Age Aspects of Habitability

Age Aspects of Habitability

M. Safonova, J. Murthy Indian Institute of Astrophysics, Bangalore, India rita@iiap.res.in, murthy@iiap.res.in Yu. A. Shchekinov Department of Space Physics, SFU, Rostov on Don, Russia yus@sfedu.ru
Abstract

A ‘habitable zone’ of a star is defined as a range of orbits within which a rocky planet can support liquid water on its surface. The most intriguing question driving the search for habitable planets is whether they host life. But is the age of the planet important for its habitability? If we define habitability as the ability of a planet to beget life, then probably it is not. After all, life on Earth has developed within only  800 Myr after its formation — the carbon isotope change detected in the oldest rocks indicates the existence of already active life at least 3.8 Gyr ago. If, however, we define habitability as our ability to detect life on the surface of exoplanets, then age becomes a crucial parameter. Only after life had evolved sufficiently complex to change its environment on a planetary scale, can we detect it remotely through its imprint on the atmosphere — the so-called biosignatures, out of which the photosynthetic oxygen is the most prominent indicator of developed (complex) life as we know it. Thus, photosynthesis is a powerful biogenic engine that is known to have changed our planet’s global atmospheric properties. The importance of planetary age for the detectability of life as we know it follows from the fact that this primary process, photosynthesis, is endothermic with an activation energy higher than temperatures in habitable zones, and is sensitive to the particular thermal conditions of the planet. Therefore, the onset of photosynthesis on planets in habitable zones may take much longer time than the planetary age. The knowledge of the age of a planet is necessary for developing a strategy to search for exoplanets carrying complex (developed) life — many confirmed potentially habitable planets are too young (orbiting Population I stars) and may not have had enough time to develop and/or sustain detectable life. In the last decade, many planets orbiting old (9–13 Gyr) metal-poor Population II stars have been discovered. Such planets had had enough time to develop necessary chains of chemical reactions and may carry detectable life if located in a habitable zone. These old planets should be primary targets in search for the extraterrestrial life.

keywords:
Planetary systems, formation, photosynthesis, habitability
journal:

1 Introduction

Habitability may be quantitatively defined as a measure of the ability of a planet to develop and sustain life (Schulze-Makuch et al., 2011); its maximum is set as 1 for a planet where life as we know it has formed, thus it is 1 for the Earth. The requirement for a planet to be called habitable (or potentially habitable)111Both definitions habitable and potentially habitable are used in the literature, meaning essentially the same, but see Sec. 4 for our discussion on the definition. is that the planet is located within the host’s HZ and has terrestrial characteristics: rocky, with a mass range of 0.1–10 Earth masses and a radius range of 2 Earth radii222The latest simulations have shown that after 1.7 Earth radii the planets are of increasingly lower density, indicating that they are less rocky and more like mini-Neptunes, placing the Earth’s twin limit on the radius (for ex. Buchhave et al. 2014), though uncertainties remain, see, e.g. Torres et al. (2015). A habitable zone (HZ) is conservatively defined as a region where a planet can support liquid water on the surface (Huang 1959). The concept of an HZ is, however, a constantly evolving one, and many different variations of it have been since suggested (see, for example, an excellent review by Lammer et al. (2009) and references therein, and Heller & Armstrong (2014a) as a more recent one). Biogenic elements (such as C, H, N, O, P and S) have also been considered as necessary complementary factors for habitability (Chyba & Hand, 2005), but their presence is implied by the existence of water as they are produced in the same stars (Heger & Woosley, 2002; Umeda & Nomoto, 2006).

