Detectability of Earth-like Planets in Circumstellar Habitable Zones of Binary Star Systems with Sun-like Components
Given the considerable percentage of stars that are members of binaries or stellar multiples in the Solar neighborhood, it is expected that many of these binaries host planets, possibly even habitable ones. The discovery of a terrestrial planet in the Centauri system supports this notion. Due to the potentially strong gravitational interaction that an Earth-like planet may experience in such systems, classical approaches to determining habitable zones, especially in close S-Type binary systems, can be rather inaccurate. Recent progress in this field, however, allows to identify regions around the star permitting permanent habitability. While the discovery of Cen Bb has shown that terrestrial planets can be detected in solar-type binary stars using current observational facilities, it remains to be shown whether this is also the case for Earth analogues in habitable zones. We provide analytical expressions for the maximum and RMS values of radial velocity and astrometric signals, as well as transit probabilities of terrestrial planets in such systems, showing that the dynamical interaction of the second star with the planet may indeed facilitate the planetâs detection. As an example, we discuss the detectability of additional Earth-like planets in the averaged, extended, and permanent habitable zones around both stars of the Centauri system.
The past decades have seen a great number of discoveries of planets around stars other than our Sun (Schneider et al., 2011). As some of these planets are of terrestrial nature, hopes to identifying Earth analogues have lead to considerable advances towards the detection of possibly habitable worlds (Borucki, 2011; Ford et al., 2012). Even though quite frequent in the Solar neighborhood (Kiseleva-Eggleton & Eggleton, 2001), not many attempts have yet been made to specifically target binary stars in this endeavor. Nonetheless, more than 60 planets have already been found in and around such systems (Haghighipour, 2010; Doyle et al., 2011; Welsh et al., 2012; Roell et al., 2012; Orosz et al., 2012a, b; Dumusque et al., 2012). Although several P-Type (circumbinary) planets orbiting both stars of a close binary have also been found (Doyle et al., 2011; Welsh et al., 2012; Orosz et al., 2012a, b), most planets are in the so-called S-Type (Rabl & Dvorak, 1988) configuration where the planet orbits only one of the binary’s stars. A prominent example of an S-Type system is Centauri AB which hosts a terrestrial planet around the fainter binary component, Cen B (Dumusque et al., 2012).
The reason for the general reluctance to include binary systems in the search for terrestrial, habitable planets lies in the assumption that the additional interactions with a massive companion will make planets harder to find. That is primarily because the gravitational interaction between the second star and a planet may alter the planet’s orbit significantly and complicate the task of interpreting the planetary signal. One aim of this work is, therefore, to show that changes in the planet’s orbit can actually enhance its detectability (see section 5). Of course, the orbit of a binary as well as its stellar parameters have to be well determined in order to be able to identify signals from additional terrestrial planets. Sensing the need for a better understanding of binary star systems, efforts have been intensified to improve physical as well as orbital data for nearby binaries (e.g. Torres et al., 2010) and to evolve existing data analysis methodologies (Chauvin et al., 2011; Haghighipour, 2010; Pourbaix, 2002; Pourbaix et al., 2002).
Understanding the complex interactions between a stellar binary and a planet is essential if a system’s potential habitability is to be evaluated. For instance, one of the main assumptions of classical habitability, as introduced by Kasting et al. (1993), is that the planet moves around its host star on a circular orbit. This may not be a valid assumption for planets in a binary star system where the gravitational perturbation of the secondary can excite the eccentricity of the planet’s orbit (Marchal, 1990; Georgakarakos, 2002; Eggl et al., 2012). Eggl et al. (2012) found that except for S-Type systems where the secondary star is much more luminous than the planet’s host star, variations in planetary orbit around the planet-hosting star are the main cause for changes in insolation. Even though Eggl et al. (2012) gave an analytic recipe for calculating the boundaries of the HZs in S-Type binaries, it remains to be seen whether an Earth-like planet in the HZ of a system with two Sun-like stars will in fact be detectable.
In order to answer this question, we consider three techniques, namely, radial velocity (RV), astrometry (AM) and transit photometry (TP), and discuss whether the current observational facilities are capable of detecting habitable planets in such systems. We provide analytical formula for estimating the strength of RV and AM signals for habitable, Earth-like planets, and show that the planet-binary interaction can enhance the chances for the detection of these objects.
The rest of this article will be structured as follows. In sections 2 and 3 analytic estimates of the maximum and root mean square (RMS) of the strength of an RV and an AM signal that an Earth-like planet produces in an S-Type binary configuration will be derived. Section 4 will deal with consequences of such a setup for TP. We will then briefly recall the different types of HZs for S-Type binaries established in Eggl et al. (2012), and use their methodology to identify similar habitable regions in the Centauri system (section 5). This system has been chosen because first, it has inspired many studies on the possibility of the formation and detection of habitable planets around its stellar components (Forgan, 2012; Guedes et al., 2008; Thébault et al., 2009) and second, Dumusque et al. (2012) have already discovered an Earth-sized planet in a short-period orbit around its secondary star. Therefore, we will compare our RV estimates to the actual signal of Cen Bb, and study its influence on an additional terrestrial planet presumed in Cen B’s HZ. Finally, in section 6, the projected RV, AM and TP traces that terrestrial planets will leave in the HZ of the Centauri system are analyzed, and the results are discussed within the context of the sensitivity of the current observational facilities.
