Issue |
A&A
Volume 521, October 2010
|
|
---|---|---|
Article Number | A76 | |
Number of page(s) | 6 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201014955 | |
Published online | 22 October 2010 |
Limits on the orbits and masses of moons around currently-known transiting exoplanets
C. Weidner - K. Horne
Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK
Received 7 May 2010 / Accepted 20 July 2010
Abstract
Aims. Current and upcoming space missions may be able to
detect moons of transiting extra-solar planets. In this context it is
important to understand if exomoons are expected to exist and what
their possible properties are.
Methods. Using estimates for the stability of exomoon orbits
from numerical studies, a list of 87 known transiting exoplanets is
tested for the potential to host large exomoons.
Results. For 92% of the sample, moons larger than Luna can be
excluded on prograde orbits, unless the parent exoplanet's internal
structure is very different from the gas-giants of the solar system.
Only WASP-24b, OGLE2-TR-L9, CoRoT-3b and CoRoT-9b could have moons
above 0.4 ,
which is within the likely detection capabilities of current
observational facilities. Additionally, the range of possible orbital
radii of exomoons of the known transiting exoplanets, with two
exceptions, is below 8 Jupiter-radii and therefore rather small.
Key words: astrobiology - planets and satellites: detection - planets and satellites: dynamical evolution and stability - planets and satellites: formation
1 Introduction
Currently more than 460 exoplanets have been detected through
various methods. With improving instrument precision smaller
and less massive objects are or will be soon accessible
observationally. With current instruments like Kepler it should even be
possible to detect moons of exoplanets
(Simon et al. 2009,2007; Kipping et al. 2009; Sartoretti & Schneider 1999; Kipping 2009). But as most planets are found by
methods most sensitive to massive planets with a small semi-major axis
(``Hot-Jupiters'') the question arises not only if it is possible to
detect exomoons but also how likely it is for them to form and survive in
the first place. Several studies (Domingos et al. 2006; Barnes & O'Brien 2002) explore the
stability of orbits around gas giants.
In this contribution we apply to a sample of observed exoplanets the results of Domingos et al. (2006) on the stability of moons around gas giants. Our sample (Table 1) includes all published transiting exoplanets for which the mass and radius of the planet and the host star, and the orbital parameters are all reasonably well known.
2 Stability domains for exomoons
The region of orbital stability around a close-in gas-giant planet is
set by two radii. We assume that the smallest orbit is set by the
Roche-radius. Any moon larger than a few km within the Roche-limit of
its planet would be torn apart by the tidal forces between the planet and
the moon. The Roche-radius,
,
depends mainly on the
density of the two interacting objects and can be written for
fluid-like objects as (Binney & Tremaine 1987):
where






The outer limit for stable orbits of a moon around an exoplanet is
the so-called Hill-radius, which defines the sphere in which the
gravitational pull of the planet on the moon is larger than that of
the star. The Hill-radius is given as (Burns 1986):
where

By using numerical integrations of the equations of motion,
recent studies (e.g. Barnes & O'Brien 2002) found that the Hill-radius
over estimates the maximum stable orbital radius by a factor
f. Domingos et al. (2006) studied this question in detail and derived two
equations for the maximal stable orbital radii, one for prograde
motion of the moon and the other one for retrograde motion. Both
depend on the eccentricities, ,
for the planet's orbit
and
for the moon's. For a prograde satellite
Domingos et al. (2006) give:
and for retrograde ones:
Table 1: Properties of the 87 transiting exoplanets.
Barnes & O'Brien (2002) also studied the possible lifetime of a moon due to
orbital decay as a result of tidal dissipation of angular momentum.
Based on this result Domingos et al. (2006) also derived an equation for the
maximum mass a moon can have for a given distance to the planet:







The largest uncertainty in Eq. (5) lies in
.
