I was watching a youtube from early in the Kepler mission (Jon Jenkins ;
http://www.youtube.com/watch?v=UNGviQ0LPDQ
if you wanna look at it), and it set out the "critical questions" the
mission (now unfortunately over) was intended to answer. I will essay to
say what they found out, based on listening to a number of NASA and
other science website lectures on the subject.
- Are terrestrial planets common or rare?
- What are their sizes and orbital distances?
- How often are they in the habitable zone?
First,
it's worth pointing out what Kepler was for and what it did in the
broadest terms. It's a space telescope, in solar orbit, that looked at
only one small patch of sky in the Constellation Cygnus, along the disk
of the Milky Way. It critically examined the "sunlike" stars in that
field of view out to an effective distance of about 3000 light years.
That's 150,000 stars, more or less similar to the Sun. The point was to
try to detect planets, and create some meaningful statistics about what
it found.
Turns out what I'll call terrestroid (i.e., small, rocky) planets (e.g., Mercury, Venus, Earth, Mars) are very common.
Kepler's methodology, which is detection of transiting planets
(crossing the disk of their star as seen from Earth) involves a
selection effect: only quite flat ecliptic-plane systems are detected,
and only something like 2 or 3% at most of stars viewed in the Kepler
field of view will be oriented correctly for detection. Single stars are
also heavily favored, because binary star planetary disks, even though
the stars (it turns out) may often have planets, are unlikely to be flat
enough to have transiting planets.
Still, it's thought that the systems Kepler has and will have
detected (once all the data is processed), are relatively well
representative of sunlike star systems in general. They found that small
rocky planets are actually much more common than gas giants (in the
Solar System we have four of each; a typical system might have four or
five dense rocky worlds and only 1 or 2 gas planets, and there is not a
preference for the rocky worlds to be close in, as formerly thought).
So, from this point of view, very roughly earthlike worlds should be
common. The question is implicit, what percentage of sunlike stars have
planets at all? ... and the answer seems to be most of them, although
the exact percentage is not really clear from Kepler data.
Unfortunately, the one type of planet that would be most interesting,
which is small planets, in the habitable zone of sunlike stars, and with
an orbital period approximately similar to Earth's, is a type that the
mission did not detect well, because it didn't have a long enough time
to form a good baseline. Based on what was seen, there's good reason to
believe that such planets (between let's say .9 and 1.5 Earth diameters,
and in the zone where water can be liquid on the surface) are not
particularly rare. A rough (but informed) guess would be maybe 2 to 5%
of sunlike stars have such a planet.
Of note, in the Solar System Earth is the largest of the terrestroid
planets, but in most of these systems, rocky planets larger than Earth,
up to 2½ Earth diameters (still small enough NOT to have retained their
hydrogen envelopes, like Neptune or Uranus), are common. Such planets
have been widely labeled "super-Earths" in the popular scientific
literature. Various models have been proposed for what the implications
of the greater mass and size of these planets would be, but there's a
good deal of uncertainty still.
- What is their dependence on stellar properties?
This
question is less clearly answered. Kepler did not look at stars dimmer
than about K5, nor brighter than F0, so it is intrinsically limited to a
category of stars that are actually quite a bit brighter than
most stars,
which are red dwarfs, on average. Turns out (from other detection
methods) that red dwarfs almost always have planets, and the sunlike
stars mostly do, too. The "habitable zones" of dimmer stars are very
narrow, so it remains likely that sunlike stars are a good deal more
likely to have liquid water surface rocky planets than are much dimmer
stars. But since dimmer stars (not only the M dwarfs but the
dimmer-range sunlike dwarfs, say from G5 to K5) are more common, it's a
safe bet that the median, or typical, earthlike world with seas, clouds,
mountains, plate tectonics, etc., (let's call them "First Order
Earthlike;" the presence of life being another matter), will orbit a
star dimmer than the Sun. Just exactly how those numbers will work out
is still somewhat uncertain.
Binary stars do, it seems, often have planets (most of this
information comes from other planet detection regimes), so it would
appear that at least some earthlike worlds could be "Tattooines"
(planets orbiting two closely separated stars), or could orbit one of
two or more very widely separated stars in a single system (e.g., Alpha
Centauri, where planets have been detected). But these, it seems safe to
say, will be the exceptions: habitable planets are more likely to be
found orbiting single stars, probably by a significant margin.
- Bottom line question: Are we alone?
Unfortunately,
unless there's a big surprise in the final reports, it doesn't appear
that Kepler is going to answer this question. There are a number of
suggested methods of teasing from the data information about whether
life could exist on a planet that's been detected. The atmosphere of a
planet transiting a star can affect the spectrum of the star, and from
that comparison such things as the presence of ozone in the atmosphere
could theoretically be inferred. A planet, for example, that had both
methane and ozone detectable in its atmosphere would be so seriously in
chemical disequilibrium that, albeit controversially, such a detection
would be widely accepted as definitive proof of the existence of life
there.* But it hasn't been demonstrated, so far. So while Kepler does not
provide any reason to infer that life is not likely, or not present on
one or more of the detected worlds, it doesn't confirm that, either. As
for the detection of intelligent life; well, not. Again, nothing to rule
it out, but nothing to confirm it either.
♦♦
*The point is that if chemicals that will react with each other strongly
both exist in the atmosphere of a planet, one or both of them must be
continuously replenished, and in the case of oxygen (which yields ozone
in the stratosphere), that can pretty much only be life, at least over
time... if there were only one such detection, it could be explained
away by transitory geological phenomena, but if the signature were
detected in several different instances, the conclusion would be that it
could pretty much
only be a biosignature.