Solar System

Solar System is a Division B event that returned for the 2018 and 2019 seasons with a focus on terrestrial planets and other rocky bodies in the solar system. In 2014 and 2015 the event focused on water and ice in the solar system, while in past years it addressed the Sun, planets and their satellites, comets, asteroids, the Oort Cloud, the Kuiper Belt, meteoroids, meteorites, and meteors.

Year-Specific Information
This page focuses on the general competition of Solar System. However, the event sometimes involves a specific topic. These topics are presented in the table below.

Origins of the Solar System
Our solar system was formed about 4.57 billion years ago in a nebula, the center of which was the protosun. Surrounding it were the materials that would be the planets, planetesimals. When the nebula was sent into a spinning motion (possibly by a large star), the heavier, rocky materials gravitated to the center, and the lighter gaseous materials fell to the outer solar system. In the inner solar system, the small planetesimals continued to gather more material becoming the 4 rocky terrestrial planets (Mercury, Venus, Earth, and Mars). In the outer solar system the rocky materials gathered to form planets, but the lighter gas materials were attracted by the gravity of the cores to form the Jovian (gaseous) planets(Jupiter, Saturn, Uranus, and Neptune). One group of planetesimals that never formed a planet was between Mars and Jupiter. They formed the asteroid belt. The leftover materials on the far edges of the solar system that did not form planets formed the Oort Cloud and Kuiper (kai-per) belt. These two bodies are the source of many comets, the dwarf planets Pluto, Ceres, Eris, Haumea, and Makemake, and the questionable planet or dwarf planet Sedna.

Quick Guide to the Solar System
Use this chart to quickly compare some basic info for all the planets.

Bodies of the Solar System
(Please note that all of the largest/smallest classifications of the planets do NOT include Pluto!)

The Sun
''Main article: Sun

Inner Planets
Main article: Terrestrial Bodies.

The inner planets of our solar system are those between the Sun and the asteroid belt; Mercury, Venus, Earth, and Mars.

Outer Planets
''Main article: Outer Planets

Dwarf Planets
The definition of a Dwarf Planet is a planet with enough of a gravitational pull to keep a spherical shape, but not strong enough to "clear the neighborhood", which means that any object that comes close to the planet, it either "pushes away" or "pulls into an orbit". In addition to that it cannot be a satellite of a non-stellar body.

Ceres
The largest object in the Asteroid Belt, containing 30% of its mass. When it was discovered in the early 1800s, Ceres was considered a planet, but was reclassified as an asteroid 50 years later. Since 2006, it has been considered a dwarf planet. Ceres orbits the Sun once every 4.6 Earth years and its day is about 9 hours.

Pluto
When it was still considered a planet, Pluto was the ninth planet from the Sun and the smallest planet. It became a dwarf planet in 2006. Pluto is the largest and second-most-massive (after Eris) known dwarf planet in the Solar System, and the ninth largest and tenth most massive known object directly orbiting the Sun. It is also the largest known trans-Neptunian object by volume but is less massive than Eris. Like other Kuiper belt objects, Pluto is mostly made of ice and rock. Its atmosphere consists nitrogen (N2), methane (CH4), and carbon monoxide (CO), which are in equilibrium with their ices on Pluto's surface. It has similarly sized moon, Charon (pronounced "karen"). Charon is so big that they are sometimes considered as a binary system because the barycenter of their orbits does not lie within either body. Pluto was discovered in 1930 by Clyde Tombaugh, and was the only planet discovered in the 20th century. It is a part of the Kuiper belt, and is one of many similar Kuiper Belt objects. Pluto’s orbit is both elliptical and tilted and takes 248 years to orbit the sun. The orbit can take it as far as 49.3 AU from the sun, and as close as 30 AU. It also has four smaller moons, Nix, Hydra, Kerberos, and Styx. In 2015, the New Horizons spacecraft became the first spacecraft to fly by Pluto.

