SIXTEEN YEARS OF ULYSSES INTERSTELLAR DUST

SIXTEEN YEARS OF ULYSSES INTERSTELLAR DUST MEASUREMENTS IN THE SOLAR SYSTEM. I. MASS DISTRIBUTION AND GAS-TO-DUST MASS RATIO Harald Krüger1, Peter Strub1, Eberhard Grün2,3, and Veerle J. Sterken3,4 1 Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077 Göttingen, Germany;

The distribution of mass in the planetary system and solar nebula

A model ''solar nebula'' is constructed by adding the solar complement of light elements to each planet, using recent models of planetary compositions. Uncertainties in this approach are estimated. The computed surface density varies approximately asr −3/2. Mercury, Mars and the asteroid belt are anomalously low in mass, but processes exist which would preferentially

Mass distribution of the solar system

Mass distribution in the solar system 1971, Astrophysics and Space Science This paper presents the results of one phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under Contract No. NAS 7-100, sponsored by the National Aeronautics and Space Administration.

Solar System evolution from compositional mapping of the

Migration models began by explaining the orbital structure and mass distribution of the outer Solar System, including the Kuiper belt past Neptune 50. Individual models could successfully recreate

The distribution of mass in the planetary system and solar nebula

A model ''solar nebula'' is constructed by adding the solar complement of light elements to each planet, using recent models of planetary compositions. Uncertainties in this approach are estimated. The computed surface density varies approximately asr−3/2. Mercury, Mars and the asteroid belt are anomalously low in mass, but processes exist which would preferentially

Interstellar Dust In The Solar System | SpringerLink

We deduce the mass distribution and total mass density of interstellar dust streaming into the solar system and compare the results to the conditions of the very local interstellar medium (VLISM). The mass distribution derived from in situ measurements shows a...

DarkMatter inthe Solar System

DarkMatter inthe Solar System X. Xu∗ and E. R. Siegel† Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721 (Dated: October 24, 2018) We determine the density and mass distribution of dark matter within our Solar System. We explore the three-body interactions between dark matter particles, the Sun, and the planets to

Distribution of Matter in the Solar System

Theoretical and observed distribution of mass in the solar system. 9 1 X mk = 2669 × 10 Kg ; hv i = mk vk2 = 149.33 (Km s−1 )2 m0 = m 0 k=1 k=1 9 X 24 2 α = GM/hv 2 i = 888.73 × 106 Km. (13) Secondly, we introduce an equilibrium point between each pair of two subsequent planets a, b in such a way that the forces of gravity of the planets

Solar System Facts

Our solar system has hundreds of moons orbiting planets, dwarf planets, and asteroids. Of the eight planets, Mercury and Venus are the only ones with no moons, although Venus does have a quasi-satellite that has officially been

Solved What do you think the mass distribution of the solar

To answer this question, start by considering the composition of the Solar System, which consists of one star (the Sun) and several smaller planets, and how this differs from larger systems like galaxies for which the rotation curve method is typically used.

8.4: Velocity and Mass Distributions in Galaxies

We looked in detail at how mass can be modeled in the Solar System, and how the Solar System rotates (or in other words, how the planets orbit the Sun) due to gravity. are distributed. The distribution of mass that goes with this curve is the one in which mass is evenly spread out; refer to the models from Section 8.3,. However, the

THE MASS DISTRIBUTION FUNCTION OF PLANETS

THE MASS DISTRIBUTION FUNCTION OF PLANETS Renu Malhotra Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USA; [email protected] The black points indicate the masses of the solar system planets. Note that this is a semi-log plot. Figure 2. Period ratio distribution in multiple-planet systems discovered by

Metal distribution in our solar system

The metal content of the Solar system is completely dominated by the Sun. The Sun contains $sim1%$ of ''metals'' (in astronomical language anything but hydrogen and helium is a ''metal''), but all the other bodies of the Solar system combined have less mass than that.

[0806.3767] Dark Matter in the Solar System

We determine the density and mass distribution of dark matter within our Solar System. We explore the three-body interactions between dark matter particles, the Sun, and the planets to compute the amount of dark matter gravitationally captured over the lifetime of the Solar System. We provide an analytical framework for performing these calculations and detail our

Milky Way

The Milky Way [c] is the galaxy that includes the Solar System, with the name describing the galaxy''s appearance from Earth: a hazy band of light seen in the night sky formed from stars that cannot be individually distinguished by the naked eye.. The Milky Way is a barred spiral galaxy with a D 25 isophotal diameter estimated at 26.8 ± 1.1 kiloparsecs (87,400 ± 3,600 light-years),

The Solar System

Composition Of The Solar System The Sun contains 99.85% of all the matter in the Solar System. The planets, which condensed out of the same disk of material that formed the Sun, contain only 0.135% of the mass of the solar system. Jupiter contains more than twice the matter of all the other planets combined.