While a
is commonly used,
Cassidy et al. (2009) suggested values as high as 1013 for
exoplanets. A recent study (Lainey et al. 2009) derived
for Jupiter through astrometric observations of the
planet and its moon Io. In this context it is
interesting to note (Barnes & O'Brien 2002) that the actual detection of exomoons
will give some important constrains on
,
as
Eq. (5) can be written the following way:
Here only a minimal value for

3 Results
A list of currently known transiting exoplanets is shown in
Table 1. In addition to the observed parameters of
these planets, the table gives the Roche-radii, maximal pro- and
retrograde Hill-radii and the maximal pro- and retrograde moon masses
(Eqs. (1), (3)-(5)) for these systems. We used
of 105 and
of 3 g cm-3 for the calculations.
In Fig. 1 the maximal stable prograde orbital radii,
,
for moons are shown for the known transiting
exoplanets from Table 1. Plotted as a shaded region
are the Roche limits for moons with densities between 1 and 6 g
cm-3. For the majority of the known exoplanets stable moons on
prograde orbits are possible. Depending on the density of the moon the
percentage is between 63% (
g cm-3), 85%
(
g cm-3) and 93% (
g cm-3).
![]() |
Figure 1:
Open circles: largest stable prograde orbital radii for
moons of the known transiting exoplanets as shown in
Table 1. The minimal stable orbits for any
substantial moon is given by the Roche-radii for moons with
|
Open with DEXTER |
![]() |
Figure 2:
Solid lines: Maximal stable prograde orbital radii vs.
planet mass for different semi-major axis of the planets for a 1.0 |
Open with DEXTER |
It should be noted here, that the majority of the Hill-radii derived through Eq. (3) agree within better than 10% with the ones derived by Donnison (2010) for the 43 exoplanets of their sample which coincide with our sample. Though, Donnison (2010) does not investigate the possible masses of the exomoons and does not consider the Roche radii as an inner limits of the orbits of the moons.
The limiting
,
calculated from
Eq. (3) are shown as solid lines in Fig. 2 for
exoplanets with planetary masses between 0.01 and 40
around a 1.0
star for ten different orbital separations, a, from 0.01 to 0.1 AU. The dashed-shaded
region marks the Roche-radii of the planet in respect to moons with
densities between 1 and 6 g cm-3. The eccentricity for both the
planet and the moon is set to zero as non-zero eccentricities would
only reduce the Hill-radii. Moons around planets on orbits of
0.02 AU and less are excluded, while only high-density
(
g cm-3) moons can survive for planets on
the 0.03 AU orbit. Also plotted in the Fig. 2 are the
exoplanets from Table 1 for which the host stars are
within 0.1
of 1.0
.
11 out of 27 of these
exoplanets have
within their Roche-radii,
depending on the density of the moon. Therefore, a detection of a moon
around one of these exoplanets would give strong constrains on the
density of the moon.
![]() |
Figure 3:
Open circles: Maximal possible moon mass for prograde
moons of the known transiting exoplanets from
Table 1. Shown as horizontal dotted lines are the
mass of the Earth, of Ganymede and Titan, the largest moons in the
solar system, and of the Earth's moon. For the error bars only the
minimal and maximal ages of the stars are considered. All moons
are assumed to reside on circular orbits (
|
Open with DEXTER |
The maximal possible masses for moons on prograde orbits around the
known transiting exoplanets (Eq. (5)) are shown in
Fig. 3. As is visible only very few exoplanets (7 of 87,
8%) have the potential for moons as massive as the Earth's moon or
larger, independent of the density of the moons. But as
Eq. (5) scales linearly with
of the
planet, larger moons would be possible for exoplanets with very
different internal structures than our solar system Gas Giants.
Also shown as dashed lines in Fig. 3 are maximal moon
masses for theoretical mass-radius relations from Fortney et al. (2007) for
different ages of the exoplanets, different orbital separations and
different solid core fractions of the exoplanets. The top-most dashed
lines corresponds to 300 Myr old exoplanets with 25
solid
cores, orbiting at 0.1 AU around a 1
star. The middle dashed
line shows explanets with 50
core mass, which are 1 Gyr old
and at a distance of 0.045 AU to the host star. And finally the lowest
dashed line are 4.5 Gyr old exoplanets with a = 0.02 AU and without
a solid core. In all three cases a host star mass of 1
is
assumed in order to calculate the Hill radii (Eq. (2))
needed for Eq. (5).