2 Radial Velocity
To estimate the RV signal that an Earth-like planet produces in an S-Type binary system, we will build upon the formalism presented by Beaugé et al. (2007). We assume that the non-planetary contributions to the host star’s RV signal (such as the RV variation caused by the motion of the binary around its center of gravity) are known and have been subtracted, leaving behind only the residual signal due to the planet. The motion of the planet around its host star then constitutes a perturbed two body problem, where the gravitational influence of the secondary star is still playing a role and is mirrored in the forced variations of the planet’s orbit.
In practice, the extraction of the planetary signal is all but a trivial task. Even after subtraction of the binary’s barycentric and proper motion, the residual will contain contributions from the binary’s orbital uncertainties as well as from non-gravitational sources which could be orders of magnitude larger than the star’s reflex signal, such as the Rossiter-McLaughlin effect in transiting systems, for example (Ohta et al., 2005). The discovery of Cen Bb showed, however, that a substantial reduction of non-planetary RV interference is possible if the respective binary star has been studied in sufficient detail.
The amplitude of the planet induced RV signal of the host star, , is given by
where is equal to
In equation (2), is the planet to star mass-ratio with and being the masses of the planet and host-star, respectively. The planet’s mean motion, , is given by with , and and being the planet’s orbital period and gravitational constant. The quantities and in equations (1) and (2) denote the planet’s semimajor axis, eccentricity, orbital inclination relative to the plane of the sky, true-anomaly, and argument of periastron, respectively.
Our goal in this section is to identify the range of the possible peak amplitudes that a terrestrial planet in an S-Type binary configuration can produce. We note that the gravitational influence of the second star causes the planet’s orbital elements to vary, thus inducing additional time dependent changes in the radial velocity signal (Lee & Peale, 2003). While we know from secular perturbation theory that does not change significantly with time for hierarchical systems such as the one under consideration (Marchal, 1990; Georgakarakos, 2003), becomes a function of time. We assume coplanar orbits of the planet and the binary star which results in the planet’s inclination to the plane of the sky () to remain constant. In contrast, the planetary eccentricity will vary between zero and a maximum , where the latter value can be expressed as a function of the system’s masses and the binary’s orbital parameters (Eggl et al., 2012). This is important, because the reflex RV signal () of a star can be increased significantly by planetary orbital eccentricities (Fig. 1). Using equation (1) we identify the global maximum of at , when . This leads to
Equation (3) presents a fully analytic estimate of the expected maximum RV signal that
a terrestrial planet produces in an S-Type binary configuration
As an example for the influence of a double star on a planetary RV signal, the induced variations in the RV of the planet’s host-star are presented in figure 1. The host-star is a constituent of a Solar-type binary with a semimajor axis of 20 AU and an orbital eccentricity of 0.5. Changes in the amplitude of are due to variations in the planet’s eccentricity.
Since we do not know the state of the planet’s orbital eccentricity at the time of observation, we consider a range for the maximum possible amplitudes of its radial velocity,
Although the range of the amplitude of the host star’s RV signal, as given by equation (5), can be used to identify the ”best case” detectability limits, the maximum values of the RV signal due to the planet will be ”snapshots” that are reached only during brief moments. As a result, their values for assessing the precision needed to trace fingerprints of an Earth-like planet are rather limited. In such cases, expressions for the RMS of the astrometric signal are preferable.
Since RMS values are by convention time-averaged, we substitute by the mean anomaly in all corresponding functions using the equation of the center expansion up to the sixth order in planetary eccentricities (see appendix A) and average over and . The vastly different rates of change of these quantities () make it possible to consider to remain constant during one cycle of , so that independent averaging can be performed. In order to eliminate short term variations in the RV signal, we first average over . Averaging over as well might be desirable if for example the initial state of is unknown, or if observations stretch beyond secular evolution timescales of the planets argument of pericenter. We, therefore, define two different types of RMS evaluations for a square-integrable function ;
as indicated in appendix B. It is noteworthy that the averaging over causes the RMS value of the RV signal to become independent of so that its difference with the peak signal in the circular case () becomes a mere factor of . Thanks to their intricate relation to power-spectra, RMS values can also be valuable for orbit-fitting. The choice of singly or doubly averaged RMS relations for this purpose will depend on how many planetary orbital periods are available in the data set. In the case of Cen Bb, there are order-of-magnitude differences in the rates of change of the mean anomaly () and the argument of pericenter (). It would, therefore, make more sense to assume to be constant and add it as a variable in the fitting process. If stronger perturbations or additional forces act on the planet, the periods can be considerably shorter, so that the fully averaged equations might come in handy.
