ASTR 1210 (O'Connell) Study Guide
21: INTERPLANETARY MATTER
Comet McNaught at Sunset (2007; Akira Fujii)
There is a smattering of material lying between and around the 8 planets.
This "interplanetary matter" (IPM) is mostly left
over from the early protoplanetary phase of the Solar System. It consists of
icy or rocky bodies that were never permanently incorporated into
the planets or which were produced by the fragmentation of larger
This would seem to be a boring footnote to the planets
themselves...except for two things:
- Some of the most beautiful and spectacular astronomial
events involve the IPM, for example Comet McNaught (shown above)
or the 1833 Leonid meteor storm shown below; and...
- This material poses the greatest natural threat to the survival
of life on this planet.
The IPM contains material that ranges from satellite-sized objects through
chunks the size of skyscrapers to tiny dust grains and atoms of gas.
The total mass in the IPM is smaller than Jupiter's. But even
relatively small bodies traveling at typical orbital speeds of over
50,000 miles per hour can have
"large impacts" on other objects, like the
The gas is mostly the expanding outer atmosphere of the Sun (the
About 50 tons of IPM, mostly dust, rains down on the Earth's
surface every day.
Scattering of sunlight by interplanetary dust
is responsible for the "Zodiacal
Light," which can be easily seen from dark locations at certain times
of the year.
Although larger chunks of IPM material (10-m or bigger) can be found
everywhere in the Solar System, they are concentrated in two main
The nomenclature for the IPM is currently in a mess, with various new
and traditional designations being used in overlapping ways. We focus
here on the following three components of the IPM:
- The "asteroid belt", lying between the orbits of Mars and Jupiter
(2-3.5 AU from the Sun). Dominated by rocky or metallic material like the
- The "Trans-Neptunian" region: beyond the orbit of Neptune
(30 AU). Dominated by icy material, like the satellites of the
Jovian planets. Includes the "Kuiper Belt Objects"
(see Study Guide 20) and
Spacecraft have been sent (either as a prime or secondary mission) to
rendezvous with a number of asteroids and comets since 1986.
Here is a montage
of the visitees through 2010.
- "Asteroids": rocky/metallic bodies ranging down to about 50-m diameter
- "Comets": produced by icy bodies, mostly between 50-m and 10-km diameter, which
enter the inner solar system
- "Meteoroids": either rocky or icy bodies, less than 50-m diameter
Closeup image of asteroid Lutetia, about 75 miles
on its longest diameter (Rosetta Mission, 2010)
- Bode's "Law" concerning the systematic spacing of planetary orbits
suggests a "missing" planet between Mars & Jupiter.
- The first asteroid, Ceres (975 km diameter), was discovered in
this region in 1801. This inspired a number of systematic searches for
asteroids, continuing to today. Ceres is large enough and round enough
to now be classified as a "dwarf planet"; but none of the other
asteroids are in this category. Traditionally, however, asteroids
were always regarded as "minor planets."
- As of 2012, there are over 310,000 identified asteroids with known orbits
- Asteroids are most easily identified by their motion with respect to
the background stars over periods of hours.
Here is a sample animation of
asteroid detection with an electronic camera [University of Washington].
Here is a video
(266KB) of asteroid Eros' motion as seen in a small, Earth-based
Planetary orbits showing location
of Asteroid and Kuiper belts (Addison-Wesley)
- Usually only modestly elliptical and lying close to the
- Most fall in the "main
asteroid belt," lying 2-3 AU from the Sun, between Mars & Jupiter.
(See drawing above).
- The main belt probably represents a region of the protoplanetary
nebula where Jupiter's gravity prevented accumulation of a single
- There are over 9300
Asteroids, with orbits that approach Earth's
orbit or actually cross it. Over 900 have diameters of 1 km or
larger. The best known group are called "Apollos" after the prototype.
These are potentially
dangerous to us. More about this in Study
a remarkable snapshot plot of the current location of known asteroids in the inner Solar
- < 1 to almost 1000 km diameter. The three largest asteroids
are Ceres (975 km). Pallas and Vesta (both 570 km).
- Rocky/metallic materials but several distinct types
- Crude determination of composition is possible
from the reflectance spectrum of an asteroid's solid surface.
