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Chapter 1. The Solar System
- Objectives:
- Upon completion of this chapter, you will be able to state distances of objects within the solar system in terms of light-time, describe the Sun as a typical star, relate its share of the mass within the solar system, and compare the terrestrial and jovian planets. You will be able to distinguish between inferior and superior planets, classical and dwarf planets, describe asteroids, comets, the Kuiper belt, and the Oort cloud. You will be able to describe the environment in which the solar system resides.
The geocentric system of Tycho Brahe (1546-1601) shows the Moon and the Sun revolving around Earth while Mercury, Venus, Mars, Jupiter, and Saturn revolve around the Sun, all surrounded by a sphere of fixed stars. Tycho's assistant Johannes Kepler later based his refinement of Nicolaus Copernicus's heliocentric system upon Tycho's lifetime compilation of astronomical data. Image courtesy Wikimedia Commons. Click image for link.
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The solar system has been a topic of study from the beginning of history. For nearly all that time, people have had to rely on long-range and indirect measurements of its objects. For all of human history and pre-history, observations were based on visible light. Then in the 20th century, people discovered how to use additional parts of the spectrum. Radio waves, received here on Earth, have been used since 1931 to investigate celestial objects. Starting with the emergence of space flight in 1957, instruments operating above Earth's obscuring atmosphere could take advantage not only of light and radio, but virtually the whole spectrum (the electromagnetic spectrum is the subject of a later chapter). At last, with interplanetary travel, instruments can be carried to many solar system objects, to measure their physical properties and dynamics directly and at very close range. In the 21st century, knowledge of the solar system is advancing at an unprecedented rate.
The solar system consists of an average star we call the Sun, its "bubble" the heliosphere, the classical planets Mercury, Venus, Earth, Mars, Jupiter, and Saturn which were known to the ancients, and Uranus and Neptune, as well as the dwarf planet Pluto, which is one of a number of objects in the Kuiper Belt. The solar system includes the satellites of the planets, numerous comets, asteroids, meteoroids, and the interplanetary medium, which permeates interplanetary space. The dwarf planet Ceres is a member of the main belt of asteroids. The Oort cloud, a vast reservoir of comet nuclei, marks the farthest extent of the Sun's practical gravitational influence, out to about 3 light years from the Sun.
Interstellar space is the term given to the space between stars in the galaxy. The Sun's nearest known stellar neighbor is a red dwarf star called Proxima Centauri, at a distance of about 4.2 light years (a light year is the distance light travels in a year, at about 300,000 km per second). We are beginning to find that many stars besides the Sun harbor their own "solar systems" with planets, which are being called extrasolar planets, or exoplanets. As of December 2007, astronomers have detected a total of 270 planets orbiting other stars. This number is up from the milestone of 100 exoplanets discovered as of January 2004. Most known exoplanets are gas giants, Jupiter-like planets, since current methods favor the detection of the more massive worlds. Most are relatively nearby, within 5,000 light years, although one candidate was discovered in September 2005 at a distance of 17,000 light years, via "microlensing."
In Cosmic Perspective
Our whole solar system, along with all the local stars you can see on a clear dark night, sit in one of our galaxy's spiral arms, known as the Orion arm, as they orbit the supermassive black hole in the dense star cluster at the center of our galaxy some 26,000 ± 1400 light-years distant from us. At this great distance, we go around once about every 250 million years. Stars very close to the central mass are observed in keplerian orbits with periods as short as 15.2 years. This spiral disk that we call the Milky Way includes
some 200 billion stars, thousands of gigantic clouds of gas and dust, and enormous quantities of mysterious dark matter.
The image at right shows a galaxy known as M100 that is similar to our own Milky Way galaxy (click the image for details). The Milky Way has two small galaxies orbiting it nearby, which are visible from Earth's southern hemisphere. They are called the Large Magellanic Cloud and the Small Magellanic Cloud.
Our galaxy, one of billions of galaxies known, is travelling through intergalactic space. On a cosmic scale, all galaxies are generally receding from each other, although those relatively close together may exhibit additional local motion toward or away from each other as well.
Aside from its galactic orbital velocity (250-300 km/second), the Sun and its planetary system wander through the local stellar neighborhood at roughly 100,000 kilometers per hour, entering and leaving various tenuous local clouds of gas on a time scale of roughly once every few thousand to millions of years.