Relatively small changes of the exoplanetary radii due to contraction with time translate into a large changes of the maximal moon mass as Eq. (5) depends to the one over 5th power on the exoplanet radius.
The dependence of the fraction of exoplanets with possible major moons
on the tidal dissipation factor ()
is quantified in
Fig. 4. The fraction rises quite steeply
for
values from 104 to 109 and then saturates at
the fraction of exoplanets which can have moons at all. This fraction
is set by the density of the moon through the Roche limit of the orbit.
![]() |
Figure 4:
Dependence of the fraction of exoplanets from
Table 1 with possible major moons
(
|
Open with DEXTER |
4 Discussion and conclusions
With the use of the results of Domingos et al. (2006) on stable orbits around gas giants the maximal and minimal orbital radii for hypothetical exomoons around the known transiting exoplanets are calculated.
Due to their much larger Hill-radii (for zero eccentricity of the planet and the moon) retrograde moons have larger maximal possible orbital radii and larger maximal masses than prograde moons.
Only WASP-24b (Street et al. 2010), OGLE2-TR-L9 (Snellen et al. 2009; Lendl et al. 2010), CoRoT-3b
(Deleuil et al. 2008) and CoRoT-9b (Deeg et al. 2010) can have a large
earth-sized (0.39, 0.51, 1.7 and 27 ,
respectively)
prograde moons, for a
of 105. In the case of
WASP-24b and OGLE2-TR-L9 this is due to young minimum age of the
stars, for CoRoT-3b the large mass of the planet (brown dwarf) of about 22
enables massive moons, and in the case of CoRoT-9b
the rather large distance of the planet to its parental star allows
for large Hill-radii and therefore large moons. Therefore, these four
exoplanets might be considered the best current candidates to search for
exomoons.
Additionally, SWEEPS-04 (Sahu et al. 2006), CoRoT-6b (Fridlund et al. 2010) and
CoRoT-13b (Cabrera et al. 2010) have
the potential for moons of the size of the Earth's moon
(
1.2
). When
considering also retrograde moons several exoplanets could have
Earth-sized or even larger moons. But the formation of large
retrograde moons seems to be unlikely at least from the point of view
of the Solar System moons. Therefore, 92% of the here studied
exoplanets probably can have only very small prograde moons.
For WASP-19b (Hebb et al. 2010), CoRoT-7b (Queloz et al. 2009), WASP-18b
(Southworth et al. 2009; Hellier et al. 2009), WASP-12b (Hebb et al. 2009), OGLE-TR-56b (Udalski et al. 2002; Southworth 2010),
WASP-33b (Collier Cameron et al. 2010), TrES-3 (O'Donovan et al. 2007; Southworth 2010), WASP-4b (Wilson et al. 2008; Southworth 2010),
OGLE-TR-113b (Southworth 2010; Bouchy et al. 2004), CoRoT-1b (Pont et al. 2010; Barge et al. 2008),
CoRoT-14b (Tingley et al. 2010) and GJ 1214b (Charbonneau et al. 2009) prograde moons larger
than a few kilometers radius are excluded. This translates into 15%
of the total sample. Even when considering moons of a high density of
6 g cm-3 and an extreme
of 1013, WASP-19b,
CoRoT-7b, WASP-18b and WASP-12b are excluded to have large moons.
In the case of HD 80606b (Hidas et al. 2010; Hebrard et al. 2010; Naef et al. 2001) both retro- and
prograde moons are excluded due to the large eccentricity of the
planets orbit. For this planet, only for a moon with a density larger
than 31 g cm-3 would be the Roche-radius smaller than the
prograde Hill-radius.
