What is a solar system? FORMATION OF SOLAR SYSTEM Components of the SOLAR SYSTEM Discovery and exploration Terminology Description of the Components of the SOLAR SYSTEM Farthest Regions Galactic Context The Solar System is located in the Milky Way galaxy, a barred spiral galaxy with a diameter of about 100,000 light-years containing about 200 billion stars. Our Sun resides in one of the Milky Way's outer spiral arms, known as the Orion Arm or Local Spur. The Sun lies between 25,000 and 28,000 light years from the Galactic Centre, and its speed within the galaxy is about 220 kilometres per second, so that it completes one revolution every 225–250 million years. This revolution is known as the Solar System's galactic year. The solar apex, the direction of the Sun's path through interstellar space, is near the constellation of Hercules in the direction of the current location of the bright star Vega. The plane of the Solar System's ecliptic lies nearly at right angles (86.5°) to the galactic plane.

1. SOLAR SYSTEM
1. FORMATION OF SOLAR SYSTEM
2. Components of the SOLAR SYSTEM
3. Discovery and exploration
4. Terminology
5. Description of the Components of the SOLAR SYSTEM
6. Farthest Regions
7. Galactic Context

2. The standard model for the formation of the Solar System (including
the Earth) is the solar nebula hypothesis. In this model, the Solar system
formed from a large, rotating cloud of interstellar dust and gas called
the solar nebula. It was composed of hydrogen and helium created shortly
after the Big Bang 13.8 Ga (billion years ago) and heavier elements ejected
by supernovae. About 4.5 Ga, the nebula began a contraction that may
have been triggered by the shock wave of a nearby supernova. A shock
wave would have also made the nebula rotate. As the cloud began to
accelerate, its angular momentum, gravity and inertia flattened it into
a protoplanetary disk perpendicular to its axis of rotation.
Small perturbations due to collisions and the angular momentum of other
large debris created the means by which kilometer-
sized protoplanets began to form, orbiting the nebular center.
FORMATION OF SOLAR SYSTEM

3. The center of the nebula, not having much angular momentum, collapsed rapidly,
the compression heating it until nuclear fusion of hydrogen into helium began. After
more contraction, a T Tauri star ignited and evolved into the Sun. Meanwhile, in the
outer part of the nebula gravity caused matter to condense around density
perturbations and dust particles, and the rest of the protoplanetary disk began
separating into rings. In a process known as runaway accretion, successively larger
fragments of dust and debris clumped together to form planets. Earth formed in this
manner about 4.54 billion years ago (with an uncertainty of 1%) and was largely
completed within 10–20 million years. The solar wind of the newly formed T Tauri
star cleared out most of the material in the disk that had not already condensed into
larger bodies. The same process is expected to produce accretion disks around
virtually all newly forming stars in the universe, some of which yield planets.
The proto-Earth grew by accretion until its interior was hot enough to melt the
heavy, siderophile metals. Having higher densities than the silicates, these metals
sank. This so-called iron catastrophe resulted in the separation of a primitive
mantle and a (metallic) core only 10 million years after the Earth began to form,
producing the layered structure of Earth and setting up the formation of Earth's
magnetic field. J. A. Jacobs was the first to suggest that the inner core—a solid
center distinct from the liquid outer core—is freezing and growing out of the liquid
outer core due to the gradual cooling of Earth's interior (about 100 degrees Celsius
per billion years).

4. SOLAR SYSTEM
1. FORMATION OF SOLAR SYSTEM
2. Components of the SOLAR SYSTEM
3. Discovery and exploration
4. Terminology
5. Description of the Components of the SOLAR SYSTEM
6. Farthest Regions
7. Galactic Context

5. The standard model for the formation of the Solar System (including
the Earth) is the solar nebula hypothesis. In this model, the Solar system
formed from a large, rotating cloud of interstellar dust and gas called
the solar nebula. It was composed of hydrogen and helium created shortly
after the Big Bang 13.8 Ga (billion years ago) and heavier elements ejected
by supernovae. About 4.5 Ga, the nebula began a contraction that may
have been triggered by the shock wave of a nearby supernova. A shock
wave would have also made the nebula rotate. As the cloud began to
accelerate, its angular momentum, gravity and inertia flattened it into
a protoplanetary disk perpendicular to its axis of rotation.
Small perturbations due to collisions and the angular momentum of other
large debris created the means by which kilometer-
sized protoplanets began to form, orbiting the nebular center.
FORMATION OF SOLAR SYSTEM

