Download The Dwarf Planets

The Dwarf Planets
Mike Brown
On August 24th 2006 the word "planet" was given its first-ever scientific definition by a vote of
the International Astronomical Union. With the raising of a few yellow cards in Prague, Pluto
was demoted from full-fledged planet to "dwarf planet." Eris, originally called 2003 UB313,
sometimes called Xena, sometimes called the "10th planet," which in many ways precipitated
this final debate, becomes the largest known dwarf planet. Unless astronomers revisit this issue
at some point in the future, it is unlikely that there will ever be more than eight planets. While
some still continue to mourn the loss of Pluto from the pantheon of planets, it is much more
interesting to consider this new class of dwarf planets, instead.
What is a dwarf planet?
When the final vote on the definition of "planet" was made, and the eight dominant bodies in the
solar system were declared (quite rationally) a class separate from the others, a new class of
objects was defined. The "dwarf planets" are all of those objects which are not one of the eight
dominant bodies (Mercury through Neptune) yet still, at least in one way, resemble a planet. The
best definition heard so far is that a dwarf planet is something that looks like a planet, but is not a
planet. The dwarf planets are bodies in the solar system which are large enough to become round
due to their own gravitational attraction. Why do astronomers care about round? If you place a
boulder in space it will just stay whatever irregular shape it is. If you add more boulders to it you
can still have an irregular pile. But if you add enough boulders to the pile they will eventually
pull themselves into a round shape. This transition from irregularly shaped to round objects is
important in the solar system, and, in some ways, marks the transition from an object without
and with interesting geological and planetary processes occurring (there are many many other
transitions that are equally important, however, a fact that tends to be ignored in these
discussions).
How many dwarf planets are there?
There are two ways to look at this question. First is to ask: according to the official list kept by
the IAU, how many dwarf planets are there? The current answer (as of 1 April 2007) is only
three. The asteroid Ceres is the only asteroid known to be round. Pluto is also considered a dwarf
planet. And Eris, a little larger than Pluto, is a dwarf planet also. Three is all the IAU will
currently deal with.
Reality, however, does not pay much attention to official lists kept by the IAU or by anyone else.
A more interesting question to ask is: how many round objects are there in the solar system that
are not planets? These are, by the definition, dwarf planets, whether or not they ever make it to
any officially sanctioned list. If the category of dwarf planet is important, then it is the reality
that is important, not the official list.
So how many dwarf planets are there? Ceres is still the only asteroid that is known to be round.
After that it gets complicated. All of the rest of the new dwarf planets are in the distant region of
the Kuiper belt, where we can't actually see them well enough to know for sure if they are round
or not.
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The Dwarf Planets
While we can't see most of the objects in the Kuiper belt well enough to determine whether they
are round or not, we can estimate how big an object has to be before it becomes round and
therefore how many objects in the Kuiper belt are likely round. In the asteroid belt Ceres, with a
diameter of 900 km, is the only object large enough to be round, so somewhere around 900 km is
a good cutoff for rocky bodies like asteroids. Kuiper belt objects have a lot of ice in their
interiors, though. Ice is not as hard as rock, so it less easily withstands the force of gravity, and it
takes less force to make an ice ball round. The best estimate for how big an icy body needs to be
to become round comes from looking at icy satellites of the giant planets. The smallest body that
is generally round is Saturn's satellite Mimas, which has a diameter of about 400 km. Several
satellites which have diameters around 200 km are not round. So somewhere between 200 and
400 km an icy body becomes round. Objects with more ice will become round at smaller sizes
while those with less rock might be bigger. We will take 400 km as a reasonable lower limit and
assume that anything larger than 400 km in the Kuiper belt is round, and thus a dwarf planet.
