The basic premise in the understanding of our origins, and the properties of all the planets we have studied this term, is that natural forces created and shaped the Solar System. And that there is a continuity to that process, i.e. it is not a sequence of random events.Any model or theory for the formation of the Solar System must have a set of explanations for large-scale and small-scale properties. Large-Scale:
the planets are isolated in orderly intervals
orbits are nearly circular
orbits are in the same plane
all planets revolve prograde
Any model or theory for the formation of the Solar System must have a set of explanations for large-scale and small-scale properties. Large-Scale:
- the planets are isolated in orderly intervals
- orbits are nearly circular
- orbits are in the same plane
- all planets revolve prograde
Small-Scale:
- most planets rotate prograde
- the systems of moons can be divided into regular objects (spherical) with direct orbits versus irregular objects with eccentric orbits
- terrestrial planets have
- high densities
- thin or no atmospheres
- rotate slowly
- rocky, poor in ices and H/He
- jovian worlds have
- low densities
- thick atmospheres
- rotate rapidly
- many moons
- fluid interiors, rich in ices, H/He
- most of outer SS objects (not just jovian worlds) are ice-rich
Also note that the overall architecture of our Solar System is orderly and the ages of its members uniform. All indicators point to a single formation event about 4.6 billion years ago. The above is not to ignore the fact that a great deal of evolution occurred in the Solar System after it formed (see below). For example, the origin secondary atmospheres of the terrestrial worlds underwent a large amount of chemical processing (Venus was baked, Mars was frozen, Earth developed life). There was also orbital evolution as well, rings were formed, moons captured, tidal locking between worlds (e.g. Pluto and Charon). So the Solar System is not a static system, it is dynamic.
How does one test a hypothesis?
To answer scientific questions requires the formulation of a hypothesis. The hypothesis is tested against the facts to look for contradictions that rule out or require modification to the hypothesis. Note that the process of hypothesis formulation and then theory building is a lengthy, career dependent operation. So the sociology of science requires that a hypothesis be tested and confirmed by many scientists since the creator of the hypothesis has a strong psychological attachment to his work.
Encounter Hypothesis:
One of the earliest theories for the formation of the planets was called the encounter hypothesis. In this scenario, 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.
However, there are two major problems for a theory of this type. One is that hot gas expands, not contracts. So lumps of hot gas would not form planets. The second is that encounters between stars are extremely rare, so rare as to be improbable in the lifetime of the Universe (15 billion years).
Nebular Hypothesis:
A second theory is called the nebular hypothesis. In this theory, the whole Solar System starts as a large cloud of gas that contracts under self-gravity. Conservation of angular momentum requires that a rotating disk form with a large concentration at the center (the proto-Sun). Within the disk, planets form.
Nebular Hypothesis:
A second theory is called the nebular hypothesis. In this theory, the whole Solar System starts as a large cloud of gas that contracts under self-gravity. Conservation of angular momentum requires that a rotating disk form with a large concentration at the center (the proto-Sun). Within the disk, planets form.
While this theory incorporates more basic physics, there are several unsolved problems. For example, a majority of the angular momentum in the Solar System is held by the outer planets. For comparison, 99% of the Solar System's mass is in the Sun, but 99% of its angular momentum is in the planets. Another flaw is the mechanism from which the disk turns into individual planets.
Protoplanet Hypothesis:
The current working model for the formation of the Solar System is called the protoplanet hypothesis. It incorporates many of the components of the nebular hypothesis, but adds some new aspects from modern knowledge of fluids and states of matter.
Protoplanet Hypothesis:
The current working model for the formation of the Solar System is called the protoplanet hypothesis. It incorporates many of the components of the nebular hypothesis, but adds some new aspects from modern knowledge of fluids and states of matter.
Meanwhile in the inner Solar System:
Note that as the planet's began to form they grew in mass by accreting planetesimals. Since force of gravity is proportional to mass, the largest planetesimals are accreted first. The early proto-planets are able to sweep the early Solar System clean of large bodies. Notice also that the lighter compounds are vaporized in the inner Solar System. So where did all the outgassing material come from? The answer is comets that fall from the outer Solar System after the planets form.