6. The center of the nebula, not having much angular momentum, collapsed rapidly,
the compression heating it until nuclear fusion of hydrogen into helium began. After
more contraction, a T Tauri star ignited and evolved into the Sun. Meanwhile, in the
outer part of the nebula gravity caused matter to condense around density
perturbations and dust particles, and the rest of the protoplanetary disk began
separating into rings. In a process known as runaway accretion, successively larger
fragments of dust and debris clumped together to form planets. Earth formed in this
manner about 4.54 billion years ago (with an uncertainty of 1%) and was largely
completed within 10–20 million years. The solar wind of the newly formed T Tauri
star cleared out most of the material in the disk that had not already condensed into
larger bodies. The same process is expected to produce accretion disks around
virtually all newly forming stars in the universe, some of which yield planets.
The proto-Earth grew by accretion until its interior was hot enough to melt the
heavy, siderophile metals. Having higher densities than the silicates, these metals
sank. This so-called iron catastrophe resulted in the separation of a primitive
mantle and a (metallic) core only 10 million years after the Earth began to form,
producing the layered structure of Earth and setting up the formation of Earth's
magnetic field. J. A. Jacobs was the first to suggest that the inner core—a solid
center distinct from the liquid outer core—is freezing and growing out of the liquid
outer core due to the gradual cooling of Earth's interior (about 100 degrees Celsius
per billion years).

7.  For many thousands of years, humanity, with a few notable exceptions,
did not recognize the existence of the Solar System. They believed the
Earth to be stationary at the center of the universe and categorically
different from the divine objects that moved through the sky. Although
the Greek philosopher Aristarchus of Samos had speculated on a
heliocentric reordering of the cosmos.
 Nicolaus Copernicus was the first to develop a mathematically
predictive heliocentric system. His 17th-century successors, Galileo
Galilei, Johannes Kepler and Isaac Newton, developed an
understanding of physics which led to the gradual acceptance of the
idea that the Earth moves around the Sun and that the planets are
governed by the same physical laws that governed the Earth.
 In more recent times, improvements in the telescope and the use of
unmanned spacecraft have enabled the investigation of geological
phenomena such as mountains and craters, and seasonal
meteorological phenomena such as clouds, dust storms and ice caps
on the other planets.

8.  The Solar System consists of the Sun and those celestial objects
bound to it by gravity, all of which formed from the collapse of a giant
molecular cloud approximately 4.6 billion years ago. Of the retinue of
objects that orbit the Sun, most of the mass is contained within eight
relatively solitary planets whose orbits are almost circular and lie within
a nearly-flat disc called the ecliptic plane. The four smaller inner planets,
Mercury, Venus, Earth and Mars, also called the terrestrial planets, are
primarily composed of rock and metal. The four outer planets, Jupiter,
Saturn, Uranus and Neptune, also called the gas giants, are composed
largely of hydrogen and helium and are far more massive than the
terrestrials.

10.  The principal component of the Solar System is the Sun, that
contains 99.86 percent of the system's known mass and dominates
it gravitationally. The Sun's four largest orbiting bodies, the gas
giants, account for 99 percent of the remaining mass, with Jupiter
and Saturn together comprising more than 90 percent.
 Most large objects in orbit around the Sun lie near the plane of
Earth's orbit, known as the ecliptic. The planets are very close to
the ecliptic while comets and Kuiper belt objects are frequently at
significantly greater angles to it.
 All the planets and most other objects also orbit with the Sun's
rotation (counter-clockwise, as viewed from above the Sun's north
pole). There are exceptions, such as Halley's Comet.