We would like to stress here that throughout the paper, when we talk about detecting life on exoplanets, we still mean life as we know it, the presence of which we are able to establish through predictable changes in planetary atmospheres. Even on Earth, there is a possibility of a different kind of life not based on a usual triad – DNA–protein–lipid, see, for example, discussion on a “shadow” biosphere by Davies et al. (2009). But just as on Earth we are not able to find it (yet) as we do not know ‘where or what to look for’, we may not be able to distinguish these different kinds of life from the natural environments of exoplanets. Hence, when we talk about biosignatures, we mean only biosignatures that our kind of life produces — oxygen, ozone, nitrous oxide, etc (e.g. Seager et al. 2012). A planet may host life as we know it (in other words, be not just habitable but inhabited), but we will still not detect it unless it has evolved sufficiently to change its environment on a planetary scale, for instance, through the production of an oxygen atmosphere by photosynthetic organisms. Photosynthesis is currently the only geologically documented biogenic process (see e.g. Lyons and Reinhard, 2011; Fomina and Biel, 2014 and references therein) that can provide sufficient energy to modify the global planetary (or atmospheric) properties. The large free energy release per electron transfer and stability of the oxygen molecule due to its strong bonding ensures that an oxygen-rich atmosphere provides the largest feasible energy source for compex life (e.g. Catling et al. 2005). Therefore, by analogy with the Earth, we presume the presence of an oxygen atmosphere as necessary for a planet to host a complex life. Such life would have modified the global planetary (or atmospheric) properties to be noticed from space, and from very far away; after all, the closest potentially habitable planet is at about 12 light years ( Ceti) and we cannot go there to verify. Even Mars might still be inhabited by a primitive subsurface biota which are undetectable without a local and detailed examination. It may also be possible for life to evolve in a manner that we have not anticipated, which, even if it changes the environment globally, would not be detectable simply because we are not looking for those particular changes. For example, aphotic life can exist in the subsurface oceans of Europa or Enceladus, but such life would be currently impossible for us to detect ex situ.

Biological methanogenesis was suggested as a rival to the photosynthesis process in changing the global environment and capable of enriching the exo-atmospheres with biogenic methane (Schindler & Kasting 2000; Kharecha et al. 2005). Kharecha et al. (2005) has shown that the rate of biogenic methanogenesis in the atmosphere of an Archaen Earth could have been high enough to enrich the atmosphere with high concentration of biogenic methane. However, planets with reduced mantles might enrich their atmospheres by methane abiotically (e.g., Etiope & Lollar 2013), and thus methane alone cannot guarantee habitability. From this point of view, methanogenic products are a less certain biosignature of Earth-like life than oxygen (Seager et al. 2012). Accounting for a competitive interrelation between metabolic and abiotic origins of methane, a more conservative understanding suggests that only the simultaneous presence of methane along with other biogases is a reliable indication of life (e.g., Selsis et al. 2002; Kaltenegger et al. 2007; Kiang et al. 2007; Kasting et al. 2014). It could also be that the planet never de- velops oxygenic photosynthetic life. In such cases, other biomarkers have been suggested; for example, dimethyl disulphide and CH3Cl may be detected in infrared (IR) in the planetary atmospheres of low-ultraviolet (UV) output stars (Domagal-Goldman et al. 2011).

Carter (1983) has pointed out that the timescale for the evolution of intelligence on the Earth ( Gyr) is comparable to the main sequence lifetime of the Sun ( Gyr). Lin et al. (2014) suggested that intelligent life on expolanets can be detected through the pollution it inflicts on the atmosphere. However, intelligent life, once evolved, is no longer in need of a very precisely defined biosphere — we can already create our own biospheric habitats on planets that are lifeless in our definition of habitability, for ex. Moon or Mars, though we are intelligent for only a 0.0000026% of the time life exists on Earth: 100 years out of 3.6 Gyr. Therefore, intelligent life may not be so easily detectable, especially if they had longer time to evolve. However, to answer the most important question of “are we alone”, we do not necessarily need to find intelligent life. Even detection of a primitive life will have a profound impact on our civilization. Therefore, we need to concentrate on the period in the planet’s history when the emerged life had already influenced the atmosphere of the planet in a way that we can possibly recognize.

We discuss here the importance of the age of the planet in the evaluation of whether that HZ planet contains life and whether that life is detectable. We examine the plausibility of a discovery of a habitable planet with detectable biota among the close (within 600 pc) neighbours of the Sun. We argue that variations in their albedos, orbits, diameters and other crucial parameters make the formation of a significant oxygen atmosphere take longer that the current planetary age and thus, life can be detectable on only half of the confirmed PHPs with a known age.

2 Initial stages of habitability

Necessary conditions for the developing of life are thought to include rocky surface and liquid water; however, the aspects connected with the stages preceding the onset of biological era are usually left out of consideration. Planetary age as a necessary condition for life to emerge was first stressed by Huang (1959) and implicitly mentioned by Crick & Orgel (1973) in their concept of a Directed Panspermia.

