblate spheroid and emitting radia...We intend to study a modified version of the planar Circular Restricted Three-Body Problem(CRTBP) by incorporating several perturbing parameters. We consider the bigger primary as an oblate spheroid and emitting radiation while the small primary has an elongated body. We also consider the perturbation from a disk-like structure encompassing this three-body system. First, we develop a mathematical model of this modified CRTBP.We have found there exist five equilibrium points in this modified CRTBP model, where three of them are collinear and the other two are non-collinear. Second, we apply our modified CRTBP model to the Sun–Haumea system by considering several values of each perturbing parameter. Through our numerical investigation, we have discovered that the incorporation of perturbing parameters has resulted in a shift in the equilibrium point positions of the Sun–Haumea system compared to their positions in the classical CRTBP. The stability of equilibrium points is investigated. We have shown that the collinear equilibrium points are unstable and the stability of non-collinear equilibrium points depends on the mass parameter μ of the system. Unlike the classical case, non-collinear equilibrium points have both a maximum and minimum limit of μ for achieving stability. We remark that the stability range of μ in non-collinear equilibrium points depends on the perturbing parameters. In the context of the Sun–Haumea system, we have found that the non-collinear equilibrium points are stable.展开更多
The population of Neptune Trojans is believed to be bigger than that of Jupiter Trojans and that of asteroids in the main belt, although only eight members of this distant asteroid swarm have been observed up to now. ...The population of Neptune Trojans is believed to be bigger than that of Jupiter Trojans and that of asteroids in the main belt, although only eight members of this distant asteroid swarm have been observed up to now. Six leading Neptune Trojans around the Lagrange point L4 discovered earlier have been studied in detail, but two trailing ones found recently around the L5 point, 2004 KV18 and 2008 LC18, have not yet been investigated. We report our investigations on the dynamical behaviors of these two new Neptune Trojans. Our calculations show that the asteroid 2004 KV18 is a temporary Neptune Trojan. Most probably, it was captured into the trailing Trojan cloud no earlier than 2.03 ×105 yr ago, and it will not maintain this position later than 1.65 × 105 yr in the future. Based on the statistics from our orbital simulations, we ar- gue that this object is more like a scattered Kuiper belt object. By contrast, the orbit of 2008 LC18 is much more stable. Among the clone orbits spreading within the orbital uncertainties, a considerable portion of clones may survive on the L5 tadpole orbits for 4 Gyr. The strong dependence of the stability on the semimajor axis and resonant angle suggests that further observations are badly required to constrain the orbit in the stable region. We also discuss the implications of the existence and dynamics of these two trailing Trojans over the history of the solar system.展开更多
Cometary nuclei, the remnant icy bodies of planet formation, located at the outer edge of the solar system, are relatively poorly studied because of their small sizes and thus faintness. Thus far more than a hundred l...Cometary nuclei, the remnant icy bodies of planet formation, located at the outer edge of the solar system, are relatively poorly studied because of their small sizes and thus faintness. Thus far more than a hundred large members (size about 100 km) of this cometary population in the Kuiper belt have been identified. Smaller bodies (10 km) are much too faint to image directly and their number so far can only be extrapolated on theoretical grounds. The Taiwan-America Occultation Survey (TAOS) will conduct a census of the number of Kuiper belt objects down to a few km size by monitoring chance stellar occultations by these cometary nuclei. We will set up an array of small (50cm), wide-field (f/1 9) telescopes, each equipped with a 2K squared CCD camera, along a 7 km baseline in central Taiwan at an elevation above ～ 3000 m. The robot telescopes will operate in a coincidence mode, so the sequence and timing of any candidate occultation event can be recorded and distinguished against a false detection. The Lawrence Livermore National Laboratory, the National Central University, and the Academia Sinica, will each contribute one telescope system. Researchers from an international variety of institutes are also participating in the project. Our experiment provides the only means to study the cometary population in the small-sized end of the distrbution. A great number of scientific byproducts, notably variable stars, will also derive from the huge TAOS database, some 10, 000 giga-bytes worth of photometrical measuremements per year.展开更多