Immediately surrounding our solar system is a warm, partly ionized cloud, called the Local Interstellar Cloud. Like most interstellar clouds, its gas comprises about 90% hydrogen and 10% helium. Roughly 1% of the cloud's mass is dust.
Approximate Typical Conditions in Galaxy |
Region of Interstellar Space
Within our Galaxy |
Number Density,
Atoms / cm3 |
Temperature,*
Kelvins |
Inside our Heliosphere,
in the Vicinity of Earth |
5 |
10,000 |
Local Cloud Surrounding
our Heliosphere |
0.3 |
7,000 |
| Nearby Void (Local Bubble) |
< 0.001 |
1,000,000 |
| Typical Star-Forming Cloud |
>1,000 |
100 |
| Best Laboratory Vacuum |
1000 |
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| Classroom Atmosphere |
2.7 X 1019 |
288 |
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*Temperatures refer to particles in the near-vacuum of space. Large physical masses, such as spacecraft, asteroids, etc., are not affected by the particles' temperature. Instead, the thermal states of massive objects are dominated by solar (or stellar) heating and exposure to shadow.
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| Outside the galaxy, in intergalactic space, the number density of particles is thought to fall off to about one atom or molecule per cubic meter (10-6 / cm3). |
Motions Within the Solar System
The Sun and planets each rotate on their axes. Because they formed from the same rotating disk, the planets, most of their satellites, and the asteroids, all revolve around the Sun in the same direction as the Sun rotates, and in nearly circular orbits. The planets orbit the Sun in or near the same plane, called the ecliptic (because it is where eclipses occur). Pluto is a special case in that its orbit is the most highly inclined (17 degrees) and the most highly elliptical of all the planets. Its orbit is more typical of a Kuiper Belt Object. Because its orbit is so eccentric, Pluto sometimes comes closer to the Sun than does Neptune. Most planets rotate in or near the plane in which they orbit the Sun, again because they formed, rotating, out of the same dust ring. The exception, Uranus, must have suffered a whopping collision that set it rotating on its side.
Distances Within the Solar System
The most commonly used unit of measurement for distances within the solar system is the astronomical unit (AU). The AU is based on the mean distance from the Sun to Earth, roughly 150,000,000 km. JPL's Deep Space Network refined the precise value of the AU in the 1960s by obtaining radar echoes from Venus. This measurement was important since spacecraft navigation depends on accurate knowledge of the AU. Another way to indicate distances within the solar system is terms of light time, which is the distance light travels in a unit of time. Distances within the solar system, while vast compared to our travels on Earth's surface, are comparatively small-scale in astronomical terms. For reference, Proxima Centauri, the nearest star at about 4.2 light years away, is about 265,000 AU from the Sun.
| Light Time |
Approximate Distance |
Example |
| 3 seconds |
900,000 km
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~ Earth-Moon Round Trip |
| 3 minutes |
54,000,000 km |
~ Sun to Mercury |
| 8.3 minutes |
149,600,000
km |
Sun to Earth (1 AU) |
| 1 hour |
1,000,000,000 km |
~ 1.5 x Sun-Jupiter Distance |
| 14.5 hours |
105 AU |
Voyager-1 (January, 2008) |
| 1 year |
~ 63,000 AU |
Light Year |
| 4.2 years |
~ 265,000 AU |
Next closest star |
Temperatures Within the Solar System
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Select the above link for the Solar System Temperature Reference showing examples and comparing temperatures of objects and conditions from absolute zero through planet temperatures, to those of stars. The reference also includes temperature conversion factors and links to a conversion engine.
The Sun
The Sun is a typical star. Its spectral classification is "G2 V." The G2 part basically means it's a yellow-white star, and the roman numeral V means it's a "main sequence" dwarf star (by far the most common) as opposed to supergiant, or sub-dwarf, etc. The fact that the Sun is the dominant source of energy for processes on Earth that sustain us makes it a subject of major interest for study. As viewed from the Earth's surface, the Sun subtends roughly half a degree of arc upon the sky (as does the Moon, at this period in cosmic time.)
You can view some remarkable current images of the Sun as seen today by the suite of instruments aboard SOHO (Solar & Heliospheric Observatory) as it views the Sun from the L1 Lagrange point between the Earth and the Sun.