In order to understand the importance of planetary age for the evolution of a detectable biosphere we will consider, as an example, the development of cyanobacteria and the related atmospheric oxidation (Irwin et al., 2014). This process involves several endothermic reactions and requires sufficiently high temperatures to be activated. In general, the temperature dependence of the photosynthetic rate is rather complicated and conditionally sensitive, with the effective activation energy being of the order of tens of kJ mol (Hikosaka et al., 2006), much higher than the typical equilibrium temperature on habitable planets. Thus small variations in atmospheric and crust properties can considerably inhibit photosynthesis and increase the growth time of the mass of cyanobacteria. This conclusion may be illustrated through the consideration of the elementary process of carboxylation of RuBP (ribulose-1,5-bisphosphate: CHCP) in the dark Benson-Bassham-Calvin cycle of photosynthesis (Bassham et al., 1950; Farquhar et al., 1980). These photosynthetic reactions, controlled by enzymes, are known to be very sensitive to ambient temperatures with an optimum rate at around 40C, and a practically zero rate outside the temperature range of C (Toole & Toole, 1997). Amongst other fundamental factors RuBP carboxylation is probably the most relevant one, determining the optimal temperature of photosynthesis, and is characterized by the activation energy kJ mol at the growth temperature (Hikosaka et al., 2006). We can roughly characterize the RuBP carboxylation by the Arrhenius law

(1)

where is the rate constant, the prefactor, and is the absolute temperature. The characteristic time of RuBP carboxylation is . Since the RuBP carboxylation is one of the main processes optimizing photosynthetic reactions, can roughly characterize the rate of photosynthesis on a planet.

The range of variation in on a habitable planet due to the uncertainty in the equilibrium temperature is

(2)

with being a characteristic time of photosynthesis at . The equilibrium temperature , in turn, is calculated using planetary parameters inferred from the observations,

(3)

where the uncertainties in the parameters determine the uncertainty in its estimate,

(4)

Here is the luminosity of the central star, and the planet’s albedo and emissivity, the orbital radius, and the Stephan-Boltzmann constant. It is readily seen that the actual time of the onset of photosynthesis for a given habitable planet might differ significantly from the value calculated from largely uncertain parameters that were, in turn, derived from observables. Indeed, uncertainties in estimates of the equilibrium temperature are heavily amplified for habitable planets with for kJ mol and 300 K, such that even relatively low observational errors in deriving the parameters in Eq. (4), say 5% each, might result in % error in the estimates of the overall photosynthesis rate. If one considers oxidation of the Earth atmosphere as a process tracing the developing photosynthesis, the characteristic time for the growth of biota on early Earth can be estimated as the oxidation time, Gyr (Kasting 1993, Wille et al. 2007, Fomina and Biel, 2014). Therefore, a 50% error in may delay the possible onset of biological evolution on a planet by 1 Gyr, i.e. biogenesis might not start earlier than 3 Gyr from the planetary formation. In general, however, the problem of photosynthetic process is much more complex, depending on many factors determined by thermal and non-thermal processes on a planet (Hikosaka et al., 2006; Shizgal & Arkos, 1996), and might be even more sensitive to variations in physical conditions. Even on the early Earth, physical conditions could have been such as to preclude the onset of biogenesis over a long time (Sagan, 1974; Maher & Stevenson, 1988; Solomatov, 2000).

From this point of view, the planetary habitability index (PHI) recently proposed by Schulze-Makuch et al. (2011) in the form

(5)

can be generalized with explicit inclusion of the age of the planet as

(6)

In Eq. (5) defines a stable substrate, the necessary energy supply, the polymeric chemistry and the liquid medium; all the variables here are in general vectors, while the corresponding scalars represent the norms of these vectors. In Eq. (6), the index denotes a chemical chain relevant for further biochemical evolution, and is its characteristic time. It is obvious that the asymptotic behaviour – approaching the maximum habitability – is controlled by the slowest process with the longest .