The orbital migration of Jovian planets is believed to have played an important role in shaping the Kuiper Belt. We investigate the effects of the long time-scale （2 ×107 yr） migration of Jovian planets on the ...The orbital migration of Jovian planets is believed to have played an important role in shaping the Kuiper Belt. We investigate the effects of the long time-scale （2 ×107 yr） migration of Jovian planets on the orbital evolution of massless test particles that are initially located beyond 28 AU. Because of the slowness of the migration, Neptune＇s mean motion resonances capture test particles very efficiently. Taking into account the stochastic behavior during the planetary migration and for proper parameter values, the resulting concentration of objects in the 3：2 resonance is prominent, while very few objects enter the 2：1 resonance, thus matching the observed Kuiper Belt objects very well. We also find that such a long time-scale migration is favorable for exciting the inclinations of the test particles, because it makes the secular resonance possible to operate during the migration. Our analyses show that the us secular resonance excites the eccentricities of some test particles, so decreasing their perihelion distances, leading to close encounters with Neptune, which can then pump the inclinations up to 20°.展开更多
A first-order question in the studies of the Solar System is how its outer zone known as the Kuiper belt was created and evolved.Two end-member models, involving coagulation vs. streaming instability, make different p...A first-order question in the studies of the Solar System is how its outer zone known as the Kuiper belt was created and evolved.Two end-member models, involving coagulation vs. streaming instability, make different predictions-testable by the cratering history of Kuiper Belt Objects(KBOs)-about the cumulative size-frequency distribution(SFD) of the KBOs. Among all of the imaged KBOs, Pluto’s largest icy moon, Charon, appears to preserve the largest size range of seemingly undisturbed craters, their diameters(D) on Charon ranging from < 1 km to > 220 km. Current work shows that Charon’s craters with D < 10-20 km are fewer than those expected by the coagulation mechanism, but whether this is an artifact of post-cratering modification of smaller craters is unknown. We address this issue by conducting systematic photogeological mapping and performing detailed landform analysis using the highest resolution images obtained by the New Horizons spacecraft, which reveal a range of differentiable terrains on Charon. The most important findings of our work include(1) truncation and obliteration of large craters(diameters > 30-40 km) and their crater rim ridges along the eastern edges of several north-trending, eastward-convex, arcuate ranges in Oz Terra of the northern encountered hemisphere,(2) lobate ridges, lobate knob trains, and lobate aprons resembling glacial moraine landforms on Earth,(3) dendritic channel systems containing hanging valleys,and(4) locally striated surfaces defined by parallel ridges, knob trains, and grooves that are > 40-50 km in length. The above observations and the topographic dichotomy of Charon’s encountered hemisphere can be explained by a landscape-evolution model that involves(i)a giant impact that created the Vulcan Planitia basin and the extensional fault zone along its northern rim,(ii) a transient atmosphere capable of driving N2-ice glacial erosion of the water-ice bedrock and transporting water-ice debris to sedimentary basins,(iii) regional glacial erosion and transport of ear展开更多
We analyze ten of the longest (127 to 230 year-long) time series of European daily temperatures available from five different Köppen-Geiger climate classes. We split these according to the level of solar cycl...We analyze ten of the longest (127 to 230 year-long) time series of European daily temperatures available from five different Köppen-Geiger climate classes. We split these according to the level of solar cycle activity (H for “higher than median” and L for “lower than median”). This reveals coherent patterns in the temperature differences: when TH-TL?are stacked according to their calendar date, the daily averages from January 1 to December 31st disclose characteristic features in addition to the dominant annual seasonal wave, namely variations up to 2°C lasting for about 1.5 to 3 months. The five observatories at intermediate latitudes in a band from Oxford in the West to Prague in the East (same climate class) have very similar signatures. These similarities are most unlikely to be due to pure chance (confirmed by confidence levels in excess of 99% with the Kolmogorov-Smirnov and Kuiper nonparametric tests). The TH-TL patterns carry a regional signature, modulated by a more local response function. On the other hand, northern European observatories (St Petersburg and Arkhangelsk), those south of the Alps (Milan and Bologna), and the easternmost one in Astrakhan, corresponding to different climate classes, have different signatures. Similarly, preliminary study of long air pressure recordings confirms what emerges from the analysis of temperatures. These new observations lead us to conclude that the climate in different regions presents different responses to variations in solar activity. Moreover, the distributions of the lower, middle, and higher quartiles of the temperature and pressure indices in solar cycles with high versus low activity are significantly different, providing further robust statistical confirmation to this conclusion (confidence level higher to much higher than 99% using the Kuiper test).展开更多