11.  Due to the vast distances involved, many representations of the Solar System show
orbits the same distance apart. In reality, with a few exceptions, the farther a planet or
belt is from the Sun, the larger the distance between it and the previous orbit. For
example, Venus is approximately 0.33 astronomical units (AU) farther out from the
Sun than Mercury, while Saturn is 4.3 AU out from Jupiter, and Neptune lies 10.5 AU
out from Uranus. Attempts have been made to determine a correlation between these
orbital distances (for example, the Titius-Bode law), but no such theory has been
accepted.
 Kepler's laws of planetary motion describe the orbits of objects about the Sun.
According to Kepler's laws, each object travels along an ellipse with the Sun at one
focus. Objects closer to the Sun (with smaller semi-major axes) have shorter years.
On an elliptical orbit, a body's distance from the Sun varies over the course of its
year. A body's closest approach to the Sun is called its perihelion, while its most
distant point from the Sun is called its aphelion. Each body moves fastest at its
perihelion and slowest at its aphelion. The orbits of the planets are nearly circular, but
many comets, asteroids and Kuiper belt objects follow highly elliptical orbits.

12. Most of the planets in the Solar System possess secondary systems
of their own. Many are in turn orbited by planetary objects called
natural satellites, or moons, some of which are larger than the
planet Mercury. Most of the largest natural satellites are in
synchronous rotation, with one face permanently turned toward their
parent. The four largest planets, the gas giants, also possess
planetary rings, thin bands of tiny particles that orbit them in
unison.
Structure Contd.

14.  Informally, the Solar System is sometimes divided into separate regions. The inner
Solar System includes the four terrestrial planets and the main asteroid belt. The
outer Solar System is beyond the asteroids, including the four gas giant planets.
Since the discovery of the Kuiper belt, the outermost parts of the Solar System are
considered a distinct region consisting of the objects beyond Neptune.
 Dynamically and physically, objects orbiting the Sun are officially classed into three
categories: planets, dwarf planets and small Solar System bodies. A planet is any
body in orbit around the Sun that has enough mass to form itself into a spherical
shape and has cleared its immediate neighbourhood of all smaller objects. By this
definition, the Solar System has eight known planets: Mercury, Venus, Earth, Mars,
Jupiter, Saturn, Uranus, and Neptune. Pluto does not fit this definition, as it has not
cleared its orbit of surrounding Kuiper belt objects.
 A dwarf planet is a celestial body orbiting the Sun that is massive enough to be
rounded by its own gravity but which has not cleared its neighbouring region of
planetesimals and is not a satellite. By this definition, the Solar System has five
known dwarf planets: Ceres, Pluto, Haumea, Makemake, and Eris.
 Other objects may be classified in the future as dwarf planets, such as Sedna, Orcus,
and Quaoar. Dwarf planets that orbit in the trans-Neptunian region are called
"plutoids". The remainder of the objects in orbit around the Sun are small Solar
System bodies.

15.  Planetary scientists use the terms gas, ice, and rock to describe the various
classes of substances found throughout the Solar System.
 Rock is used to describe compounds with high condensation temperatures or
melting points that remained solid under almost all conditions in the
protoplanetary nebula. Rocky substances typically include silicates and metals
such as iron and nickel. They are prevalent in the inner Solar System, forming
most of the terrestrial planets and asteroids.
 Gases are materials with extremely low melting points and high vapor pressure
such as molecular hydrogen, helium, and neon, which were always in the
gaseous phase in the nebula. They dominate the middle region of the Solar
System, comprising most of Jupiter and Saturn. Ices, like water, methane,
ammonia, hydrogen sulfide and carbon dioxide, have melting points up to a few
hundred kelvins, while their phase depends on the ambient pressure and
temperature. They can be found as ices, liquids, or gases in various places in
the Solar System, while in the nebula they were either in the solid or gaseous
phase.
 Icy substances comprise the majority of the satellites of the giant planets, as well
as most of Uranus and Neptune (the so-called "ice giants") and the numerous
small objects that lie beyond Neptune's orbit. Together, gases and ices are
referred to as volatiles.