In order to derive the maximum and RMS values for an astrometric signal, we will use the framework presented in Pourbaix (2002). We again assume that the non-planetary contributions have been subtracted from the combined signal of the host star and planet. The projected motion of the planet on the astrometric plane is then given by
where and are the Cartesian coordinates of the projected orbit, is the planet’s orbital eccentricity, is the eccentric anomaly, and and are the modified Thiele-Innes constants given by
In these equations, is the distance between the observer and the observed system in units of the planetary semimajor axis . We can rewrite equations (10) in terms of the true anomaly as,
In these equations, represents the planet’s radial distance to its host star. Because the motion of the planet itself cannot be traced, we translate these equations into the apparent motion of the host star by the application of Newton’s third law. That is,
Here, and are the projected coordinates of the center of mass of the planet-star system, and denotes the planet-star mass-ratio as defined for equation (2).
Assuming without the loss of generality that the barycenter of the star-planet system coincides with the origin of the associated coordinate system, the distance of the projected stellar orbit to the coordinate center will be equal to
The right-hand side of equation (14) is independent of and has a global maximum at when . This translates into a maximum astrometric amplitude given by
The planetary maximum AM signal will again lie between and . A remarkable feature of and is their independence of the system’s inclination . This is visualized in figure 2. The same figure also shows the time evolution of the AM signal due to an Earth-like planet orbiting Cen B at a distance of 1 AU.
The astrometric RMS values are given by
Details regarding the derivation of equations (17) and (18) can be found in appendix B.
In contrast to the doubly averaged equations for the RMS of an RV signal, equation (18)
shows a dependence on the binary’s eccentricity. In cases where the planetary inclination coincides
with the inclination of the binary itself, analytic expressions
for are available (Georgakarakos, 2003, 2005)
4 Transit Photometry
In transit photometry, signal strength is equivalent to the relative depth of the dint the planet produces in the stellar light-curve during its transit. Assuming that the star-planet configuration allows for occultations, and excluding grazing transits, the fractional depth of the photometric transit () produced by an Earth-like planet is simply given by the proportion of the luminous area of the disk of the star that is covered by the planet as the planet moves between the observer and the star. Ignoring limb darkening, that means, where is the radius of the planet and is the stellar radius. The overall probability to observe a transit is given by (Borucki & Summers, 1984):
In equation (19), is the radial distance of the planet to the star during the transit.
For an eccentric
planetary motion, the planet-star distance during transit can be expressed as
(Ford et al., 2008), where denotes
the argument of pericenter measured from the line of sight
Equations (20) and (21) indicate that the increase in the eccentricity of the planet due to the perturbation of the secondary increases the probability of transit. In deriving these equations, we have ignored the occultation of the planet by the second star. However, depending on the period ratio between the secondary and the planet, such conjunctions are either scarce or short-lived. Consequently, their contribution to the probability of witnessing a planetary transit is negligibly small.
5 Application to the Centauri system
In this section we will show that the previously derived analytic expressions produce results that are in good agreement with the current observations of Cen Bb. We will also present numerical evidence that the presence - or absence - of an additional terrestrial-planet in the HZ of Cen B cannot be derived easily from the orbit evolution of Cen Bb. Consequently, we argue that an independent detection of additional terrestrial companions might be difficult, but more promising. For this purpose, we will determine the HZ of Cen B, as well as the RV, AM and TP signatures of an Earth-like planet orbiting in the HZ of Cen B. Since there is no a priori reason why the brighter component of Centauri could not be hosting a terrestrial planet as well, we perform a similar analysis for Cen A. We will also study the behavior of equations (1-21) for a broad range of binary eccentricities.
5.1 Centauri’s terrestrial planet
The planet discovered around Cen B offers a perfect opportunity to compare the RV amplitude predictions derived in section 2 with actual measurements. The planet’s known orbital parameters are given in Table 1. In Table 2 we present the analytic estimates of section 2 applied to the Centauri ABb system. Assuming the system to be coplanar (), the predicted RV amplitude for circular planetary motion () is very close to the observed RV amplitude. This is not surprising, since the planetary parameters were derived from an RV signal using the same methodology in reverse. While still well within measurement uncertainties, the deviation of the maximum RV amplitude () from the observed value is larger than that of . On the one hand, this might indicate that the planet is currently in an orbital evolution phase where its eccentricity is almost zero. On the other hand, the planet may be too close to its host star for our model to predict correctly. In fact, we show in section 5.3 that the latter explanation is more likely, since the influence of general relativity (GR) cannot be neglected in this case. Estimates based on Newtonian physics exaggerate the actual eccentricity of Cen Bb. Its orbit remains practically circular despite the interaction with the binary star (see section 5.3 for a detailed discussion). This justifies the assumption of a circular planetary orbit made by Dumusque et al. (2012).