A quantum-like model of gravitational system is introduced to explore the formation of the solar system structure. In this model, the chaos behavior of a large number of original nebular particles in a gravitational f...A quantum-like model of gravitational system is introduced to explore the formation of the solar system structure. In this model, the chaos behavior of a large number of original nebular particles in a gravitational field can be described in terms of the wave function satisfying formal Schr?dinger equation, in which the Planck constant is replaced by a constant on cosmic scale. Numerical calculation shows that the radial distribution density of the particles has the character of wave curves with decreasing amplitudes and elongating wavelengths. By means of this model, many questions of the solar system, such as the planetary distance, mass, energy, angular momentum, the distribution of satellites, the structure of the planetary rings, and the asteroid belt and the Kuiper belt etc., can be explained in reason. In addition, the abnormal rotations of Venus and Mercury can be naturally explained by means of the quantum-like model.展开更多
受地球大气影响,使用地基光学望远镜观测角距离较小的双星系统或主卫星系统时往往会出现星象不可分辨的情况.因此,系统光心位置与系统质心位置可能存在一定的偏差.准确地测量太阳系天体系统质心位置可以改进其轨道参数,有助于揭示太阳...受地球大气影响,使用地基光学望远镜观测角距离较小的双星系统或主卫星系统时往往会出现星象不可分辨的情况.因此,系统光心位置与系统质心位置可能存在一定的偏差.准确地测量太阳系天体系统质心位置可以改进其轨道参数,有助于揭示太阳系的形成与演化.以矮行星Haumea及其亮卫星Hi’iaka的运动为例,仿真系统光心围绕质心扰动的过程,探究视宁度(用星象的半高全宽表示)变化对准确测量光心位置的影响.仿真结果表明,使用二维高斯定心算法测定的系统光心位置随视宁度变化,而修正矩定心算法的定心结果不受视宁度的影响.根据仿真结果,研究能够有效减少视宁度变化对光心位置准确测量影响的定心算法十分必要;同时,新的定心算法还需考虑主星光度变化的影响.使用云南天文台2.4 m望远镜, 1 m望远镜以及紫金山天文台姚安观测站0.8 m望远镜从2022年2月7日至2022年5月25日观测矮行星Haumea系统,得到29晚共463幅CCD图像.新定心算法确定的光心位置与使用二维高斯定心算法的结果相比具有更好的位置拟合效果.此外,还发现亮卫星Hi’iaka在Jet Propulsion Laboratory (JPL)历表与Institut de Mécanique Céleste et de Calcul des éphémérides (IMCCE)历表中的位置存在较大偏差.展开更多
In this paper, a criterion on the C^0-sufficiency for a function germ with non-isolated singularity is obtained analogously to that of Kuiper-Kuo for the case of isolated singularities. Moreover, the Kuiper Kuo condit...In this paper, a criterion on the C^0-sufficiency for a function germ with non-isolated singularity is obtained analogously to that of Kuiper-Kuo for the case of isolated singularities. Moreover, the Kuiper Kuo condition and the Thom condition for an analytic function germ with non-isolated singularity are proved to be equivalent.展开更多
文摘Despite Pluto’s demotion to dwarf planet status,people are still attached to it.Scientists combined observations of Pluto from NASA’s New Horizons probe with observations of comet Churyumov-Gerasimenko from the European Space Agency’s Rosetta probe and found that Pluto’s nitrogen abundance matched the pattern of about a billion comets,which led to the theory that Pluto is made of about a billion comets.Yet they don’t know exactly when or where these comets originated.By studying the origin and orbit of comets,the author of this paper found that the material that condensed Pluto was mainly comets and dust ejected by Neptune,and the Kuiper Belt objects were condensed by material ejected by Neptune toward the outer side of its orbit.
基金funded partially by BRIN’s research grant Rumah Program AIBDTK 2023。
文摘We intend to study a modified version of the planar Circular Restricted Three-Body Problem(CRTBP) by incorporating several perturbing parameters. We consider the bigger primary as an oblate spheroid and emitting radiation while the small primary has an elongated body. We also consider the perturbation from a disk-like structure encompassing this three-body system. First, we develop a mathematical model of this modified CRTBP.We have found there exist five equilibrium points in this modified CRTBP model, where three of them are collinear and the other two are non-collinear. Second, we apply our modified CRTBP model to the Sun–Haumea system by considering several values of each perturbing parameter. Through our numerical investigation, we have discovered that the incorporation of perturbing parameters has resulted in a shift in the equilibrium point positions of the Sun–Haumea system compared to their positions in the classical CRTBP. The stability of equilibrium points is investigated. We have shown that the collinear equilibrium points are unstable and the stability of non-collinear equilibrium points depends on the mass parameter μ of the system. Unlike the classical case, non-collinear equilibrium points have both a maximum and minimum limit of μ for achieving stability. We remark that the stability range of μ in non-collinear equilibrium points depends on the perturbing parameters. In the context of the Sun–Haumea system, we have found that the non-collinear equilibrium points are stable.
