scholarly journals How many interstellar visitors are there in the Solar System?

2021 ◽  
pp. 16-21
Author(s):  
Б.М. Шустов
Keyword(s):  
Particle Size ◽  
Solar System ◽  
Interstellar Dust ◽  
Particle Flux ◽  
Dynamic Evolution ◽  
Small Bodies ◽  
The Earth ◽  
Total Particle ◽  
The Masses ◽  
The Relationship

По результатам краткого обзора наблюдений вошедших в Солнечную систему межзвездных пылинок, метеороидов и более крупных тел и на основе моделей, описывающих спектры масс таких тел, отмечен огромный разброс (много порядков величины) в оценках отношения η потока межзвездных частиц к общему потоку частиц в окрестности Земли и в целом в Солнечной системе. Этот разброс означает, что современные возможности не позволяют определенно ответить на вопрос в заголовке статьи. При анализе результатов наблюдений необходимо учитывать характер зависимости отношения η от размера частиц r, т. е. η(r). Эта зависимость определяется процессами генерации и динамической эволюции населения малых тел в Солнечной системе и за ее пределами. According to the results of a brief review of observations included in the Solar system, interstellar dust, meteoroids and larger bodies, and on the basis of models describing the spectra of the masses of these bodies, we mark a huge spread (many orders of magnitude) in estimates of the relationship η of the flow of interstellar particles to the total particle flux near the Earth and in the whole Solar system. These differences mean that modern capabilities do not allow us to definitely answer the question in the title of the article. When analyzing the results of observations, it is necessary to take into account the nature of the dependence of the ratio η on the particle size r, i.e. η(r). This dependence is determined by the processes of generation and dynamic evolution of the population of small bodies in the Solar system and beyond.

scholarly journals The Contribution of Kuiper Belt Dust Grains to the Inner Solar System

1996 ◽  
Vol 150 ◽  
pp. 163-166
Author(s):  
Jer-Chyi Liou ◽  
Herbert A. Zook ◽  
Stanley F. Dermott
Keyword(s):  
Solar System ◽  
Interstellar Dust ◽  
Numerical Study ◽  
Kuiper Belt ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Dust Grains ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
The Earth

AbstractThe recent discovery of the so-called Kuiper belt objects has prompted the idea that these objects produce dust grains that may contribute significantly to the interplanetary dust population at 1 AU. We have completed a numerical study of the orbital evolution of dust grains, of diameters 1 to 9 μm, that originate in the region of the Kuiper belt. Our results show that about 80% of the grains are ejected from the Solar System by the giant planets while the remaining 20% of the grains evolve all the way to the Sun. Surprisingly, these dust grains have small orbital eccentricities and inclinations when they cross the orbit of the Earth. This makes them behave more like asteroidal than cometary-type dust particles. This also enhances their chances to be captured by the Earth and makes them a possible source of the collected interplanetary dust particles (IDPs); in particular, they represent a possible source that brings primitive/organic materials from the outer Solar System to the Earth.When collisions with interstellar dust grains are considered, however, Kuiper belt dust grains larger than about 9 μm appear likely to be collisionally shattered before they can evolve to the inner part of the Solar System. Therefore, Kuiper belt dust grains may not, as they are expected to be small, contribute significantly to the zodiacal light.

scholarly journals Sources of Interplanetary Dust

1996 ◽  
Vol 150 ◽  
pp. 141-153 ◽  
Author(s):  
S.F. Dermott ◽  
K. Grogan ◽  
B.Å.S. Gustafson ◽  
S. Jayaraman ◽  
S.J. Kortenkamp ◽  
...  
Keyword(s):  
Solar System ◽  
Interstellar Dust ◽  
Large Scale ◽  
Thermal Flux ◽  
Interplanetary Dust ◽  
Scale Height ◽  
Size Frequency Distribution ◽  
Zodiacal Cloud ◽  
The Earth ◽  
Characteristic Features

AbstractAsteroids, comets and interstellar dust are possible sources of the particles that constitute the dust in the inner solar system. Each of these components gives rise to particular, characteristic features, the amplitudes of which can be used to estimate the size of the associated source. The asteroidal component feeds the dust bands and the Earth's resonant ring, while the cometary component may account for the large scale height of the zodiacal cloud observed at 1 AU Previous discussions of the observed strengths of these various features indicated that the source of about one third of the thermal flux observed, for example, in the IRAS 25μm waveband is asteroidal, while two thirds is cometary. However, a variety of assumptions go into this calculation (the size-frequency distribution of the particles is particularly significant) and we now know that the result is highly dependent on these assumptions. The zodiacal cloud is also the source of the IDPs collected on Earth. Because of strong gravitational focusing by the Earth of particles in low e and I orbits, it is probable that the majority of IDPs originate from asteroids, particularly those asteroids in the Themis and Koronis families.