Since we are especially interested in additional habitable planets, however, it is worthwhile to ask whether predictions on the orbital evolution of Cen Bb can be used to exclude the presence of other gravitationally active bodies in the system. In other words: Could an Earth-like planet still orbit in the HZ of Cen B or would the accompanying distortions of the orbit of Cen Bb be significant enough to detect them immediately? Before we try to answer these questions, we need to briefly recall some important aspects regarding HZs in binary star systems.
5.2 Classification of HZs
Combining the classical definition of a HZ (Kasting et al., 1993) with the dynamical properties of a planet-hosting double star system, Eggl et al. (2012) have shown that one can distinguish three types of HZ in an S-type binary system:
- The Permanently Habitable Zone (PHZ)
where a planet always stays within the insolation limits (, ) as defined by Kasting et al. (1993) and Underwood et al. (2003). In other words, despite the changes in its orbit, the planet never leaves the classical HZ. The total insolation the planet receives will vary between the inner and outer effective radiation limits as where, for a given stellar spectral type, and are in units of Solar constant (1360 [W/m]).
- The Extended Habitable Zone (EHZ)
where, in contrast to the PHZ, parts of the planetary orbit may lie outside the HZ due to the planet’s high eccentricity, for instance. Yet, the binary-planet configuration is still considered to be habitable when most of the planet’s orbit remains inside the boundaries of the HZ. In this case, and where denotes the time-averaged effective insolation from both stars and is the effective insolation variance.
- The Averaged Habitable Zone (AHZ).
Following the argument of Williams & Pollard (2002) that planetary eccentricities up to may not be prohibitive for habitability as long as the atmosphere can act as a buffer, the AHZ is defined as encompassing all configurations which support the planet’s time-averaged effective insolation to be within the limits of the classical HZ. Therefore, .
Analytic expressions for the maximum insolation, the average insolation , and insolation variance that a planet encounters in a binary system have been derived in Eggl et al. (2012). We refer the reader to that article for more details.
Figures 3 and 4 show the application of the proposed habitability classification scheme to the Centauri system. In these figures, blue denotes PHZs, green shows EHZs, and yellow corresponds to AHZs. The red areas in figures 3 and 4 are uninhabitable, and purple stands for dynamically unstable regions. Table 1 shows the physical properties of the system. We used the formulae by Underwood et al. (2003) to calculate and for the given effective temperatures of Cen A and B. In general, these formulae allow for extending the analytic estimates for HZs, as given by Eggl et al. (2012), to main sequence stars with different spectral types. Runaway greenhouse and maximum greenhouse insolation limits were used to determine the inner and outer boundaries of HZ, respectively.
As shown in figures 3 and 4, the locations of the HZs and the detectability of habitable planets in those regions depend strongly on the eccentricity of the binary (). The actual eccentricity of the Centauri system is denoted by a horizontal line at . The values for the borders of the different HZs using Centauri’s actual eccentricity are listed in Table 3. As shown here, both stars permit dynamical stability for habitable, Earth-like planets. Due to the difference in stellar luminosities, the HZs around Cen A are larger and farther away from the host star compared to Cen B. Since the binary’s mass-ratio is close to 0.45, the gravitational influence of Cen B is more pronounced on the PHZ of Cen A. This is a consequence of the larger injected planetary eccentricities () as can be seen from the top row of figure 5. The relatively larger gravitational influence of Cen B onto the HZ of Cen A is also mirrored in the fact that the region of dynamical instability (purple) reaches towards lower binary eccentricities. The change in the range and configuration of HZs with the change in planetary semimajor axis and eccentricity of the binary is pronounced. A clear shrinking trend for PHZ and EHZ can be observed for high values of the binary’s eccentricity. While as shown by Eggl et al. (2012), the AHZ in general expands slightly when the eccentricity is enhanced, figures 3 and 4 show that in the Centauri system, this HZ depends only weakly on making it the closest approximation to the classical HZ as defined by Kasting et al. (1993). Comparing these results with the existing studies on the HZs for Cen B such as Guedes et al. (2008) and Forgan (2012), one can see that the values of the inner boundaries of the HZs around Cen B as given in figures 3 and 4, coincide well with the previous studies. Forgan (2012) even found a similar shrinking trend with higher planetary eccentricity. Yet, Forgan (2012) did not take the actual coupling between the planet’s eccentricity and the binary’s orbit into account. The limits for the outer boundaries of HZ in our model are different from the ones in Forgan (2012) since different climatic assumptions were made. In this work we used insolation limits for atmospheric collapse assuming a maximum greenhouse atmosphere (Kasting et al., 1993) whereas Forgan (2012) focused on emergence from snowball states.
5.3 Additional terrestrial planets in Centauri’s HZs
While the classification of habitable zones presented in the previous section is globally applicable to binary star systems, the analytic estimates to calculate their extent (Eggl et al., 2012) are only strictly valid for three body systems, e.g. the binary star and a planet. Additional perturbers will influence the shape and size of the HZs. It is thus necessary to investigate which effect the already discovered planet around Cen B would have on an additional terrestrial planet in Cen B’s HZ.