Eris
Eris is in the scattered disc, a region beyond the Kuiper Belt. Since Eris is larger than Pluto, its discovery led the IAU (International Astronomical Union) to define "planet" and reclassify Pluto as a dwarf planet. Its only known satellite is Dysnomia.

Haumea
An "egg-shaped" dwarf planet in the Kuiper belt. The odd shape is believed to come from a high rotational speed, which flattens the poles and creates a bulge around the equator. Haumea has a year of about 283 earth years. It also has two moons, Hi'iaka and Namaka. These are believed to be fragments of the KBO - early in its history, it was hit by something, breaking off Hi'iaka and Namaka.

Makemake
Makemake has no moons, making it unique among the larger Kuiper Belt objects. It orbits the sun every 310 years. Like most KBOs, it has an highly eccentric orbit - it's perihelion (distance closest to sun), is 38.5 AU(5,760,000,000 km). It's aphelion (distance farthest from sun), is 53.1 AU (7,939,000,000 km). It has a mass of 3 × 10^21 kg.

Plutoids
To be considered a Plutoid, a dwarf planet must have a semi-major axis greater than that of Neptune. In other words, it must orbit outside of Neptune. Any Dwarf planet that orbits within Neptune is considered still considered a dwarf planet. As of right now, there are four official Plutoids. They are Pluto, Haumea, Makemake, and Eris.

Plutoid Candidates
Some objects in the solar system are not officially considered dwarf planets or plutoids, but are large enough to be prime candidates for plutoid status.

Sedna
Sedna is a plutoid candidate with an orbit lasting about 11,518 Earth years. Its orbit is also highly eccentric, with a perihelion in the outer Kuiper Belt and an aphelion possibly in the inner Oort Cloud. Sedna's diameter is 995 miles, or about 1,600 kilometers. This object has no known natural satellites. Its discovery was mostly luck, as it was near its perihelion and at a (barely) detectable magnitude. Should it have been at the aphelion, it would remain unknown for thousands more years. This great distance is a potential reason that no natural satellites have been found; they would be way too dim.

Small Solar System Bodies
''Main article: Small Bodies

Some examples of small bodies in the Solar System include asteroids, meteoroids, and comets.

Oort Cloud
The Oort cloud is an immense cloud at the outer limits of the solar system. This is believed to be the farthest reaches of the Sun's gravitational pull that measurably affects other objects. This cloud is so vast that comets within it can be tens of millions of kilometers apart. It is believed that the cloud is denser along the elliptical plane. The estimated mass of all the bodies in the Oort cloud is about 40 times Earth's mass. These comets are easily influenced by other stars, and often a star that comes to close to another star's Oort cloud can fling these comets out into deep space or into the solar system. It is believed that this is where many of the comets and asteroids in our solar system originated from.



Kuiper Belt
The Kuiper belt is similar to the Asteroid belt. It lies beyond Neptune, about 30-50 AU from the Sun. It is believed that these are the remains of when the Solar System was first created. When the solar system was created, most space debris was condensed to form planets. The debris that did not form planets slowly drifted outwards to form the Kuiper Belt. NASA’s New Horiozons was the first spacecraft to actually visit an object in the Kuiper Belt. It flew by Pluto and its moons in July 2015. New Horizons is to fly past another Kuiper Belt object, 2014 MU69 on New Year's Eve 2018.

Moons of the Solar System
Mercury: No moons

Venus: No moons There are 79 moons of Jupiter (53 named and 26 awaiting confirmation as of July 2018), but only the most famous ones are listed here. There are 60 moons and numerous moonlets of Saturn, but only the most famous ones are listed here. There are 27 moons of Uranus, but only the major ones, those massive enough for their surfaces to have collapsed into a spheroid, are listed here. 1Negative orbital periods indicate retrograde orbit.