Calculation and visualization of distortions in morphographic projections

2019 ◽  
Vol 945 (3) ◽  
pp. 26-36
Author(s):  
M.V. Nyrtsov ◽  
A.A. Domatieva
Keyword(s):  
Solar System ◽  
Celestial Body ◽  
Spherical Shape ◽  
Irregular Shape ◽  
Triaxial Ellipsoid ◽  
Reference Surface ◽  
Small Bodies ◽  
The Earth ◽  
Regular Shape

There are different ways of estimating the distortions that help us find the best cartographic projections and recommend them for a specific range of tasks from mapping the Earth to extraterrestrial mapping. Besides the planets and their satellites there are small bodies in the Solar System. For mapping these bodies it is advisable to use morphographic projections to show their non-spherical shape. These projections were developed by Philip Stooke. He also proposed replacement of a regular reference surface with a phoboid and methods for estimating distortions but practically implemented them on the example of a body with a regular shape approximated by test triaxial ellipsoid with a ratio of axes 4:3:2. In this regard we set the task of developing and implementing the method for determining distortions in morphographic projections for a body with an irregular shape. We used the algorithm of comparison cartographic cell on projection and on phoboid in order to estimate distortion. The object of mapping is Phobos, a satellite of Mars. Phobos is a non-spherical celestial body for which morphographic projections were first applied. Comparing our results by the values of distortions with the results obtained by Philip Stooke we can conclude that using morphographic projections makes less distortion at portraying a phoboid than a test triaxial ellipsoid.

scholarly journals On secular resonances of small bodies in the planetary systems

2006 ◽  
Vol 2 (S236) ◽  
pp. 77-84
Author(s):  
Jianghui Ji ◽  
L. Liu ◽  
G. Y. Li
Keyword(s):  
Solar System ◽  
Planetary System ◽  
Planetary Systems ◽  
Giant Planets ◽  
Small Bodies ◽  
Secular Resonances ◽  
Mean Motion Resonances ◽  
The Earth ◽  
Habitable Zones ◽  
Earth Like Planets

AbstractWe investigate the secular resonances for massless small bodies and Earth-like planets in several planetary systems. We further compare the results with those of Solar System. For example, in the GJ 876 planetary system, we show that the secular resonances ν1 and ν2 (respectively, resulting from the inner and outer giant planets) can excite the eccentricities of the Earth-like planets with orbits 0.21≤ a <0.50 AU and eject them out of the system in a short timescale. However, in a dynamical sense, the potential zones for the existence of Earth-like planets are in the area 0.50≤ a ≤1.00 AU, and there exist all stable orbits last up to 105 yr with low eccentricities. For other systems, e.g., 47 UMa, we also show that the Habitable Zones for Earth-like planets are related to both secular resonances and mean motion resonances in the systems.

scholarly journals From Discovery to Impact - Near Earth Asteroids

2012 ◽  
Vol 8 ◽  
pp. 73-78
Author(s):  
Miloš Tichý ◽  
Michaela Honková ◽  
Jana Tichá ◽  
Michal Kočer
Keyword(s):  
Solar System ◽  
Current System ◽  
Small Bodies ◽  
Impact Site ◽  
The Earth ◽  
Near Earth Asteroids ◽  
Near Earth Objects

The Near-Earth Objects (NEOs) are the most important of the small bodies of the solar system, having the capability of close approaches to the Earth and the chance to collide with the Earth.  We present here the current system of discovery of these dangerous objects, standards for selecting useful and important targets for NEO follow-up astrometry, system of impact probabilities calculations, and also determination of impact site and evacuation area.

scholarly journals Mapping the location of terrestrial impacts and extinctions onto the spiral arm structure of the Milky Way

2018 ◽  
Vol 18 (4) ◽  
pp. 323-328 ◽  
Author(s):  
Michael P Gillman ◽  
Hilary E Erenler ◽  
Phil J Sutton
Keyword(s):  
Solar System ◽  
Relative Importance ◽  
Star Formation Region ◽  
Spiral Arms ◽  
The Earth ◽  
Robust Model ◽  
Methanol Masers ◽  
Life On Earth ◽  
The Relationship ◽  
Spiral Arm

AbstractHigh-density regions within the spiral arms are expected to have profound effects on passing stars. Understanding of the potential effects on the Earth and our Solar System is dependent on a robust model of arm passage dynamics. Using a novel combination of data, we derive a model of the timings of the Solar System through the spiral arms and the relationship to arm tracers such as methanol masers. This reveals that asteroid/comet impacts are significantly clustered near the spiral arms and within specific locations of an average arm structure. The end-Permian and end-Cretaceous extinctions emerge as being located within a small star-formation region in two different arms. The start of the Solar System, greater than 4.5 Ga, occurs in the same region in a third arm. The model complements geo-chemical data in determining the relative importance of extra-Solar events in the diversification and extinction of life on Earth.

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