If the mutual perturbations were large, the HZ boundaries given in Table 3 would have to be adapted, but Cen Bb’s orbital evolution could also contain clues on the presence - or absence - of an additional planet. Should the interaction between the inner planet and an additional terrestrial body in the HZ be small, then the HZ boundaries would hold. However, a detection of the habitable planet via its influence on Cen Bb’s orbit would become difficult.
In figure 6, results of numerical investigations on the coupled orbital evolution of an additional terrestrial planet and Cen Bb are presented. The top row of figure 6 shows the eccentricity evolution of Cen Bb altered by an additional Earth-like planet at the inner (red curve) and outer (orange curve) edge of Cen B’s AHZ . The corresponding reference curve (blue) represents Cen Bb’s eccentricity influenced only by the binary Cen AB. The top left panel of figure 3 shows the results in Newtonian three (3BP) and four (4BP) body problems. The top right panel depicts similar analysis with general relativity (GR) included. The difference between the two approaches is quite pronounced, as GR clearly prevents the secular rise in Cen Bb’s eccentricity predicted in the classical setup (Blaes et al., 2002; Fabrycky & Tremaine, 2007). Thus, the orbit of Cen Bb stays circular, even when tidal forces are neglected. The variations in semimajor axis () for Cen Bb are not shown, because they remain below AU for all cases.
A possible method to search for additional companions is to measure variations in Cen Bb’s orbital period. Yet, the small values make this approach difficult, since . Disentangling the effects of GR and perturbations due to other habitable planets on Cen Bb’s period would require precisions several orders of magnitude greater than currently available. The top right panel in figure 6 shows that the perturbations an additional planet at the inner edge of Cen B’s AHZ causes in Cen Bb’s eccentricity (red) are, in principle, distinguishable from the nominal signal (blue). Unfortunately, it is also clear from this graph that neither the required precision nor the observational timescales necessary to identify the presence of an additional Earth-sized companion via observations of Cen Bb’s eccentricity seem obtainable in the near future. For habitable planets at the outer edge of Cen B’s AHZ the chances for indirect detection seem even worse, as their influence on Cen Bb’s orbit is negligible (orange vs. blue curves).
In order to confirm that the interaction between Cen Bb and Earth-like planets in the HZ is small, as well as to further study the influence of the GR on the dynamics of the system, we examined the orbital evolution of a fictitious habitable planet in that region. The results are shown in the bottom row of figure 6. The left panel depicts the eccentricity evolution of additional terrestrial planets positioned at the inner (red) and outer (green) edges of Cen B’s AHZ. The secular variations in the eccentricity (bottom left panel) and semimajor axis (bottom right panel) of the habitable planet were computed numerically, taking the influence of the binary Cen AB, the planet Cen Bb, as well as GR into account. When comparing the analytic estimates of with the evolution of the habitable planet’s eccentricity in the full system, it is evident that neither GR nor Cen Bb alter the results for planets in Cen B’s HZ significantly. Also, the deviation in the habitable planet’s semimajor axis due to GR and Cen Bb () remains below 0.1% and 0.5% for planets at the inner and outer edge of Cen B’s AHZ, respectively.
We conclude that the interaction between additional terrestrial planets in Cen B’s HZ and Cen Bb is indeed small. Thus, our estimates for the HZs of the Centauri system remain valid. The existence of additional terrestrial planets on the other hand cannot be determined easily from observing the orbital evolution of Cen Bb.
The presented results are, strictly speaking, only valid for a coplanar configuration, i.e. the binary and both planets are in the same orbital plane. Mutually inclined configurations can exhibit much more involved dynamics such as Kozai resonant behavior (see e.g. Correia et al. (2011)). A detailed study of such effects lies beyond the scope of this work. Nevertheless, the arguments presented in this section suggest that the search for an additional coplanar planet in the HZ around Cen B will most likely have to be performed without relying on observations of Cen Bb. We will, therefore, investigate whether habitable planets can actually be detected independently in Sun-like binary star configurations using current observational facilities.
5.4 Detectability Through Radial Velocity and Astrometry
We apply our methodology, as derived in sections 2 and 3, to a fictitious terrestrial planet in the HZ of binary systems similar to Centauri AB but with a broadened range of binary eccentricities. In addition to the habitability maps discussed in section 5.2, figures 3 and 4 show the results regarding peak and RMS strength of the RV and astrometric signals. Here, the aim is to illustrate how the different types of HZs presented in section 5.2, as well as the maximum and RMS signal strengths defined in section 2 vary with the binary’s eccentricity () and planetary semimajor axis (). The left column of figure 3 shows maximum (top) and RMS (bottom) values of the signal strengths for the more massive binary component, in this case similar to Cen A. Results for the less massive component akin to Cen B are shown in the right column.