Lunar Eclipses
A type of eclipse that occurs when the Earth passes directly between the moon and sun, which means that the moon is in Earth's shadow. Since Earth is in the middle of the moon and sun, it must always be a full moon for a lunar eclipse to occur. There are several types of lunar eclipses:

Penumbral Eclipse- The moon passes through Earth's penumbra, causing its surface to darken slightly. Total Penumbral Eclipse- The moon passes "exclusively" through Earth's penumbra. The area of the moon closest to the umbra can appear darker than the rest of it. Partial Lunar Eclipse- A portion of the moon passes through Earth's umbra.

Total Lunar Eclipse- The whole moon passes through Earth's umbra. Totality can last up to 107 minutes, depending on the distance of the moon (at apogee, the moon's speed is slower, meaning a longer eclipse). Selenehelion- Also known as a "horizontal eclipse", this is when the sun and the eclipsed moon can be seen at the same time. It can only occur right after sunrise or just before sunset. Technically, the moon and sun shouldn't be visible at the same time, but Earth's atmosphere refracts light and things near the horizon appear higher in the sky than they really are. The name is derived from the Greek goddess of the Moon (Selene) and their word for Sun, helios.



Solar Eclipses
The moon passes between the Earth and sun so that the sun's light is partially or completely blocked. Solar Eclipses can only occur during a new moon, when the moon is between the earth and the sun. However, since the moon's orbit around the earth is inclined at about 5°, solar eclipses can only happen when the moon's orbit crosses the ecliptic. There are four types of solar eclipses:

Total Eclipse- The sun is completely blocked by the moon. A total eclipse often happens near perigee because the moon is closer to the earth and its apparent size is larger. When earth is close to aphelion, total eclipses are also more likely to occur. The sun's disk is obscured and its corona is visible. Total eclipses are only visible from the path of totality in the moon's umbra. Annular Eclipse- The sun and moon are in line, but the moon's apparent size is smaller than the sun because the moon is close to apogee. Annular eclipses are more likely to occur during earth's perihelion. The sun appears as a bright ring around the moon's outline. Annular eclipses are only visible in the antumbra. Hybrid Eclipse- A hybrid eclipse is visible as a total eclipse from some places on earth and is visible as an annular eclipse from other places. This kind of eclipse is rare compared to the other kinds. Partial Eclipse- The moon only obscures part of the sun. Partial eclipses can be seen from "a large part of earth" (the moon's penumbra) outside the path of totality for a total or annular eclipse. Some eclipses are only visible as a partial eclipse because the umbra passes above the poles.

Laws of motion
1. An object at rest stays at rest unless acted on by an outside force. An object in motion stays in motion unless acted on by an outside force.

2. F=ma. Force equals mass times acceleration.

3. For every action, there is an equal and opposite reaction.

Law of Gravitational Attraction
Every object attracts every other object with a force proportional to the product of their masses and inversely proportional to the square of their distance.

[math]F = G \frac{m_1 m_2}{r^2}[/math]

Where,

F is the magnitude of the gravitational force between the two point masses,

G is the gravitational constant,

m1 is the mass of the first point mass,

m2 is the mass of the second point mass, and

r is the distance between the two point masses.

Kepler's Laws of Planetary Motion
Kepler's Laws are as follows:
 * 1) The orbit of every planet is an ellipse with the sun at a focus.
 * 2) A line joining a planet and the sun sweeps out equal areas during equal intervals of time.
 * 3) The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit.

See here for more info. Many of the pictures and diagrams used in this section are from here.

Law 1
The orbit of every planet is an ellipse with the sun at a focus.

To understand this law, you must first understand ellipses. You can think of an ellipse as a flatten circle, with two axes. There is the major axis, which is the longer one, and the minor axis, which is the shorter one. There are always two focuses, which are on the major axis. There is also a semi-major axis, which is half the major axis, and a semi-minor axis, or half the minor axis. The sum of the distance to both of the foci is constant.