16.  The Solar System is also home to two regions populated by smaller objects. The
asteroid belt, which lies between Mars and Jupiter, is similar to the terrestrial planets
as it is composed mainly of rock and metal. Beyond Neptune's orbit lie trans-
Neptunian objects composed mostly of ices such as water, ammonia and methane.
Within these two regions, five individual objects, Ceres, Pluto, Haumea, Makemake
and Eris, are recognized to be large enough to have been rounded by their own
gravity, and are thus termed dwarf planets. In addition to thousands of small bodies in
those two regions, various other small body populations, such as comets, centaurs
and interplanetary dust, freely travel between regions.
 The solar wind, a flow of plasma from the Sun, creates a bubble in the interstellar
medium known as the heliosphere, which extends out to the edge of the scattered
disc. The hypothetical Oort cloud, which acts as the source for long-period comets,
may also exist at a distance roughly a thousand times further than the heliosphere.
 Six of the planets and three of the dwarf planets are orbited by natural satellites,[b]
usually termed "moons" after Earth's Moon. Each of the outer planets is encircled by
planetary rings of dust and other particles.

17. ROTATING PLANETS AROUND THE
SUN

19. The Sun is the Solar System's star, and by far its chief component. Its large mass
(332,900 Earth masses) produces temperatures and densities in its core great
enough to sustain nuclear fusion, which releases enormous amounts of energy,
mostly radiated into space as electromagnetic radiation, peaking in the 400–to–
700 nm band we call visible light.
 The Sun is classified as a yellow dwarf, but this name is misleading as, compared to
the majority of stars in our galaxy, the Sun is rather large and bright. Stars are
classified by the Hertzsprung-Russell diagram, a graph which plots the brightness of
stars with their surface temperatures. Generally, hotter stars are brighter. Stars
following this pattern are said to be on the main sequence, and the Sun lies right in
the middle of it. However, stars brighter and hotter than the Sun are rare, while
substantially dimmer and cooler stars, known as red dwarfs, are common, making up
85 percent of the stars in the galaxy.
 The Sun is growing brighter; early in its history it was 70 percent as bright as it is
today.
 The Sun is a population I star; it was born in the later stages of the universe's
evolution, and thus contains more elements heavier than hydrogen and helium than
older population II stars. This high metallicity is thought to have been crucial to the
Sun's developing a planetary system, because planets form from accretion of "metal .

20.  Along with light, the Sun radiates a continuous stream of charged particles (a plasma)
known as the solar wind. This stream of particles spreads outwards at roughly 1.5
million kilometres per hour, creating a tenuous atmosphere (the heliosphere) that
permeates the Solar System out to at least 100 AU (see heliopause). This is known
as the interplanetary medium. Geomagnetic storms on the Sun's surface, such as
solar flares and coronal mass ejections, disturb the heliosphere, creating space
weather. The largest structure within the heliosphere is the heliospheric current sheet,
a spiral form created by the actions of the Sun's rotating magnetic field on the
interplanetary medium.
 Cosmic rays originate outside the Solar System. The heliosphere partially shields the
Solar System, and planetary magnetic fields (for those planets that have them) also
provide some protection. The density of cosmic rays in the interstellar medium and
the strength of the Sun's magnetic field change on very long timescales, so the level
of cosmic radiation in the Solar System varies, though by how much is unknown.
 The interplanetary medium is home to at least two disc-like regions of cosmic dust.
The first, the zodiacal dust cloud, lies in the inner Solar System and causes zodiacal
light. It was likely formed by collisions within the asteroid belt brought on by
interactions with the planets. The second extends from about 10 AU to about 40 AU,
and was probably created by similar collisions within the Kuiper belt .

22.  The inner Solar System is the traditional name for the region comprising the
terrestrial planets and asteroids. Composed mainly of silicates and metals,
the objects of the inner Solar System are relatively close to the Sun; the
radius of this entire region is shorter than the distance between Jupiter and
Saturn.
 Inner planets
 The four inner or terrestrial planets have dense, rocky compositions, few or
no moons, and no ring systems. They are composed largely of refractory
minerals, such as the silicates which form their crusts and mantles, and
metals such as iron and nickel, which form their cores. Three of the four inner
planets (Venus, Earth and Mars) have atmospheres substantial enough to
generate weather; all have impact craters and tectonic surface features such
as rift valleys and volcanoes. The term inner planet should not be confused
with inferior planet, which designates those planets which are closer to the
Sun than Earth is (i.e. Mercury and Venus).