Mass:
The Sun dominates the gravitational field of the solar system. The motion of everything within a few light years of the Sun is dominated by the effect of the solar mass. At 1.98892 X 1030 kilograms, or roughly 333,000 times the mass of the Earth, it contains over 99 percent of the solar system's mass. The planets, which condensed out of the same disk of material that formed the Sun, contain just over a tenth of a percent the mass of the solar system.
Here's how the Sun's mass can be calculated.
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This SOHO image of the Sun is from a movie combining three wavelengths of extreme ultravilot light. Click image to select movie.
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Mass Distribution Within the Solar System |
| 99.85% |
Sun |
| 0.135% |
Planets |
| 0.015% |
Comets
Kuiper belt objects
Satellites of the planets
Minor Planets (Asteroids)
Meteroids
Interplanetary Medium |
| Even though the planets make up only a small portion of the solar system's mass, they do retain the vast majority of the solar system's angular momentum. This storehouse of momentum can be utilized by interplanetary spacecraft on so-called "gravity-assist" trajectories.
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Fusion:
The Sun's gravity creates extreme pressures and temperatures within its core, sustaining a thermonuclear reaction fusing hydrogen nuclei and producing helium nuclei. This reaction converts about 4 billion kilograms of mass to energy every second. This yields tremendous amounts of energy, causing the state of all the Sun's material to be plasma and gas. These thermonuclear reactions began about 5 billion years ago in the Sun, and will probably continue for another 5 billion years into the future. Energy produced in the core takes over a million years to reach the surface and be radiated as light and heat (view this illustrated description). Our star's output varies slightly over an 11-year cycle, during which the number of sunspots changes.
Solar sound waves are mostly trapped inside the sun. They refract away from the hot core, and reflect back and forth between different parts of the photosphere. By monitoring the sun's vibrating surface, helioseismologists can probe the stellar interior in much the same way that geologists use seismic waves from earthquakes to probe the inside of our planet.
Rotation:
The Sun rotates on its axis with a period of approximately 25.4 days. This is the adopted value at 16° latitude. Because the Sun is a gaseous body, not all its material rotates together. This solar fact sheet describes how rotation varies with latitude. Solar matter at very high latitudes takes over 30 days to complete a rotation.
The Sun's axis is tilted about 7.25 degrees to the plane of the Earth's orbit, so we see a little more of the Sun's northern polar region each September and more of its southern region in March.
Magnetic Field:
Magnetism is produced in the Sun by the flow of electrically charged particles: ions and electrons. Sunspots are somewhat cooler places seen on the photosphere (the Sun's bright surface) where very intense magnetic lines of force break through. Prominences that seem to float above the photosphere are supported by, and threaded through with, magnetic fields. All the streamers and loops seen in the corona (the Sun's extended upper atmosphere) are shaped by magnetic fields. Magnetic fields are at the root of virtually every feature observed on and above the Sun.
SOHO image in extreme ultra violet light. Click to view 1-Mbyte movie of solar activity increasing toward 11-year maximum in early 2000 then decreasing.
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Not surprising, the Sun's magnetic field permeates interplanetary space. The magnetic field of the Sun influences the way in which charged particles (cosmic rays, solar energetic particles, and even interstellar dust grains) move through the heliosphere.
The 11-year solar magnetic cycle that sunspot activity follows, is part of a 22-year "Hale" cycle. During the first half of the 22-year cycle, the Sun's magnetic north pole is in the northern hemisphere, while the magnetic south pole is in the southern hemisphere. Right around the peak of the sunspot cycle (solar maximum) about 11 years into the magnetic cycle, the magnetic poles flip, exchanging places, so that magnetic north is then located in the southern hemisphere.
Mass Ejections:
Coronal mass ejections, CMEs, are huge magnetic bubbles of plasma that expand away from the Sun at speeds as high as 2000 km per second. A single CME can carry up to ten billion tons (1013 kilograms) of plasma away from the Sun. Coronal mass ejections were once thought to be initiated by solar flares. Although some are accompanied by flares, it is now known that most CMEs are not associated with flares.
When a CME arrives at Earth, it can cause fluctuations in the Earth's magnetic field that can play havoc with the civil electrical power distribution infrastructure, by inducing unwanted voltages.
View this spectacular 5-Mbyte SOHO movie of CMEs in August, 1999. Stars are seen moving behind the Sun as the view from SOHO changes while Earth orbits toward the right.