The dashed vertical lines in the top rows of figures 3 and 4 represent the sections of the parameter space with similar and values, respectively. Since and are independent of the planetary (and consequently the binary’s) eccentricity, the different values of these quantities vary linearly with the planet’s semimajor axis. In contrast, and , represented by the solid contour lines, depend on the maximum eccentricity of the planet () and therefore change with the binary’s eccentricity (). Since for circular binary configurations only small eccentricities are induced into the planet’s orbit, and almost coincide. The same holds true for and in this case. Yet, and grow with the binary’s eccentricity. The corresponding contour lines indicate that for high binary eccentricities even small planetary semimajor axes can produce similar AM peak signal strength. Similarly, planets with larger distances to their host stars can still cause similar RV amplitudes if the binary’s eccentricity is sufficiently large. If a fixed detection limit is set, e.g. m/s, planets with semimajor axes up to AU could still be found around stars similar to Cen A, assuming a binary eccentricity of . To produce a similarly high RV amplitude, a circular planet has to orbit its host star at roughly AU (Fig. 3). In other words, high binary eccentricities lead to excited planetary eccentricities which in turn increase the peak signal strengths suggesting that binary-planet interactions can actually improve the chances for detecting terrestrial planets. Naturally, if the planet’s eccentricity happens to be close to zero at the time of observation, this advantage is nullified.
The bottom row of Fig. 3 shows the same setup with RMS signal strengths and , respectively. While is independent of the binary’s eccentricity, it is evident from equation (17) that depends weakly on since for the cases considered and therefore (see Fig. 5, bottom). The slight curvature of the contour lines representing the RMS signal in Fig. 4 indicates this behavior. A summery of RV and AM signal strengths for an Earth-like planet at the boundaries of Centauri’s HZ is presented in Table 3.
We illustrated in this section that the dynamical interactions between a terrestrial planet and the secondary star can produce large peak amplitudes which may enhance the detectability of the planet with the RV and AM methods considerably. The RMS values of the planet’s AM and RV signals, on the other hand, remain almost unaffected by the gravitational influence of the secondary star.
5.5 Transit Photometry
To assess the detectability of a terrestrial planet in the HZ of Centauri AB (and similar
binaries) through transit photometry, we calculated the relative transit depths that an Earth-like
planet would produce during its transit. If such a system hosted a transiting terrestrial planet,
TD values would range around 55 ppm for Cen A, and 115 ppm for Cen B. Such transit
depths are detectable by NASA’s Kepler telescope for instance – stellar and instrumental
sources included – as the spacecraft’s median noise level amounts to 29 ppm
(Gilliland et al., 2011). Therefore, Earth-like planets could in theory be found around
Centauri stars. However, Kepler was not designed to observe stars with apparent magnitudes between
0 and 3 such as those of Centauri.
The TESS mission (Transiting Exoplanets Survey Satellite), for instance, will aim for TP of brighter stars (Ricker et al., 2010).
Nevertheless, the example of Kepler suggests that the
detection of transiting habitable planets in S-type systems would be possible using current technology.
In fact, very much similar to the cases discussed in the previous sections, the eccentricity excitation
that an Earth-like planet experiences in a binary star system may enhance its possibility of detection
via transit photometry (Kane & von Braun, 2008; Kane, Horner & von Braun, 2012; Borkovits et
al., 2003, also see Fig. 7). Assuming Centauri
was a transiting
The increase in transit probability for planets in double star systems is less dramatic when the equations are averaged over all possible configurations of the argument of pericenter as in equation (21). Averaged transit probabilities are represented by the straight lines in figure 7. As , for terrestrial planets’ orbits with , the chance for transit is in general higher for Earth-like planets in binary stars than for terrestrial planets in circular orbits around single stars.
Comparing the quantitative estimates of RV, AM and TP signals, TP seems to be the best choice for finding Earth-like planets in the HZs of a coplanar S-Type binary configuration with Sun-like components. Even for a system as near as Centauri, AM peak signals only measure as. Unfortunately, neither ESO’s VLBI with PRIMA, nor ESA’s GAIA mission will be able to deliver such precision in the near future (Quirrenbach et al., 2011). GAIA’s aim to provide as astrometry will most likely not be achieved until the end of the mission (Hestroffer et al., 2010). Also, from an astrometric point of view, Earth-like planets would be easier to find around Cen A than Cen B. That is because the HZ around star A is more distant from this star. Naturally, the opposite is true for RV detections. Due to the difference in the stellar masses, Cen B offers a better chance of finding a terrestrial planet there using RV techniques. The recent discovery of an Earth-sized planet around this star supports our results. The observed planetary RV signal was reproduced excellently by our analytic estimates for circular planetary orbits.
Our prediction of RV amplitudes for terrestrial planets around Cen B are also in good agreement with those presented by Guedes et al. (2008). The four terrestrial planets used in the RV model by these authors produce almost exactly four times the predicted RMS amplitude given in figure 3. Guedes et al. (2008) claim that Earth-like planets in the Centauri are detectable even for signal-to-noise ratios (SNR) of single observations below 0.1. However, obtaining sufficient data to reconstruct the planetary signal requires a great amount of dedicated observing time (approximately 5 years in their example). Validating this statement, it took Dumusque et al. (2012) about 4 years of acquired data to detect Cen Bb. The data published by Dumusque et al. (2012) also allow a glimpse on the current performance of the HARPS spectrograph revealing a precision around cm/s. Given the fact that the RV signal of a habitable planet around Cen B would be still half an order of magnitude smaller (Fig. 3), considerably more observation time would be required to identify habitable companions. HIRES measurements are currently yielding precisions around m/s. Identifying RV signals of habitable worlds around Cen B therefore seems even more unlikely when using HIRES. The previous examples show that some development of observational capacities is still necessary to achieve the RV resolution required for discovering habitable planets in the Centauri system.