24.  Mercury (0.4 AU from the Sun) is the closest planet to
the Sun and the smallest planet in the Solar System
(0.055 Earth masses). Mercury has no natural
satellites, and its only known geological features
besides impact craters are lobed ridges or rupes,
probably produced by a period of contraction early in
its history. Mercury's almost negligible atmosphere
consists of atoms blasted off its surface by the solar
wind. Its relatively large iron core and thin mantle have
not yet been adequately explained. Hypotheses
include that its outer layers were stripped off by a giant
impact, and that it was prevented from fully accreting
by the young Sun's energy.

25.  Venus (0.7 AU from the Sun) is close in size to Earth, (0.815
Earth masses) and like Earth, has a thick silicate mantle around
an iron core, a substantial atmosphere and evidence of internal
geological activity. However, it is much drier than Earth and its
atmosphere is ninety times as dense. Venus has no natural
satellites. It is the hottest planet, with surface temperatures over
400 °C, most likely due to the amount of greenhouse gases in
the atmosphere. No definitive evidence of current geological
activity has been detected on Venus, but it has no magnetic
field that would prevent depletion of its substantial atmosphere,
which suggests that its atmosphere is regularly replenished by
volcanic eruptions.

26.  Earth (1 AU from the Sun) is the largest and densest of the
inner planets, the only one known to have current geological
activity, and is the only place in the universe where life is known
to exist. Its liquid hydrosphere is unique among the terrestrial
planets, and it is also the only planet where plate tectonics has
been observed. Earth's atmosphere is radically different from
those of the other planets, having been altered by the presence
of life to contain 21% free oxygen. It has one natural satellite,
the Moon, the only large satellite of a terrestrial planet in the
Solar System.

27.  Mars (1.5 AU from the Sun) is smaller than Earth and Venus
(0.107 Earth masses). It possesses an atmosphere of mostly
carbon dioxide with a surface pressure of 6.1 millibars (roughly
0.6 percent that of the Earth's). Its surface, peppered with vast
volcanoes such as Olympus Mons and rift valleys such as
Valles Marineris, shows geological activity that may have
persisted until as recently as 2 million years ago. Its red colour
comes from iron oxide (rust) in its soil. Mars has two tiny natural
satellites (Deimos and Phobos) thought to be captured
asteroids.

28.  Asteroids are mostly small Solar System bodies composed mainly of refractory rocky
and metallic minerals.
The main asteroid belt occupies the orbit between Mars and Jupiter, between 2.3 and
3.3 AU from the Sun. It is thought to be remnants from the Solar System's formation that
failed to coalesce because of the gravitational interference of Jupiter.
 Asteroids range in size from hundreds of kilometres across to microscopic. All
asteroids save the largest, Ceres, are classified as small Solar System bodies, but some
asteroids such as Vesta and Hygieia may be reclassed as dwarf planets if they are
shown to have achieved hydrostatic equilibrium.
 The asteroid belt contains tens of thousands, possibly millions, of objects over one
kilometre in diameter. Despite this, the total mass of the main belt is unlikely to be more
than a thousandth of that of the Earth. The main belt is very sparsely populated;
spacecraft routinely pass through without incident. Asteroids with diameters between 10
and 10−4 m are called meteoroids.
 Asteroids in the main belt are divided into asteroid groups and families based on their
orbital characteristics. Asteroid moons are asteroids that orbit larger asteroids. They are
not as clearly distinguished as planetary moons, sometimes being almost as large as
their partners. The asteroid belt also contains main-belt comets which may have been
the source of Earth's water.