基金Supported by the National Natural Science Foundation of Chinasupported by the Natural Science Foundation of China (NSFC+2 种基金Grant Nos. 10833001 and 11073012)the Qing Lan Project (Jiangsu Province)J. Li is also supported by the NSFC (Grant Nos. 1103008 and 11078001)
文摘The population of Neptune Trojans is believed to be bigger than that of Jupiter Trojans and that of asteroids in the main belt, although only eight members of this distant asteroid swarm have been observed up to now. Six leading Neptune Trojans around the Lagrange point L4 discovered earlier have been studied in detail, but two trailing ones found recently around the L5 point, 2004 KV18 and 2008 LC18, have not yet been investigated. We report our investigations on the dynamical behaviors of these two new Neptune Trojans. Our calculations show that the asteroid 2004 KV18 is a temporary Neptune Trojan. Most probably, it was captured into the trailing Trojan cloud no earlier than 2.03 ×105 yr ago, and it will not maintain this position later than 1.65 × 105 yr in the future. Based on the statistics from our orbital simulations, we ar- gue that this object is more like a scattered Kuiper belt object. By contrast, the orbit of 2008 LC18 is much more stable. Among the clone orbits spreading within the orbital uncertainties, a considerable portion of clones may survive on the L5 tadpole orbits for 4 Gyr. The strong dependence of the stability on the semimajor axis and resonant angle suggests that further observations are badly required to constrain the orbit in the stable region. We also discuss the implications of the existence and dynamics of these two trailing Trojans over the history of the solar system.
文摘Cometary nuclei, the remnant icy bodies of planet formation, located at the outer edge of the solar system, are relatively poorly studied because of their small sizes and thus faintness. Thus far more than a hundred large members (size about 100 km) of this cometary population in the Kuiper belt have been identified. Smaller bodies (10 km) are much too faint to image directly and their number so far can only be extrapolated on theoretical grounds. The Taiwan-America Occultation Survey (TAOS) will conduct a census of the number of Kuiper belt objects down to a few km size by monitoring chance stellar occultations by these cometary nuclei. We will set up an array of small (50cm), wide-field (f/1 9) telescopes, each equipped with a 2K squared CCD camera, along a 7 km baseline in central Taiwan at an elevation above ～ 3000 m. The robot telescopes will operate in a coincidence mode, so the sequence and timing of any candidate occultation event can be recorded and distinguished against a false detection. The Lawrence Livermore National Laboratory, the National Central University, and the Academia Sinica, will each contribute one telescope system. Researchers from an international variety of institutes are also participating in the project. Our experiment provides the only means to study the cometary population in the small-sized end of the distrbution. A great number of scientific byproducts, notably variable stars, will also derive from the huge TAOS database, some 10, 000 giga-bytes worth of photometrical measuremements per year.
基金Supported by the National Natural Science Foundation of China.
文摘The orbital migration of Jovian planets is believed to have played an important role in shaping the Kuiper Belt. We investigate the effects of the long time-scale （2 ×107 yr） migration of Jovian planets on the orbital evolution of massless test particles that are initially located beyond 28 AU. Because of the slowness of the migration, Neptune＇s mean motion resonances capture test particles very efficiently. Taking into account the stochastic behavior during the planetary migration and for proper parameter values, the resulting concentration of objects in the 3：2 resonance is prominent, while very few objects enter the 2：1 resonance, thus matching the observed Kuiper Belt objects very well. We also find that such a long time-scale migration is favorable for exciting the inclinations of the test particles, because it makes the secular resonance possible to operate during the migration. Our analyses show that the us secular resonance excites the eccentricities of some test particles, so decreasing their perihelion distances, leading to close encounters with Neptune, which can then pump the inclinations up to 20°.
