Figure 1. Subterrestrial planets orbiting Sun-like
stars, with the Earth included for comparison.
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Over the past few weeks, Kepler Mission scientists have reported
two new transiting systems containing members of a tiny but growing extrasolar
population: planets smaller than Earth, which I christen “subterrestrials” (Figure 1). Although objects of this
size account for more than one-third of the planets and all of the spheroidal
moons and dwarf planets in the Solar System, they represent only 2% of all
transiting planets, and less than 1% of the vaguely defined census of confirmed
exoplanets. (I say “vaguely” because the Extrasolar
Planets Encyclopaedia currently lists 861 exoplanets discovered by all
methods, but it omits some of the newest and smallest transiting subterrestrials.
Qui peut dire pourquoi?)
The two newest systems are especially interesting (Figure 2). Kepler-68,
the subject of a forthcoming article by Ronald Gilliland and colleagues,
centers on a G-type star almost identical in mass to our Sun, although it is
evidently older, hotter, and more bloated in radius. The star’s three
companions define an inner system that includes two transiting low-mass planets
(b and c) and an outer system that includes a single non-transiting gas giant
(d) whose orbital period is about 580 days. Kepler-68 therefore meets my
definition of a mixed-mass
system. Still better, it joins the exclusive club of extrasolar systems
that contain at least one gas giant and at least two low-mass planets (like our
Solar System). Since most known mixed-mass systems (e.g., 55 Cancri, Mu Arae) contain
only one low-mass planet, that club previously included just three members: GJ
876, HD 10180, and Kepler-30. Even with its enlarged membership, only two systems,
HD 10180 and Kepler-68, present low-mass planets in adjacent orbits plus a gas
giant on a wider orbit. This arrangement is one of the most
distinctive features of the architecture of our Solar System.
Figure 2. Kepler-37 and Kepler
68, two new systems with subterrestrial and Super Earth planets, represented at
the same scale. Orbital dimensions are measured in astronomical units (AU). Red
lines mark the planets of Kepler-68; blue lines mark those of Kepler-37. Pink
fill indicates rock/metal composition; purple indicates an additional water or
hydrogen envelope, or both. Only one of these objects has an estimated mass: Kepler-68b,
at 8.3 Earth masses (Mea). Kepler-68 also harbors a third planet, a
Jupiter-mass giant with a semimajor axis of 1.4 AU, similar to the orbit of
Mars.
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Nevertheless, it was the second new subterrestrial system that got all the headlines: Kepler-37, announced in Nature (Barclay et al. 2013), featured in Wikipedia news, and reported in global media outlets ranging from the Los Angeles Times to the Malaysia Chronicle. The system’s primary appears to be a K-type star whose mass is 80% of Solar (0.80 Msol). Three low-mass planets have been detected, all transiting and all confined within an astrocentric radius of 0.21 astronomical units (AU). The international flood of headlines originated in the fact that Kepler-37b is the smallest exoplanet yet detected (der kleinste Exoplanet! il più piccolo esopianeta!) – so small that it barely exceeds the diameter of the Earth’s Moon. Its characterization represents a new frontier in exoplanetary astronomy.
With these additions we now have at least seven
subterrestrial exoplanets, orbiting in four different Kepler multiplanet
systems (Table 1). Their host stars
include a very small M dwarf, Kepler-42, which is similar in mass to GJ 1214 and
Barnard’s Star; a
K-type star, Kepler-37; a G-type star, Kepler-20,
which is similar in metallicity to our Sun but less massive by 9%; and a more
massive and metal-rich G-type star, Kepler-68. The range of masses and
metallicities represented by this group implies that low-mass rocky planets
like those in our Solar System are common in the Milky Way Galaxy, whether in
habitable orbits or not.
Table 1. All confirmed subterrestrial
exoplanets. Column 2 lists the planet radius in Earth units (Rea); column 3,
the orbital period in days; column 4, the semimajor axis in AU; column 5, the
estimated equilibrium temperature in Kelvin; column 6, the distance of the star
in parsecs; column 7, the stellar metallicity; column 8, the stellar mass in
Solar units (Msol); and column 9, the stellar radius in Solar units (Rsol).
------------------------------
With their high equilibrium temperatures and small radii,
most or all of the objects in Table 1 must be rocky. Planets so lightweight
have difficulty retaining volatiles; they cannot sustain hydrogen envelopes.
Most, if not all, are also too warm to retain ices. They may be cousins of
Mercury, which after all is one of the Earth’s siblings.
Another potential subterrestrial object, KIC 12557548 b, has
been interpreted as a solitary companion to a K-type star of 0.70 Msol located about
470 parsecs away (Rappaport et al. 2012). The star exhibits unusual transits at
intervals of less than 16 hours: regular in period but irregular in depth. Two
studies have explained this behavior as the signature of a low-mass rocky
planet undergoing catastrophic disintegration (Rappaport et al. 2012,
Perez-Becker & Chiang 2013). In these models, the disintegrating planet is less
massive than Mars. Successive transits vary in depth because the planet constantly
sheds a cloud of dust that streams after it like a comet’s tail. As the cloud
disperses semi-chaotically, it varies in size, and the area of the star
occulted during each transit varies along with it. Perez-Becker & Chiang
detail a scenario in which the planet was originally similar to Mercury (0.06
Mea) but by now has lost 80% of its mass, so that it is as lightweight as the
Moon. At the implied rate of loss, this object will disappear completely within
100 million years. Given its peculiar physical status, I don’t include it in my
personal census of subterrestrials.
The emergence of this new subpopulation of small planets adds
substantially to our understanding of the likely distribution of Earth-like
planets in the Galaxy. We now know that low-mass planets can range continuously
from less than the mass of Mercury to twice the mass of Uranus. They occur
preferentially alongside similar planets, so that a single system (e.g.,
Kepler-20 or Kepler-68) can harbor both rocky terrestrial planets (like Venus) and
more massive gas dwarfs (like Uranus) in close proximity. Unfortunately, the
known terrestrials and subterrestrials are still confined to short-period
orbits, with very few detected on orbits longer than 100 days. Further
collection and analysis of Kepler data should correct at least some of that
bias.
REFERENCES
Barclay T, Rowe
JF, Lissauer JJ, Huber D, Fressin F, Howell SB, and 58 others. (2013) A
sub-Mercury-sized exoplanet. Nature
494, 452-454.
Gilliland RL,
Marcy GW, Rowe JF, Rogers L, Torres G, Fressin F, and 27 others. (2013) Kepler-68:
Three planets, one with a density between that of Earth and ice giants. Astrophysical Journal, in press.
Perez-Becker D, Chiang E. (2013) Catastrophic evaporation of rocky planets. Monthly Notices of the Royal Astronomical
Society, in press.
Rappaport S, Levine A, Chiang E, El Mellah I, Jenkins J, Kalomeni
B, Kotson M, Nelson L, Rousseau-Nepton L, Tran K. (2012) Possible
disintegrating short-period Super-Mercury orbiting KIC 12557548. (2012) Astrophysical Journal 752, 1.
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