30.  The outer region of the Solar System is home to the gas giants and their
large moons. Many short period comets, including the centaurs, also orbit in
this region. Due to their greater distance from the Sun, the solid objects in
the outer Solar System contain more ices (such as water, ammonia,
methane, often called ices in planetary science) than the rocky denizens of
the inner Solar System, as the colder temperatures allow these compounds
to remain solid.
 The four outer planets, or gas giants (sometimes called Jovian planets),
collectively make up 99 percent of the mass known to orbit the Sun. Jupiter
and Saturn are each many tens of times the mass of the Earth and consist
overwhelmingly of hydrogen and helium; Uranus and Neptune are far less
massive (<20 Earth masses) and possess more ices in their makeup. For
these reasons, some astronomers suggest they belong in their own category,
“ice giants. All four gas giants have rings, although only Saturn's ring system
is easily observed from Earth. The term outer planet should not be confused
with superior planet, which designates planets outside Earth's orbit and thus
includes both the outer planets and Mars.

31.  Uranus
• Uranus (19.6 AU), at 14 Earth masses, is the lightest of the outer planets.
Uniquely among the planets, it orbits the Sun on its side; its axial tilt is over ninety
degrees to the ecliptic. It has a much colder core than the other gas giants, and
radiates very little heat into space.
• Uranus has 27 known satellites, the largest ones being Titania, Oberon, Umbriel,
Ariel and Miranda.
 Neptune
• Neptune (30 AU), though slightly smaller than Uranus, is more massive
(equivalent to 17 Earths) and therefore more dense. It radiates more internal heat,
but not as much as Jupiter or Saturn.
• Neptune has 13 known satellites. The largest, Triton, is geologically active, with
geysers of liquid nitrogen. Triton is the only large satellite with a retrograde orbit.
Neptune is accompanied in its orbit by a number of minor planets, termed
Neptune Trojans, that are in 1:1 resonance with it.

32.  Jupiter
-- Jupiter (5.2 AU), at 318 Earth masses, is 2.5 times all the mass of all the other
planets put together. It is composed largely of hydrogen and helium.
--Jupiter has 63 known satellites. The four largest, Ganymede, Callisto, Io, and
Europa, show similarities to the terrestrial planets, such as volcanism and internal
heating.[58] Ganymede, the largest satellite in the Solar System, is larger than
Mercury.
 Saturn
• Saturn (9.5 AU), distinguished by its extensive ring system, has several similarities
to Jupiter, such as its atmospheric composition and magnetosphere. Although
Saturn has 60% of Jupiter's volume, it is less than a third as massive, at 95 Earth
masses, making it the least dense planet in the Solar System.
• Saturn has 62 confirmed satellites; two of which, Titan and Enceladus, show signs
of geological activity, though they are largely made of ice. Titan, the second
largest moon in the Solar System, is larger than Mercury and the only satellite in
the Solar System with a substantial atmosphere. rnal heat creates a number of
semi-permanent features in its atmosphere, such as cloud bands and the Great
Red Spot.

34. Comets
• Comet Hale-Bopp
• Comets are small Solar System bodies, typically only a
few kilometres across, composed largely of volatile
ices. They have highly eccentric orbits, generally a
perihelion within the orbits of the inner planets and an
aphelion far beyond Pluto. When a comet enters the
inner Solar System, its proximity to the Sun causes its
icy surface to sublimate and ionise, creating a coma: a
long tail of gas and dust often visible to the naked eye.

36.  The Kuiper belt, the region's first formation, is a great ring of debris similar to the
asteroid belt, but composed mainly of ice. It extends between 30 and 50 AU from
the Sun. It is composed mainly of small Solar System bodies, but many of the
largest Kuiper belt objects, such as Quaoar, Varuna, and Orcus, may be
reclassified as dwarf planets. There are estimated to be over 100,000 Kuiper belt
objects with a diameter greater than 50 km, but the total mass of the Kuiper belt
is thought to be only a tenth or even a hundredth the mass of the Earth. Many
Kuiper belt objects have multiple satellites, and most have orbits that take them
outside the plane of the ecliptic.
 The Kuiper belt can be roughly divided into the "classical" belt and the
resonances. Resonances are orbits linked to that of Neptune (e.g. twice for
every three Neptune orbits, or once for every two). The first resonance begins
within the orbit of Neptune itself. The classical belt consists of objects having no
resonance with Neptune, and extends from roughly 39.4 AU to 47.7 AU.
Members of the classical Kuiper belt are classified as cubewanos, after the first
of their kind to be discovered, (15760) 1992 QB1, and are still in near primordial,
low-eccentricity orbits.