The success of NASA’s Kepler space telescope in identifying countless Earth-sized planetary candidates (e.g., Borucki, 2011) that require follow-up observations might provide the necessary momentum to develop instruments capable of resolving RV signals in the range of cm/s. Focusing on less massive binaries would have the advantage of having greatly enhanced RV signals as the HZs will be situated closer to the planet’s host stars. How far this might simplify the task of finding habitable worlds will be the topic of further investigations.
In regard to transit photometry, both Kepler and CoRoT telescopes have proven that it is possible to find terrestrial planets around Sun-like stars (e.g., Léger et al., 2009; Borucki et al., 2012). The combination of proven technology and the presented argument that the dynamical environment in binary star systems will enhance transit probabilities makes photometry currently the most promising method for finding Earth-like planets in the HZs of S-Type binary star systems.
In this work, we provided an analytic framework to estimate the detectability of a terrestrial planet using radial velocity (RV), astrometry (AM), as well as transit photometry (TP) in coplanar S-Type binary configurations. We have shown that the gravitational interactions between the stars of a binary and a terrestrial planet can improve the chances for the planet’s detection. The induced changes in the planet’s eccentricity enhance not only RV and AM peak amplitudes, but also the probability to witness a planetary transit. Next to the presented ”best case” estimates, we offered RMS/averaged expressions which are deemed to be more suited to determine the long-term influence of the second star on planetary fingerprints in S-Type systems. In contrast to peak amplitudes, the RMS of a planet’s AM signal is only modified slightly by the additional gravitational interaction with the second star. A similar behavior can be seen in planetary transit probabilities. The RMS values of RV signals are altogether independent of the secondary’s gravitational influence, assuming that the system is nearly coplanar.
After defining the Permanent, Extended, and Average Habitable Zones for both stellar components of the Centauri system, we investigated the possible interaction between the newly discovered Cen Bb and additional terrestrial companions in Cen B’s HZ. Our results suggest that Cen Bb is on an orbit with very low eccentricity which would not be influenced significantly by habitable, terrestrial companions. Conversely, Cen Bb’s presence would also not affect Earth-like planets in the habitable zone of Cen B.
We estimated the maximum and RMS values of the RV as well as AM signal for a terrestrial planet in the Centauri habitable zones. The peak and RMS amplitudes of the RV signal ranged between and cm/s. Astrometric signals were estimated to lie between and 5 as. Given the current observational facilities, enormous amounts of observing time would be required to achieve such precisions. If the Centauri was a transiting system, however, a habitable planet could be detectable using current technologies. It seems that the detection of Earth-like planets in circumstellar habitable zones of binaries with Sun-like components via astrometry and radial velocity is still somewhat beyond our grasp, leaving photometry to be the only current option in this respect.
Appendix A Equation of the Center
The equation of the center providing a direct relation between the true anomaly and the mean anomaly is presented up to the order in eccentricity :
Appendix B Averaging of
The integration over is trivial. Using the partial integration technique to integrate over , we obtain
Here we have used the fact that does no longer depend on . From the definition of averaging given by equation (6), we have
A similar procedure has been applied to derive equation (8).
|Cen A||Cen B|
|Cen A||Cen B|
|Cen A||Cen B|
|mass ||1.105 0.007||0.934 0.007|
|distance [pc]||1.339 0.002|
|period () [d]||29187 4|
|minimum mass () ||1.13 0.09|
|Predicted signal [m/s]||Observed signal [m/s]|
|0.517 0.041||0.51 0.04|
|Cen||[AU]||inner AHZ||inner EHZ||inner PHZ||outer PHZ||outer EHZ||outer AHZ|
- affiliation: University of Vienna, IfA, Türkenschanzstr. 17, A-1180 Vienna, Austria
- affiliation: Institute for Astronomy and NASA Astrobiology Institute, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
- affiliation: University of Vienna, IfA, Türkenschanzstr. 17, A-1180 Vienna, Austria
- Larger signals are possible, if the terrestrial planet has a considerable initial eccentricity after its formation and migration phase. Yet, due to the eccentricity dampening in protoplanetary discs this seems unlikely (Paardekooper & Leinhardt, 2010).
- The analytic expressions given in these articles are also averaged over initial phases, i.e. different relative starting positions of the planet and the binary stars.
- Note that this is different from the conventions used for RV and AM measurements.
- (Borucki & Summers, 1984).