- Most common are carbon-rich ("C")
objects, with dark surfaces; others are stony ("S") or metallic
- A handful of asteroids have been imaged by spacecraft or radar,
but most shapes are inferred from variations in brightness as
- Asteroids are mostly irregular in shape (see
and covered by impact craters
- The more massive asteroids tend to be more spherical
- Most are fragments from shattered rocky planetesimals from those
inner regions of the solar nebula that never accreted into planets.
Collisions cause continual
"grinding down" to
- C-types were the least affected (processed) by interactions with
each other or the pressure/heat of protoplanetary interiors. They
yield important information on physical conditions in the primitive
- Asteroids with substantial metallic inclusions are from larger
proto-planetary objects which partially melted &
Topographic map of Vesta showing two large impact basins.
Altitude range (blue to red) spans 25 miles (Dawn Mission).
- The first good pictures of asteroids were Viking Mission images
of Phobos and Deimos, the satellites of Mars. These are "domesticated" asteroids (i.e. captured by a
- An image of the "wild" asteroid Ida taken by the Galileo
mission during its traverse of the asteroid belt is shown
here. Ida is a large, elongated (35 x
13 miles) stony asteroid with a heavily cratered (old) surface and has
its own satellite(!), Dactyl (the starlike speck to the right of
- NEAR (the Near
Earth Asteroid Rendezvous) mission, completed a close-up study of the
asteroid Eros in 2003. This was the
first spacecraft to orbit and later to land on an
- Eros is one of the largest "near-Earth" asteroids, coming within 0.15
AU (14 million miles) of Earth. It is potato-shaped (21x8x8 miles)
"S"-type asteroid and rotates once in 5 hours.
- NEAR went into orbit around Eros on February 14, 2000 (get it?). It
spent 12 months in orbit around the asteroid (distances 3-100 miles), and
was then directed to soft-land on its surface.
- The Dawn
spacecraft went into orbit around Vesta, the second largest asteroid,
in July 2011 and delivered thousands of observations before leaving
in August 2012 to rendezvous with Ceres. Visit the mission site for a
large collection of images and videos.
Comet West 1975, showing dust (white) and ion (blue) tails (J. Laborde)
Comets are the effluent of icy planetesimals from the cold,
outer regions of the solar system that evaporate when they get within
several Astronomical Units of the Sun, producing a
gaseous coma and sometimes tails.
- Early interpretation: atmospheric exhalations.
- Tycho (1577) demonstrates that comets are astronomical objects, lying
beyond the Moon.
- Halley (1704) uses the Newtonian theory of gravity to interpret 4
comets as the same object in an elliptical orbit with semimajor axis
18 AU, period 76 yr. Correctly predicts return (1759).
- Highly elliptical; at all angles to ecliptic. Here is a chart of the
orbit of Halley's Comet.
- Main reservoirs:
the Oort Cloud (~spherical, enormous, ~ 50,000 AU) and the
Kuiper Belt (more flattened, centered on ecliptic plane, ~ 50
AU size). These contain trillions of comet nuclei (icy planetesimals).
The total mass in Kuiper Belt and inner Oort Cloud objects is probably many
times the combined mass of the asteroids.
- Most comets have very long periods. Comets obey Kepler's Laws,
as long as they are not disturbed by planets, so an orbit size of
10000 AU's implies a period of 1,000,000 years.
- Only comets with small (< 20 AU) orbits have been observed on
more than one solar passage; these are called "periodic" comets.
Halley's Comet is the most famous
- Long period orbits can be shifted by the gravitational field of planets,
especially Jupiter, into shorter period ones.
- The brightness and size of a comet as seen from Earth depends on
both the comet's orbit around the Sun and the location of Earth in
its orbit. See this animation
of the passage of Hale-Bopp in 1997.
- Nucleus: best characterized as a "dirty snowball"--mainly ices with embedded
dust grains; typical size 0.5-10 km diameter.
- The surface of the comet nucleus begins to evaporate when < 3 AU
from Sun, producing a gaseous "coma" typically 106 km in
diameter. Here is a pictorial
summary of comet evolution.
Here is a
video showing gaseous and dust outbursts from the nucleus of comet
Tempel-1 (from the Deep Impact mission)
- Tail(s) emerge from the coma: these are cold, but they
reflect/fluoresce sunlight and so look "flamelike"
- Tails point roughly away from the sun, not away from the comet's motion
- The tails of bright comets can be up to 1 AU in length
- Gas (ion) tail: bluish, straight, complex structure. Dragged back
by solar wind. Hale-Bopp (at right) had nicely separated ion
and dust tails.