What the law states is that the sun is at one of the foci, and the planet orbits around it in an ellipse. Most of the time the ellipse is close to a circle in shape, but is never a circle.

Law 2
A line joining a planet and the sun sweeps out equal areas during equal intervals of time. This one is harder to envision. So we've established that the orbit is elliptical, right? Two lines extending out of the sun will always have the same area, and the planet we are talking about will always travel this distance in equal time. Look at this picture:



Make sense now? The blue sections have the same area, and the Earth will travel the distance the blue area covers in the same time. So when the blue is wider, the Earth moves faster. The blue is wider closer to the sun, so the closer to the sun you are, the faster the planet will orbit around the sun.

Law 3
The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit. This is purely math. [math]\frac{P_1^2}{P_2^2} = \frac{R_1^3}{R_2^3}[/math]

So what this means is that these two fractions are equal. Remember in the first law, we defined the major and minor axes? The semi-major axis is half of the major axis. So that shows that the minor axis defines the orbital period! You can use this law to find either the semi-major axis, which can then be used to find the major axis, or the orbital period. Since [math]p^2 = a^3[/math], we can use the formula [math]p = a^{3/2}[/math] to find the orbital period, or [math]a = p^{2/3}[/math] to find the semi-major axis.

Escape Velocity
Escape Velocity is the velocity something must reach in order to escape the gravitational pull of a planet. You can calculate the escape velocity using this formula: [math]E_v = \sqrt{\frac{2GM}{R}} [/math]

Where, Ev is the escape velocity, M is the mass (in kg) of the planet, G is the gravitational constant (equal to [math]6.67\times10^{-11} \ {\rm N} \ {\rm m^{2}} \ {\rm  kg^{-2}}[/math]), and R is the radius of your planet in meters.

This is a strange form of measurement for a planet, so watch out. It can change your answer dramatically.

Here is a simple, easy to use Escape Velocity calculator made with Microsoft Excel. To use it, you fill in each box in a row with the mass and radius of your planet, respectively. You usually use meters for the radius, but this calculator converts it for you, so fill in the radius in kilometers. The first two boxes are used for the mass, so that a*10^b = mass, you would fill in "a" in the first box and "b" in the second box. Just look at the examples to figure out how to use it. [[Media:Escape_Velocity_Calculator.xls|Escape Velocity Calculator (.xls)]]

Effects of Planets/Satellites
Tidal locking- when one side of an astronomical object always faces another astronomical body. For example, the Moon takes just as long to rotate one time as it does to revolve around Earth one time. Two objects of a similar size (like Pluto and Charon) may both become tidally locked to each other.

Shepherding- Where a moon orbits near the edge of a ring, using its gravitational pull to keep the ring's particles in a tight band and prevent them from spreading out too much.

Resonance- A relationship in which the orbital period of one body is related to that of another by a simple integer fraction.

* Eventually (in a few hundred million years), Io, Europa, Ganymede, and Callisto will be in a 1:2:4:8 resonance with these three moons. Callisto will orbit Jupiter once for every 2 Ganymede orbits, every 4 Europa orbits, or every 8 Io orbits.

Laplace Resonance- Where 3 or more astronomical bodies are in resonance with each other. The only known Laplace resonance is between Jupiter's moons Io, Europa, and Ganymede.

Trojans- A 1:1 resonance between two astronomical bodies where a minor planet or moon shares the same orbital path as a larger body but does not collide with it because it orbits 60° ahead of or behind the larger planet or moon (at the Lagrangian points L₄ or L₅). Mars, Jupiter, and Neptune each share their orbits with Trojan asteroids, while Saturn's moons have smaller Trojan moons (Telesto and Calypso share an orbit with Tethys, Helene and Polydeuces with Dione).

Aristarchus
Aristarchus was an ancient Greek astronomer. He was the one to first put forward the idea of a heliocentric Solar System. After observing solar and lunar eclipses, he deduced correctly that the Solar System was heliocentric.