How many objects larger than 400 km are there in the Kuiper belt? We can't answer this question
precisely, because we don't know the sizes of more than a handful of Kuiper belt objects (for an
explanation why, see the discussion on the size of Eris), but, again, we can make a reasonable
guess. If we assume that the typical small Kuiper belt object reflects 10% of the sunlight that hits
its surface we know how bright a 400 km object would be in the Kuiper belt. As of late August
2006, 44 objects this size or larger in the Kuiper belt (including, of course, Eris and Pluto), and
one (Sedna) in the region beyond the Kuiper belt. In addition our large ongoing Palomar survey
has detected approximately 30 more objects of this size which are currently undergoing detailed
study.
We have not yet completed our survey of the Kuiper belt. Our best estimate is that a complete
survey of the Kuiper belt would double this number.
For now, the number of known objects in the solar system which are likely to be round is 53,
with the number jumping to 80 when the objects from our survey are announced, and to ~200
when the Kuiper belt is fully surveyed.
Beyond the Kuiper belt there may be even more dwarf planets than in the Kuiper belt. Our best
guess is that the region where Sedna resides could contain another ~2000 dwarf planets.
The new dwarf planets in the solar system are very different from the previous 8 planets. Most
are so small that they are smaller across than the distance from Los Angeles to San Francisco.
They are so small that about 30,000 of them could fit inside the earth.
What does the new solar system look like?
Here is the before (black circles with nine planets) and after (add red ellipses to show the dwarf
planets) views of the solar system:
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(images may be freely used; credit: Mike Brown, Caltech)
In order from closest to furthest, the dwarf planets are shown below (with the planets, shown for
comparison, in blue). A few of them have been studied well enough that we know interesting
details. Click the links to learn more.......
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The Dwarf Planets
Object name
Average distance from sun
estimated size
(semi major axis, AU)
(km)
Mercury
0.39
4880
Venus
0.72
12,100
Earth
1.0
12,700
Mars
1.5
6780
Ceres
2.8
950
Jupiter
5.2
139,800
Saturn
9.6
116,500
Uranus
19.2
50,700
Neptune
30.0
49,200
2004TY364
38.72
540
2002KX14
39.01
560
2002XV93
39.22
430
2003VS2
39.27
610
1999TC36
39.27
440
2001QF298
39.30
490
Orcus
39.34
1100
2003AZ84
39.45
710
Pluto
39.53
2300
Ixion
39.65
980
Huya
39.76
480
2005RN43
41.53
740
1995SM55
41.64
470
2002MS4
41.90
740
2004SB60
41.97
560
2004GV9
42.23
680
2002UX25
42.53
810
Varuna
42.90
780
2002TX300
43.11
800
1996TO66
43.19
540
2003OP32
43.24
650
2003EL61
43.31
2000
Quaoar
43.58
1290
2003QW90
43.65
560
1999CD158
43.69
410
1997CS29
43.87
410
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2000CN105
44.65
430
1998WH24
45.56
450
2005FY9
45.66
1600
2004PR107
45.75
520
2003MW12
45.94
740
2002CY248
46.18
410
2002KW14
47.08
510
2002AW197
47.30
940
2002WC19
47.67
410
2003QX113
49.56
450
2003FY128
49.77
430
2001UR163
51.40
620
2002TC302
55.02
710
1999DE9
55.72
490
2004XR190
57.36
540
2000YW134
57.77
430
Eris
67.69
2400
2005RM43
89.73
560
Sedna
486.0
1800
Who has discovered dwarf planets?
Many people have found dwarf planets, starting with the discovery of Ceres by Piazzo in 1801,
continuing with Pluto by Tombaugh in 1930, and the moving to the discovery of the many many
objects in the Kuiper belt beginning in 1992. For the likely dwarf planets listed above, here is the
list of discoverers (some planets were discovered by teams which change a bit, in general the
team name or the team leader is listed. Sometimes no discoverer is recorded):






Brown et al.: 15 dwarf planets
Deep Ecliptic Survey: 8 dwarf planets
Near Earth Asteroid Tracking Survey: 4 dwarf planets
Spacewatch: 4 dwarf planets
Jewitt et al.: 3 dwarf planets
Rupenstein, Ferrin, Danzl, Roe, Luu, Piazzo, Tombaugh: 1 dwarf planet each
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