38.  The point at which the Solar System ends and
interstellar space begins is not precisely defined, since
its outer boundaries are shaped by two separate
forces: the solar wind and the Sun's gravity. The outer
limit of the solar wind's influence is roughly four times
Pluto's distance from the Sun; this heliopause is
considered the beginning of the interstellar medium.
However, the Sun's Roche sphere, the effective range
of its gravitational dominance, is believed to extend up
to a thousand times farther.

39.  The heliosphere is divided into two separate regions. The solar wind travels at
roughly 400 km/s until it collides with the interstellar wind; the flow of plasma in
the interstellar medium. The collision occurs at the termination shock, which is
roughly 80–100 AU from the Sun upwind of the interstellar medium and roughly
200 AU from the Sun downwind. Here the wind slows dramatically, condenses
and becomes more turbulent, forming a great oval structure known as the
heliosheath. This structure is believed to look and behave very much like a
comet's tail, extending outward for a further 40 AU on the upwind side but tailing
many times that distance downwind; but evidence from the Cassini and
Interstellar Boundary Explorer spacecraft has suggested that it is in fact forced
into a bubble shape by the constraining action of the interstellar magnetic field.
Both Voyager 1 and Voyager 2 are reported to have passed the termination
shock and entered the heliosheath, at 94 and 84 AU from the Sun, respectively.
The outer boundary of the heliosphere, the heliopause, is the point at which the
solar wind finally terminates and is the beginning of interstellar

41.  The hypothetical Oort cloud is a spherical cloud of up to a trillion
icy objects that is believed to be the source for all long-period
comets and to surround the Solar System at roughly 50,000 AU
(around 1 light-year (LY)), and possibly to as far as 100,000 AU
(1.87 LY). It is believed to be composed of comets which were
ejected from the inner Solar System by gravitational interactions
with the outer planets. Oort cloud objects move very slowly, and
can be perturbed by infrequent events such as collisions, the
gravitational effects of a passing star, or the galactic tide, the
tidal force exerted by the Milky Way.

43.  The Solar System is located in the Milky Way galaxy, a barred spiral
galaxy with a diameter of about 100,000 light-years containing about 200
billion stars. Our Sun resides in one of the Milky Way's outer spiral arms,
known as the Orion Arm or Local Spur. The Sun lies between 25,000 and
28,000 light years from the Galactic Centre, and its speed within the
galaxy is about 220 kilometres per second, so that it completes one
revolution every 225–250 million years. This revolution is known as the
Solar System's galactic year. The solar apex, the direction of the Sun's
path through interstellar space, is near the constellation of Hercules in
the direction of the current location of the bright star Vega. The plane of
the Solar System's ecliptic lies nearly at right angles (86.5°) to the
galactic plane.

44. The Solar System's location in the galaxy is very likely a factor in the
evolution of life on Earth. Its orbit is close to being circular and is at roughly
the same speed as that of the spiral arms, which means it passes through
them only rarely. Since spiral arms are home to a far larger concentration
of potentially dangerous supernovae, this has given Earth long periods of
interstellar stability for life to evolve. The Solar System also lies well
outside the star-crowded environs of the galactic centre. Near the centre,
gravitational tugs from nearby stars could perturb bodies in the Oort Cloud
and send many comets into the inner Solar System, producing collisions
with potentially catastrophic implications for life on Earth. The intense
radiation of the galactic centre could also interfere with the development of
complex life. Even at the Solar System's current location, some scientists
have hypothesised that recent supernovae may have adversely affected
life in the last 35,000 years by flinging pieces of expelled stellar core
towards the Sun as radioactive dust grains and larger, comet-like bodies.
GALACTIC CONTEXT

46. THANKS