文摘A first-order question in the studies of the Solar System is how its outer zone known as the Kuiper belt was created and evolved.Two end-member models, involving coagulation vs. streaming instability, make different predictions-testable by the cratering history of Kuiper Belt Objects(KBOs)-about the cumulative size-frequency distribution(SFD) of the KBOs. Among all of the imaged KBOs, Pluto’s largest icy moon, Charon, appears to preserve the largest size range of seemingly undisturbed craters, their diameters(D) on Charon ranging from < 1 km to > 220 km. Current work shows that Charon’s craters with D < 10-20 km are fewer than those expected by the coagulation mechanism, but whether this is an artifact of post-cratering modification of smaller craters is unknown. We address this issue by conducting systematic photogeological mapping and performing detailed landform analysis using the highest resolution images obtained by the New Horizons spacecraft, which reveal a range of differentiable terrains on Charon. The most important findings of our work include(1) truncation and obliteration of large craters(diameters > 30-40 km) and their crater rim ridges along the eastern edges of several north-trending, eastward-convex, arcuate ranges in Oz Terra of the northern encountered hemisphere,(2) lobate ridges, lobate knob trains, and lobate aprons resembling glacial moraine landforms on Earth,(3) dendritic channel systems containing hanging valleys,and(4) locally striated surfaces defined by parallel ridges, knob trains, and grooves that are > 40-50 km in length. The above observations and the topographic dichotomy of Charon’s encountered hemisphere can be explained by a landscape-evolution model that involves(i)a giant impact that created the Vulcan Planitia basin and the extensional fault zone along its northern rim,(ii) a transient atmosphere capable of driving N2-ice glacial erosion of the water-ice bedrock and transporting water-ice debris to sedimentary basins,(iii) regional glacial erosion and transport of ear
文摘We analyze ten of the longest (127 to 230 year-long) time series of European daily temperatures available from five different Köppen-Geiger climate classes. We split these according to the level of solar cycle activity (H for “higher than median” and L for “lower than median”). This reveals coherent patterns in the temperature differences: when TH-TL?are stacked according to their calendar date, the daily averages from January 1 to December 31st disclose characteristic features in addition to the dominant annual seasonal wave, namely variations up to 2°C lasting for about 1.5 to 3 months. The five observatories at intermediate latitudes in a band from Oxford in the West to Prague in the East (same climate class) have very similar signatures. These similarities are most unlikely to be due to pure chance (confirmed by confidence levels in excess of 99% with the Kolmogorov-Smirnov and Kuiper nonparametric tests). The TH-TL patterns carry a regional signature, modulated by a more local response function. On the other hand, northern European observatories (St Petersburg and Arkhangelsk), those south of the Alps (Milan and Bologna), and the easternmost one in Astrakhan, corresponding to different climate classes, have different signatures. Similarly, preliminary study of long air pressure recordings confirms what emerges from the analysis of temperatures. These new observations lead us to conclude that the climate in different regions presents different responses to variations in solar activity. Moreover, the distributions of the lower, middle, and higher quartiles of the temperature and pressure indices in solar cycles with high versus low activity are significantly different, providing further robust statistical confirmation to this conclusion (confidence level higher to much higher than 99% using the Kuiper test).
文摘A quantum-like model of gravitational system is introduced to explore the formation of the solar system structure. In this model, the chaos behavior of a large number of original nebular particles in a gravitational field can be described in terms of the wave function satisfying formal Schr?dinger equation, in which the Planck constant is replaced by a constant on cosmic scale. Numerical calculation shows that the radial distribution density of the particles has the character of wave curves with decreasing amplitudes and elongating wavelengths. By means of this model, many questions of the solar system, such as the planetary distance, mass, energy, angular momentum, the distribution of satellites, the structure of the planetary rings, and the asteroid belt and the Kuiper belt etc., can be explained in reason. In addition, the abnormal rotations of Venus and Mercury can be naturally explained by means of the quantum-like model.
文摘受地球大气影响,使用地基光学望远镜观测角距离较小的双星系统或主卫星系统时往往会出现星象不可分辨的情况.因此,系统光心位置与系统质心位置可能存在一定的偏差.准确地测量太阳系天体系统质心位置可以改进其轨道参数,有助于揭示太阳系的形成与演化.以矮行星Haumea及其亮卫星Hi’iaka的运动为例,仿真系统光心围绕质心扰动的过程,探究视宁度(用星象的半高全宽表示)变化对准确测量光心位置的影响.仿真结果表明,使用二维高斯定心算法测定的系统光心位置随视宁度变化,而修正矩定心算法的定心结果不受视宁度的影响.根据仿真结果,研究能够有效减少视宁度变化对光心位置准确测量影响的定心算法十分必要;同时,新的定心算法还需考虑主星光度变化的影响.使用云南天文台2.4 m望远镜, 1 m望远镜以及紫金山天文台姚安观测站0.8 m望远镜从2022年2月7日至2022年5月25日观测矮行星Haumea系统,得到29晚共463幅CCD图像.新定心算法确定的光心位置与使用二维高斯定心算法的结果相比具有更好的位置拟合效果.此外,还发现亮卫星Hi’iaka在Jet Propulsion Laboratory (JPL)历表与Institut de Mécanique Céleste et de Calcul des éphémérides (IMCCE)历表中的位置存在较大偏差.
文摘In this paper, a criterion on the C^0-sufficiency for a function germ with non-isolated singularity is obtained analogously to that of Kuiper-Kuo for the case of isolated singularities. Moreover, the Kuiper Kuo condition and the Thom condition for an analytic function germ with non-isolated singularity are proved to be equivalent.