Meanwhile in the outer Solar System:
The Jovian worlds, having an early edge on gathering mass in the colder outer solar disk, were the most efficient at capturing planetesimals, which only served to increase their already large masses. As the planetesimals shrink in average size, collisions with proto-planets lead to fragmentation. So quickly the Solar System divided into large proto-planets and smaller and smaller planetesimals which eventually became the numerous meteors we see today. Any leftover large bodies were captured as moons or ejected by gravity assist into the Oort cloud. The start of thermonuclear fusion in the Sun's core created enough luminosity so that the remaining hydrogen and helium gas in the solar disk was removed by radiation pressure.
The only remaining problem is the distribution of angular momentum. The current explanation for the fact that most of the angular momentum is in the outer planets is that, by some mechanism, the Sun has lost angular momentum. The mechanism of choice is magnetic braking.
Meanwhile in the outer Solar System:
The Jovian worlds, having an early edge on gathering mass in the colder outer solar disk, were the most efficient at capturing planetesimals, which only served to increase their already large masses. As the planetesimals shrink in average size, collisions with proto-planets lead to fragmentation. So quickly the Solar System divided into large proto-planets and smaller and smaller planetesimals which eventually became the numerous meteors we see today. Any leftover large bodies were captured as moons or ejected by gravity assist into the Oort cloud. The start of thermonuclear fusion in the Sun's core created enough luminosity so that the remaining hydrogen and helium gas in the solar disk was removed by radiation pressure.
The only remaining problem is the distribution of angular momentum. The current explanation for the fact that most of the angular momentum is in the outer planets is that, by some mechanism, the Sun has lost angular momentum. The mechanism of choice is magnetic braking.
The early Sun had a much heavier flow of solar winds particles. Many of the particles in the solar wind are charged, and are effected by the laws of motion as well as electromagnetic forces. As the solar wind leaves the solar surface, they are ``dragged'' by the magnetic field, which in turn slows down the Sun's rotation.
Migrating Planets:
The protoplanet hypothesis explains most of the features of the Solar System; however, the outer solar system is still strange, especially the properties of Pluto/Charon. One explanation is that the Solar System was not born in the configuration that we see today. That the planets in the outer Solar System migrated to their present positions.
Migration requires some interaction between the planet and a fairly large body or the gravitational forces are too weak. Early in the formation of the Solar System, there were lots of Moon-sized to Mars-sized bodies, especially in the outer SS. A large planetesimal that crosses near Neptune will lose some energy, fall down near Jupiter, gain energy to be ejected into the Oort Cloud.
Migrating Planets:
The protoplanet hypothesis explains most of the features of the Solar System; however, the outer solar system is still strange, especially the properties of Pluto/Charon. One explanation is that the Solar System was not born in the configuration that we see today. That the planets in the outer Solar System migrated to their present positions.
Migration requires some interaction between the planet and a fairly large body or the gravitational forces are too weak. Early in the formation of the Solar System, there were lots of Moon-sized to Mars-sized bodies, especially in the outer SS. A large planetesimal that crosses near Neptune will lose some energy, fall down near Jupiter, gain energy to be ejected into the Oort Cloud.
This will have the effect of decreasing the size of Jupiter's orbit, and expanding the size of Saturn, Uranus and Neptunes' orbits. As Neptune moves outward, it will beginning to perturb the orbits of the trans-Neptunian objects (large ice covered astroids of which Pluto/Charon are a member). This pushes Pluto/Charon into a highly eccentric, inclined 3:2 resonant orbit that it occupies today.
All the leftover planetesimals near Neptunes orbit are pushed into a torus shaped region called the Kuiper belt. Smaller planetesimals are thrown farther out into the Oort cloud.
Extrasolar Systems:
Support for the protoplanet hypothesis has been found by the detection of disk material around of stars, such as Beta Pictoris and by Hubble images of the Orion Nebula.
Support for the protoplanet hypothesis has been found by the detection of disk material around of stars, such as Beta Pictoris and by Hubble images of the Orion Nebula.
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