3 Other Factors Delaying the Onset of Habitability

Sagan (1974) was the first to stress that harmful endogenous and exogeneous processes in the early Earth could postpone emergence of life on it. Such processes could be important even in the very initial primitive episodes of biogenesis and delay the formation of biota for up to billions of years. It is known from the W isotope dating that the late heavy bombardment (LHB) of Earth, Moon and Mars lasted till about 3.8 Ga (Schoenberg et al., 2002; Moynier et al., 2009; Robbins & Hynek, 2012). The Martian primitive atmosphere is believed to have been lost through catastrophic impacts about 4 Ga (e.g., Melosh et al. 1989, Webster et al. 2013). Evidence of a heavy bombardment in other exoplanet systems exists: collision-induced hot dust was detected in several young planetary systems. Spectral signatures of warm water- and carbon-rich dust in the HZ of a young Ga MS star Corvi (Lisse et al., 2012), and of host dust in seven sun-like stars (Wyatt et al. 2007) indicate recent frequent catastrophic collisions between asteroids, planetesimals or even possible planets (Song et al. 2005). Out of these seven stars, five are young systems within their first Gyr of life.

It is also well-known that solar-type stars remain very active in the first billion years of their life, sustaining conditions that are hostile to the survival of the atmosphere and to the planetary habitability. G-type stars, within the first 100 Myr of reaching ZAMS, produce continuous flares of EUV radiation up to 100 times more intense than the present Sun, and have much denser and faster stellar winds with an average wind density of up to 1000 times higher. Low-mass K- and M-type stars remain X-ray and EUV-active longer than solar-type stars, where EUV emission can be up to 3–4 times and 10–100 times, respectively, higher than G-type stars of the same age; and active M-type stars could keep stellar winds in the HZ that are at least 10 times stronger than that of present Sun (France et al. 2013).

In recent simulations by Schaefer et al. (2014) of the development of oceans on super-Earths, it was shown that though larger than the Earth planets keep their oceans for longer (up to 10 Gyr), it takes longer for them to develop the surface ocean due to the delayed start of volcanic outgassing that returns water back to the surface from the mantle. For super-Earths 5 times the Earth’s mass, that would take about a billion years longer. The oceans are believed to have established on Earth 750 Myr after formation, therefore super-Earths would have their surface water established at only 2 Gyr after formation. After all, the Great Oxygenation Event about 2.5 Ga (Anbar et al. 2007) was most likely induced by oceanic cyanobacteria, which allowed life to emerge on land about 480 – 360 Ma (Myr ago) (Kenrick and Crane, 1997).

4 Potentially Habitable Planets

At the time of writing, more than 1900 exoplanets have been confirmed (Extrasolar Planets Encyclopaedia, June 2015) with another 4000 waiting for confirmation (NASA Exoplanet Archive). The majority of detected planets is in the vicinity of the Sun, and their hosts are mostly young Population I (Pop I) stars with ages of hundreds of Myr to a few Gyr. The age distribution of the host stars with measured ages is shown in Figure 1. of the host stars have ages of 4.5 Gyr and less, and more than a third () are younger than 3 Gyr. Simple statistics shows the median age of Gyr.

Figure 1: Age distribution of the stars hosting confirmed planets (total 583 hosts with known ages at time of writing). We highlight the number of stars with ages below 3 Gyr in black, and between 3 and 4.5 Gyr as hatched. The predominance of young host stars is clearly seen, which could be the effect of observational selection (Shchekinov, Safonova & Murthy, 2013). This figure was made using the Extrasolar Planets Encyclopaedia data.

The fact that more than a third of the planetary systems, discovered by ongoing exoplanetary missions, are younger than Gyr is not surprising, because the continuous star formation (SF) in the Galactic disk supplies young stars, and the fraction of hosts younger than 3 Gyr represents that very fraction of Pop I stars that would be born provided the star formation rate is nearly constant during the whole period of the thin disk formation. Most of current exoplanet missions suffer from an observational bias — they mostly detect systems that are younger than the age at which life is presumed to have appeared on the Earth.333The earliest geological/fossilized evidence for the existence of biota on Earth dates to Ga, see Brack et al. (2010) and references therein.

Incidentally, Fig. 1 shows a deficit of stars with ages Gyr. Assuming that Pop I stars, i.e. the thin Galactic disk, have started forming at around 10 Ga (Chen et al., 2003; Carraro et al., 2007), one might expect the presence of such old stars in our vicinity in the proportion corresponding to the SF history in the early Galaxy. The most conservative assumption implies a constant SF rate, in which case one should expect the number of planet-hosting stars with ages Gyr of about 40%. It is, however, believed that the star formation was more active in the early epochs (Bouwens et al., 2008), therefore, the fraction of hosts older than 6 Gyr should be correspondingly higher. The reason for the decline in the number of the hosts in this age range is unclear and might, in particular, indicate that planetary systems lose planets with age.