Therefore it is reasonable to conclude that for the vast majority
of transiting exoplanets the existence of exomoons as large as the
Earth moon or larger is rather unlikely, unless the tidal dissipation
factor
is considerably larger than 105 for these
planets. The actual detection of exomoons would give considerable
insight into the internal structure of the host planet and possibly
the moon itself due to the relatively limited parameters space of
possible orbits around the known transiting exoplanets.
As the ``habitable zone'' of M dwarfs is very close to the star, the rotational period of a planet becomes tidally locked to its orbital period (Peale 1977b) or the planet could be in a spin-orbit resonance, like Mercury in the Solar System. Several studies (Joshi et al. 1997; Heath et al. 1999; Merlis & Schneider 2010) argue that despite tidal-locking such planets might still bear life, though the odds for Earth-like life would seem rather low. Exomoons around tidally-locked gas giants may circumvent the problem of tidal-locking (Kaltenegger 2010). If close-in exoplanets or the exomoons of Hot-Jupiters could be habitable (for Earth-like life) is controversially discussed in the literature (Kiang et al. 2007; Segura et al. 2010; Peale 1977a; Cuntz et al. 2010; Khodachenko et al. 2007; Kaltenegger 2010; Scalo et al. 2007; Jones & Sleep 2010; Heath et al. 1999; Tarter et al. 2007; Williams et al. 1997; Lammer 2007), but of great interest as M dwarfs are the most common stars in the Galaxy.
The lowest-mass star in the current sample of transiting
exoplanets is the M4.5 dwarf GJ 1214, with a mass of
0.16
.
A hypothetical Jupiter-sized gas
giant in the habitable zone of this star (
0.057 AU)
could host a prograde moon no larger than the Earth moon, unless the
of the planet is significantly larger than 105
and any such moon would be very close to the planet (
8
).
It should also be noted here that 95% of the exoplanets included here
have maximal possible prograde orbital radii less than 4
km
(
5.7
), independent of the density of
the moon and the
of the planet. In our Solar System
only two moons with masses similar to that of Earth's moon are so
close to their planets: Jupiter's moon Io
(
,
6
)
and the Earth moon itself
(
). The formation
of very massive moons within the Hill-sphere of close-in exoplanets
might therefore be considered very difficult (Namouni 2010) - at least
on the basis of our current knowledge of the Solar System. Even
if the formation of close-in massive exomoons is possible, the
contraction of its host planet with time (Fortney et al. 2007) will lead to
the orbital decay and eventual destruction of less and less massive
exomoons over time due to the strong dependence of the maximal
possible moon mass (Eq. (5)) on the radius of the planet.
We like to thank the referee Jason Barnes for helpful suggestions. C.W. is happy to thank Christine Liebig, Moira Jardine, and Andrew Collier Cameron for helpful discussions. The authors also gratefully acknowledge the use of the Extrasolar Planets Encyclopedia (http://exoplanet.eu/).
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Footnotes
- ... 460 exoplanets
- For an up-to-date list see http://exoplanet.eu/
- ... AU)
- Since from
(in solar units) and
, follows
.
All Tables
Table 1: Properties of the 87 transiting exoplanets.
All Figures
![]() |
Figure 1:
Open circles: largest stable prograde orbital radii for
moons of the known transiting exoplanets as shown in
Table 1. The minimal stable orbits for any
substantial moon is given by the Roche-radii for moons with
|
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Solid lines: Maximal stable prograde orbital radii vs.
planet mass for different semi-major axis of the planets for a 1.0 |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Open circles: Maximal possible moon mass for prograde
moons of the known transiting exoplanets from
Table 1. Shown as horizontal dotted lines are the
mass of the Earth, of Ganymede and Titan, the largest moons in the
solar system, and of the Earth's moon. For the error bars only the
minimal and maximal ages of the stars are considered. All moons
are assumed to reside on circular orbits (
|
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Dependence of the fraction of exoplanets from
Table 1 with possible major moons
(
|
Open with DEXTER | |
In the text |
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