- Dust tail: dust grains, yellowish-whiteish, smooth &
broad. Driven back by radiation pressure of sunlight.
Mission flew through the tail of comet Wild 2, trapping dust
particles in a gel, and returned the sample to Earth in 2006.
Analysis showed the presence of many organic molecules and evidence
for liquid water on the comet nucleus at some time in the past.
- Comet nuclei disintegrate if overheated by the Sun. Some collide
with the Sun. Satellite observatories that monitor the sun have picked
up hundreds of these, many not otherwise detected because they were too
faint until they approached the Sun. Here is a video compilation of comet-Sun passages or strikes.
Most comets are faint and only visible in telescopes. There are
typically 20 of these observable each year. Brighter, naked-eye
comets are less frequent---one every few years on average. The most
spectacular comets, like Hale-Bopp are usually first-time
visitors to the inner Solar System. Here are some well-known bright
Comet (1910, 1986, 2062...). An "Armada" of spacecraft sent
during the 1986 passage confirms the dirty snowball model
The image of the nucleus of Halley's Comet at right, taken by the
Giotto spacecraft (1986), shows an elongated, 7 mi long object, with a
dark crust (reflecting less light than does asphalt) and gas jets.
Click on the image for a labeled diagram.
This was the first resolved image of
a comet nucleus. Spacecraft have since obtained images of 4 more.
A montage is shown here.
- Hale-Bopp, the "Great
Comet of 1997"
Orbit: semimajor axis 260 AU; period about 2400 years
Closest approach to Earth: 1.3 AU (March 22, 1997)
Best Web-available pictures:
The Deep Impact Mission
- The Deep Impact spacecraft was sent to rendezvous with the 6.5-km
nucleus of comet Tempel-1. It carried an impactor unit that
was sent to collide with the nucleus as a means of probing its
structure. A perfect hit was accomplished at 23,000 mph on July 4,
2005, blasting material off the comet nucleus and allowing analysis of
its composition. Complete information is at
the Deep Impact
Videos of the mission:
Meteoroids are smaller interplanetary bodies, of both icy and
rocky/metallic types. The boundary in size between these and the larger
types of IPM bodies is arbitrary, but here we will take it to be 50-m
Meteors (aka "shooting stars") are the incandescent trails of
tiny meteoroids burning up at high altitudes in the Earth's
- Meteoroids enter Earth's atmosphere at orbital velocities of
~ 100,000 mph
- Smaller objects burn up, producing a fiery streak and occasionally
airborne explosions. A bright meteor has a typical
mass of ~ 1 gram. There are typically about 10 meteors per hour visible
from any location under good sky conditions.
- "Meteor Showers" (concentrations) occur when Earth passes
through the denser debris lying along the orbit of a comet. E.g.: the
Perseids (~ Aug 12; from Comet Swift-Tuttle); the Orionids (~ Oct 22;
from Comet Halley). Rates can be over 1000 per hour.
- The Leonids have produced some of the best showers, starting in
1833 with a meteor
"storm." The picture above right shows the 1833 storm over Niagara
showers occurred in 1998 and 2001. (Shower maximum is Nov. 17-18
- "Meteorites" are meteoroids that survive to reach the ground; they are rocky
or metallic (icy types are destroyed). A slice through a metallic
meteorite is shown at right.
- Meteorites are predominantly samples of asteroidal
material. They are highly valuable for insights into properties
of otherwise mostly unreachable extraterrestrial objects.
- "Carbonaceous condrites" are fragments of "C" asteroids. These
are especially important because they yield information on
the primitive protoplanetary disk.
- Remarkably, we have found meteoritic samples of both the Moon and
Mars (the "SNC" meteorites, see Guide 17).
Reading for this lecture:
Study Guide 21
Bennett textbook, Chapter 12
Reading for next lecture:
Study Guide 22
Bennett textbook, Chapter 12
April 2013 by rwo
Asteroid 1997XF-11 animation courtesy of Eric Deutsch (University
of Washington). Telescope video of Eros copyright © 1998 by
Text copyright © 1998-2013 Robert W. O'Connell. All rights
reserved. These notes are intended for the private, noncommercial use
of students enrolled in Astronomy 1210 at the University of Virginia.