SIXTEEN YEARS OF ULYSSES INTERSTELLAR DUST MEASUREMENTS IN THE SOLAR

We now consider the contributions of grains with different masses to the overall mass density of interstellar dust in the solar system. In Figure 6 we show the mass distribution of interstellar grains as the differential mass density per unit

MASS DISTRIBUTION AND PLANET FORMATION IN THE

characteristics of the solar system (discussed in x 2.1) by posit-ing that the giant planets formed between 5 and 15 AU rather than from 5 to 30AU. If true, this means that theMMSN model SOLAR NEBULA MASS DISTRIBUTION 879. Jupiter and Saturn crossed their mutual 2:1 MMR, causing cha-otic behavior in the outer solar system for several tens

grains in the solar system from in situ measurements

the shape of the extinction curve is sensitive to the mass distribution of dust grains that cause the extinction, the mass distribution can be determined, in part, by fitting the wavelength dependence of extinction [Mathis et al., 1977; Kim et al., 1994; Li and Greenberg, 1997]. These models of the mass distribution and composition of in-

Mass Distribution in the Solar System. Mass (Md) that is enclosed

Finally, the values of time coefficient of metric (g 00 ) have been calculated from (24) for ξ I =1. In addition, the corresponding Rotation Curves and Mass Distribution in the Solar System are

Aspects of the Mass Distribution of Interstellar Dust Grains in the

The in-situ detection of interstellar dust grains in the Solar System by the dust instruments on-board the Ulysses and Galileo spacecraft as well as the recent measurements of hyperbolic radar

THE MASS DISTRIBUTION FUNCTION OF PLANETS

The distribution of orbital period ratios of adjacent planets in extrasolar planetary systems discovered by the Kepler space telescope exhibits a peak near ∼1.5–2, a long tail of larger period ratios, and a steep drop-off in the number of systems with period ratios below ∼1.5. We find from these data that the dimensionless orbital separations have an approximately log

Aspects of the mass distribution of interstellar dust grains in the

The in situ detection of interstellar dust grains in the solar system by the dust instruments on-board the Ulysses and Galileo spacecraft as well as the recent measurements of hyperbolic radar meteors give information on the properties of the interstellar solid particle population in the solar vicinity. Especially the distribution of grain masses is indicative of growth and destruction

A question about the distribution of mass among the planets in

First, Pluto isn''t a planet, and hasn''t been for about a decade. It''s a dwarf planet, and is better grouped with other small, rocky objects beyond Neptune''s orbit, such as Haumea.These objects, and other minor planets, have more in common with objects in the Kuiper Belt and Oort Cloud than the eight planets of the Solar System. 1 Therefore, we see a different

Distribution of Matter in the Solar System

A new formula for the distribution of matter in the solar system is derived by assuming that the planets were formed from trapped particles of a cosmic dust disk attached to the Sun. Contrary to Boltzmann''s distribution which predicts thermal collapse of this cloud on the Sun, it is found that if the primeval particles move on circular orbits

Mass inventory of the giant-planet formation zone in a solar

The initial mass distribution in the solar nebula is a critical input to planet formation models that seek to reproduce today''s Solar System 1.Traditionally, constraints on the gas mass

Solar System

OverviewTrans-Neptunian regionFormation and evolutionGeneral characteristicsSunInner Solar SystemOuter Solar SystemMiscellaneous populations

Beyond the orbit of Neptune lies the area of the "trans-Neptunian region", with the doughnut-shaped Kuiper belt, home of Pluto and several other dwarf planets, and an overlapping disc of scattered objects, which is tilted toward the plane of the Solar System and reaches much further out than the Kuiper belt. The entire region is still largely unexplored. It appears to consist overwhelming

The Distribution of Mass in the Planetary System and Solar Nebula

A model ''solar nebula'' is constructed by adding the solar complement of light elements to each planet, using recent models of planetary compositions. Uncertainties in this approach are estimated. The computed surface density varies approximately asr ‑3/2 . Mercury, Mars and the asteroid belt are anomalously low in mass, but processes exist which would preferentially

Solar Elemental Abundances

percent of the mass in the solar system and therefore the composition of the sun is a good proxy for the composition of the overall solar system. The solar system composition can be taken as the overall composition of the molecular cloud within the interstellar medium from which the solar system formed 4.567 billion years ago.

The Dependence of the Mass Distribution of Exoplanets on the

Abstract We analyze the mass distributions of exoplanets of three groups: transit planets discovered by the Kepler telescope, those found in ground-based observational programs and with the CoRoT satellite, and planets discovered in the vicinity of red dwarfs (M class) with the radial-velocity method. The dependence of the mass distributions of the Kepler transit