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is located within the milky way
revolves around the galactic center once 240 million years
it includes, the sun, planets, moons, asteroids, comets, gasses, solar wind.
OBJECTIVE:
Identify the large scale and small scale properties of the Solar System.
LARGE SCALE AND SMALL SCALE PROPERTIES OF SOLAR SYSTEM
Large Scale Features of Solar System
Large Scale Features of Solar System
1. Much mass of the solar system is concentrated at the center (sun) while angular momentum is held by the outer planets .
2.Orbits of the planets are elliptical and on the sample.
3. All planets revolve around the sun .
4.The periods of revolution of planets increase with the increasing distance from the sun.
5. All planets are located at the regular intervals from the sun.
Small Scale Features of Solar System
1.Most of the planets rotate prograde .
2. Terrestrial planets have :
high densities
thin or no atmosphere
rotate slowly
rocky materials such as silicates, iron, and nickel of high melting points.
3. Jovian Planets have:
low densities thick atmospheres
rotate rapidly
many natural satellites .
4. Most of outer Solar System objects are ice-rich.
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jennifer.mp4
The Different Hypotheses Explaining the Origin of the Solar System
Learning Objectives:
Describe the different hypotheses of the origin of the solar system; and
Explain the different hypotheses of the origin of the solar system.
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Georges Leclerc and Comte de Buffon
Who proposed the Encounter Hypothesis
Encounter Hypothesis
One of the earliest theories for the formation of the planets.
A rogue star passes close to the Sun about 5 billion years ago. Material, in the form of hot gas, is tidally stripped from the Sun and the rogue star. This material fragments into smaller lumps which form the planets. This hypothesis has the advantage of explaining why the planets all revolve in the same direction (from the encounter geometry) and also provides an explanation for why the inner worlds are denser than the outer worlds.
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Emanuel Swedenborg
Who proposed the Nebular Hypothesis
Nebular Hypothesis
The idea that a spinning cloud of dust made of mostly light elements, called a nebula, flattened into a protoplanetary disk, and became a solar system consisting of a star with orbiting planets.
This states that the solar system developed out of an interstellar cloud of dust and gas, called a nebula, most likely left over from a previous supernova. The nebula started to collapse and condense; this collapsing process continued for some time. The Sun-to-be collected most of the mass in the nebula’s center, forming a Protostar . The nebula flattened into a disk called the Protoplanetary Disk ; planets eventually formed from and in this disk.
Three processes occurred with the nebular collapse:
1. Temperatures continued to increase
2. The solar nebula spun faster and faster
3. The solar nebula disk flattened
The orderly motions of the solar system today are a direct result of the solar system’s beginnings in a spinning, flattened cloud of gas and dust.
Nebular Hypothesis
A nebula is an enormous cloud of dust and gas occupying the space between stars and acting as a nursery for new stars. The roots of the word come from Latin nebula, which means a “mist, vapor, fog, smoke, exhalation.” Nebulae are made up of dust, basic elements such as hydrogen and other ionized gases
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William McCrea
Who proposed the Protoplanet Hypothesis
IIt has been found that rapidly rotating nebulas will develop large whirlpools or vortexes at various places on the disk of nebular material. Each of these great whirlpools might then have collected the surrounding material by gravitational attraction, thus forming a protoplanet
It is believed that nine protoplanets –one for each of the present-day planets—were formed, and these were originally much larger than the finished planet. Smaller whirlpools developed inside some of the larger vortexes, and these gave rise to spinning discs that became the satellites, or moons, of the planets
Protoplanet Hypothesis
The hypothesis essentially says that very small objects stuck to each other and grew bigger and bigger — big enough to even form the gas giants, such as Jupiter.
The Chamberlin-Moulton planetesimal hypothesis is a catastrophic hypothesis, proposed by Thomas Chamberlin and Forest Moulton in 1905, in which the planets of the Solar System are seen to arise from an encounter between the Sun and another star. In this scenario, the gravity of the passing star tears a succession of bolts from the solar surface. Bolts coming from the side nearer the star are thrown out to distances comparable with those of the giant plants, while those from the far side of the Sun are ejected less violently to the distances of the terrestrial planets. From the inner remains of these bolts formed the initial cores of the planets. The outer parts expanded and cooled into a huge swarm of solid particles spread out in a disk rotating about the Sun in a plane determined by the motion of the passing star. The cores gradually grew into planets by gathering in the planetesimals, most of the growth taking place in the outer parts of the Solar System where material was more plentiful.
Planetesimal Hypothesis
Planetesimal Hypothesis
The hypothesis was based on the idea that a star passed close enough to the sun early in its life to cause tidal bulges to form on its surface, which along with the internal process that leads to solar prominences, caused material to be ejected repeatedly from the sun. Due to the gravitational effects of the passing star, two spiral-like arms would have extended from the sun, and while most of the material would have fallen back, part of it would remain in orbit. This orbiting material would cool and condense into numerous small bodies that they termed planetesimals and a few larger protoplanets. .
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