- Beaugé, C., Ferraz-Mello, S., & Michtchenko, T. A. 2007, Planetary Masses and Orbital Parameters from Radial Velocity Measurements, ed. R. Dvorak, 1
- Blaes, O., Lee, M. H., & Socrates, A. 2002, ApJ, 578, 775
- Borucki, W. J., & Summers, A. L. 1984, Icarus, 58, 121
- Borucki, W. J., et al. 2012, ApJ, 745, 120
- Borucki, W. J., et al. 2011, ApJ, 736, 19
- Borkovits, T., Érdi, B., Forgács-Dajka, E., & Kovács, T. 2003, A&A, 398, 1091
- Chauvin, G., Beust, H., Lagrange, A.-M., & Eggenberger, A. 2011, A&A, 528, A8
- Correia, A. C. M., Laskar, J., Farago, F., & Boué, G. 2011, Celestial Mechanics and Dynamical Astronomy, 111, 105
- Doyle, L. R., et al. 2011, Science, 333, 1602
- Dumusque, X. et al., 2012, Nature, 491, 207
- Eggl, S., Pilat-Lohinger, E., Georgakarakos, N., Gyergyovits, M., & Funk, B. 2012, ApJ, 752, 74
- Einstein, A., Infeld, L., & Hoffmann, B. 1938, Annals of Mathematics, 39, 65
- Fabrycky, D., & Tremaine, S. 2007, ApJ, 669, 1298
- Ford, E. B., Quinn, S. N., & Veras, D. 2008, ApJ, 678, 1407
- Ford, E. B., et al. 2012, ApJ, 750, 113
- Forgan, D. 2012, MNRAS, 422, 1241
- Georgakarakos, N. 2002, MNRAS, 337, 559
- —. 2003, MNRAS, 345, 340
- —. 2005, MNRAS, 362, 748
- Gilliland, R. L., et al. 2011, ApJS, 197, 6
- Guedes, J. M., Rivera, E. J., Davis, E., Laughlin, G., Quintana, E. V., & Fischer, D. A. 2008, ApJ, 679, 1582
- Haghighipour, N., 2010, Planets in Binary Star Systems, Springer, New York
- Hestroffer, D., Dell’Oro, A., Cellino, A., & Tanga, P. 2010, in: Lecture Notes in Physics, ed. J. Souchay & R. Dvorak, Vol. 790, pp. 251, Springer Verlag, Berlin
- Holman, M. J., & Wiegert, P. A. 1999, AJ, 117, 621
- Kane, S. R., & von Braun, K. 2008, ApJ, 689, 492
- Kane, S. R., Horner, J., & von Braun, K. 2012, ApJ, 757, article id. 105
- Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108
- Kervella, P., Thévenin, F., Ségransan, D., Berthomieu, G., Lopez, B., Morel, P., & Provost, J. 2003, A&A, 404, 1087
- Kiseleva-Eggleton, L., & Eggleton, P. P. 2001, in: Evolution of Binary and Multiple Star Systems, ed. P. Podsiadlowski, S. Rappaport, A. R. King, F. D’Antona, & L. Burderi , Astronomical Society of the Pacific Conference Series, 229, pp. 91
- Lee, M. H., & Peale, S. J. 2003, ApJ, 592, 1201
- Léger, A., et al. 2009, A&A, 506, 287
- Marchal, C. 1990, The three-body problem, Elsevier
- Ohta, Y., Taruya, A., & Suto, Y. 2005, ApJ, 622, 1118
- Orosz, J. A., et al. 2012a, A&A, 758, article id.87
- Orosz, J. A., et al. 2012b, Science, 337, 1511
- Paardekooper, S.-J., & Leinhardt, Z. M. 2010, MNRAS, 403, L64
- Pilat-Lohinger, E., & Dvorak, R. 2002, CeMDA, 82, 143
- Pourbaix, D. 2002, A&A, 385, 686
- Pourbaix, D., et al. 2002, A&A, 386, 280
- Quirrenbach, A., et al. 2011, European Physical Journal Web of Conferences, 16, 7005
- Rabl, G., & Dvorak, R. 1988, A&A, 191, 385
- Ricker, G. R., Latham, D. W., Vanderspek, R. K., et al. 2010, Bulletin of the American Astronomical Society, 42, #450.06
- Roell, T., Neuhäuser, R., Seifahrt, A., & Mugrauer, M. 2012, A&A, 542, A92
- Schneider, J., Dedieu, C., Le Sidaner, P., Savalle, R., & Zolotukhin, I. 2011, A&A, 532, A79
- Thébault, P., Marzari, F., & Scholl, H. 2009, MNRAS, 393, L21
- Torres, G., Andersen, J., & Giménez, A. 2010, A&A Rev., 18, 67
- Underwood, D. R., Jones, B. W., & Sleep, P. N. 2003, Inter. J. Astrobio., 2, 289
- Welsh, W. F., et al. 2012, Nature, 481, 475
- Williams, D. M., & Pollard, D. 2002, Inter. J. Astrobio, 1, 61