Tycho Brahe
(1546-1601)

Tycho Brahe was a Danish astronomer that was famous for creating precise measurements of the planets, and also more than 700 stars. He discovered a supernova in 1572 near Cassiopeia. The king of Denmark was so impressed with this discovery that he funded a large observatory on the island of Ven. He also invented his own view of the Universe, the Tychonian System. In it, every planet but Earth orbited the Sun, and the Sun and Moon orbited the Earth.

Galileo Galilei
(1564-1642)

Galileo Galilei was a very famous astronomer who is sometimes known as "the father of modern observational astronomy". His greatest astronomical achievements include discovering Jupiter's four largest satellites, observing and recording the phases of Venus, improving the design of the telescope, and greatly supporting the theory of a heliocentric solar system.

Galileo was born in Pisa, Italy, but moved to Florence at the age of 8. He later applied to the University of Pisa to get a medical degree, but his interests took a different course (no pun intended) and he ended up studying mathematics.

This upset the church, who then sentenced him to house arrest. He went blind (most likely from studying the sun), shortly before he died.

Johannes Kepler
(1571-1630)

Johannes Kepler was a German astronomer most famous for developing the Kepler's Laws of Planetary Motion. He began to work on complex math formulas to explain planetary motion, which he mistakenly thought were circular in shape. Later, he became Tycho Brahe's assistant. Kepler and Tycho did not get along, however, and Tycho set Kepler to the task of understanding Mars' orbit. It was just this that allowed him to find the final piece in developing the Laws of Planetary Motion.

Clyde Tombaugh
(1906-1997)

Clyde Tombaugh is credited for discovering Pluto. He began at home with a nine inch home-made telescope, and used this to draw pictures of Saturn and Jupiter. He sent the pictures to the Lowell Observatory, and was immediately offered a position. His goal was to discover the elusive "planet X", later to be renamed Pluto. Even after this great accomplishment, he went on to discover many more things such as comets, open clusters, and globular clusters.

Nicholas Copernicus
(1473-1543)

Nicholas Copernicus was a Polish astronomer who developed the Copernicus theory, stating that the sun lies near the center of the Solar System, and the Earth revolves around it, rather than the other way around. This theory was not proven until Galileo, and not widely accepted for many more years. Later in life he went on to lecture in Rome about astronomy.

Edmond Halley
(1656-1742)

Edmond Halley was a British astronomer who was the first to calculate a comet's orbit. He went to the University of Oxford where he studied the theories of Sir Issac Newton. He published a book in 1705 called Astronomiae Cometicae Synopsis (Synopsis on Cometary Astronomy). His theories were validated when a comet appeared in 1758, just as he predicted. The comet was named after him for his remarkable accuracy, and is now known as Halley's comet.

Missions
For more information on each individual mission, see Solar System/Missions.

Many missions have been undertaken for the exploration and advancement of knowledge of the celestial bodies described above. In addition, many missions are currently being planned and prepared. Some of the most noteworthy are highlighted in the table below.

Helpful Tips
This event often contains many questions/tasks not listed on the event sheet, so you should study anything that could be interpreted as related to our solar system. If you do this (And have a decent reference book) you should be guaranteed to get a top ten finish. Also, make sure to check information posted on the site - it may be mistaken and/or outdated.

When making a note sheet, use One Note, since you can fit a lot of text and diagrams on one page, and you can easily use the clipping tool to copy and paste text from websites onto your note sheet.

Links

 * [[Media:Solar_Study_Guide.pdf]] - Example Study Guide
 * The 9 planets
 * Views of the solar system
 * Soinc's solar system page
 * Information on famous astronomers
 * Kepler's Laws of Planetary Motion
 * Facts about the solar system
 * [[Media: SS Planet Characteristics.doc |Notes on planet characteristics]]
 * Formation of Cycloidal Ridges on Europa