Solar Wind:
The solar wind streams off of the Sun in all directions. The source of the solar wind is the Sun's hot corona, whose temperature is so high that the Sun's gravity cannot hold on to it. Although why this happens is understood, the details about how, and exactly where, the coronal gases are accelerated is one subject of ongoing investigation. The solar wind flows fastest when the sunspot cycle is at its minimum, because there is less turbulence in the corona to slow it down. Discussion of the solar wind's effects continues below.
Our Bubble of Interplanetary Space
The "vacuum" of interplanetary space includes copious amounts of energy radiated from the Sun, some interplanetary and interstellar dust (microscopic solid particles) and gas, and the solar wind. The solar wind, discovered by Eugene Parker in 1958, is a flow of lightweight ions and electrons (which together comprise plasma) thrown from the Sun.
The solar wind flows outward from our star at about 400 km per second (about 1 million miles per hour), measured in the vicinity of Earth's orbit. The Ulysses spacecraft found that it approximately doubles its speed at high solar latitudes. It has a visible effect on comet tails, blowing the charged-particle component of the comet's tail out away from the Sun as if they were wind socks. The solar wind inflates a bubble, called the heliosphere, in the surrounding interstellar medium (ISM).
Diagram courtesy Dr. Gary Zank, University of Delaware
The boundary at which the solar wind meets the ISM, containing the collective "solar" wind from other local stars in our galaxy, is called the heliopause. This is where the solar wind and the Sun's magnetic field stop. The boundary is theorized to be roughly teardrop-shaped, because it gets "blown back" to form a heliotail, as the Sun moves through the ISM (toward the right in the diagram above). The Sun's relative motion may also create an advance bow shock, analogous to that of a moving boat. This is a matter of debate and depends partly on the strength of the interstellar magnetic field.
But before it gets out to the heliopause, the solar wind slows to subsonic speeds, creating a termination shock. This appears at the perimeter of the green circle in the diagram. Its actual shape, whether roughly
Water flowing from a faucet onto a plate presents an analogy for the solar wind piling up at the termination shock. Click to animate. Planetary orbits are not drawn to scale.
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spherical or teardrop, depends on magnetic field strengths, as yet unknown. Humanity's most distant object the Voyager 1 spacecraft, still in routine communication with JPL, crossed the termination shock in December 2004 at a distance of 94 AU from the Sun. Today the craft is passing through the heliosheath, the region between the termination shock and the heliopause, at a rate of 3.6 AU per year, and is expected to reach the heliopause in about 2015 while still communicating with Earth.
In the diagram above, temperatures are theorized; none have been actually measured very far beyond the termination shock. Note that even with the high particle temperatures, their density is so low that massive objects like spacecraft do not "feel" these temperatures. Instead, their thermal states are dominated by solar (stellar) heating and exposure to shadow.
The white lines in the diagram represent charged particles, mostly hydrogen ions, in the interstellar wind. They are deflected around the heliosphere's edge (the heliopause). The pink arrow shows how neutral particles penetrate the heliopause. These are primarily hydrogen and helium atoms, which are mostly not affected by magnetic fields, and there are also heavier dust grains. These interstellar neutral particles make up a substantial fraction of the material found within the heliosphere. The little black + in the green area represents the location where Voyager 1 was, at 80 AU from the Sun, in January 2001.
The solar wind changes with the 11-year solar cycle, and the interstellar medium is not homogeneous, so the shape and size of the heliosphere probably fluctuate.
The solar magnetic field is the dominating magnetic field within the heliosphere, except in the immediate environment of those planets that have their own global magnetic fields. It can be measured by spacecraft throughout the
HST view February 1995. Arcing structure is stellar bow shock about half a light-year across, from star L.L. Orionis's wind colliding with the Orion Nebula flow. Click for much larger image. Courtesy NASA, Hubble Heritage Team (STScI/AURA).
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solar system, but not here on earth, where we are shielded by our planet's own magnetic field.
The actual properties of the interstellar medium (outside the heliosphere), including the strength and orientation of its magnetic field, are important in determining the size and shape of the heliopause. Measurements that the two Voyager spacecraft will make in the region beyond the termination shock, and possibly beyond the heliopause, will provide important inputs to models of the termination shock and heliopause. Even though the Voyagers will sample these regions only in discrete locations, their information will result in more robust overall models.
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