About 40 potentially habitable planets (PHPs) are currently documented444See, for example, the online Habitable Exoplanets Catalog (HEC), maintained by the Planetary Habitability Laboratory at the University of Puerto Rico, Arecibo, http://phl.upr.edu/projects/habitable-exoplanets-catalog, but not exclusively., though extrapolation of Kepler’s data shows that in our Galaxy alone there could be as many as 40 billion PHPs (Petigura et al. 2013). In Table 1 we show the data for PHPs for which the host ages were available in the literature. The fraction of young planetary systems is nearly consistent with the age distribution of Pop I stars: among the 33 confirmed habitable planets with known ages more than half are Gyr old.

It seems reasonable to update the definitions in footnote 1 on page 2 as

  1. Potentially Habitable planet – a rocky, terrestrial-size planet in a HZ of a star.

  2. Habitable planet – a rocky, terrestrial-size planet in an HZ with detected surface water and some of the biogenic gases in atmosphere.

  3. Inhabited planet – the best case scenario: a rocky, terrestrial-size planet in a HZ with simultaneous detection of species such as water, ozone, oxygen, nitrous oxide or methane in atmosphere, as proposed by e.g. Sagan et al. (1993) or Selsis et al. (2002).

We may expect only a primitive form of biota on the youngest planets ( Gyr) in Table 1, which would not be detectable. Biogenesis could have started, or even progressed to more advanced stages with an oxidized atmosphere, on older planets with ages from 2 to 4 Gyr. In the former case, one can expect that methane from metabolic reactions has already filled the atmosphere, while in the latter case, oxygen molecules at some level can appear in the atmosphere — though atmospheric oxygen on Earth appeared about 2.5 Ga, the Earth itself became visibly habitable only about 750–600 Ma, when the biosphere became active and complex enough to modify the environment to be noticed from space (e.g. Mendéz et al. 2013). The traces of these gases may, in principle, be observed in sub-mm and micron wavelengths, provided the planets are orbiting low-mass stars (0.5–0.8 ). Even if a third of the low-mass stars in the sky host planets (Tutukov & Fedorova, 2012), there may be as many as a thousand planets within a 10 pc vicinity with ages ranging from Myr to a few Gyr.

Star Planet(s) Age Estimate Metallicity Distance Ref. to age
 (Gyr) [Fe/H] (pc)
Kepler 61 Kepler-61 b 326 1
Gliese 667C Gl 667 c ; 2–5; 7.24 1; 2; 3
Kepler 62 Kepler-62 e,f 368 4
Kapteyn’s Kapteyn’s b 10–12 3.91 5
Gliese 163 Gl 163 c ; ; 15 1; 7; 8
HD 40307 HD 40307 g ; 4.5; 6.1 12.8 9; 10
HD 85512 HD 85512 b 11 11
Kepler 22 Kepler-22 b 190 12
Gliese 832 GJ 832 c 9.24 4.95 13
Kepler 186 Kepler-186 f 172 14
Kepler 296 Kepler-296 e,f 4.2 (+3.4, -1.6) 226 14
Kepler 436 Kepler-436 b 3.0 (+7.7, -0.3) 618 14
Kepler 437 Kepler-437 b 2.9 (+7.5, -0.3) 417 14
Kepler 438 Kepler-438 b 4.4 (+0.8, -0.7) 145 14
Kepler 439 Kepler-439 b 7.2 (+3.6, -3.9) 693 14
Kepler 440 Kepler-440 b 1.3 (+0.6, -0.2) 261 14
Kepler 441 Kepler-441 b 1.9 (+0.65, -0.4) 284 14
Kepler 442 Kepler-442 b 2.9 (+8.1, -0.2) 342 14
Kepler 443 Kepler-443 b 3.2 (+7.5, -0.4) 779 14
KOI 4427 KOI 4427 b 3.6 (+2.6, -1.3) 240 14
Kepler 174 Kepler-174 d 360 15
Kepler 309 Kepler-309 c 1.5 581 16
Kepler 421 Kepler-421 b 320 15
Kepler 108 Kepler-108 c 861 15
Kepler 397 Kepler-397 c 1154 15
Kepler 90 Kepler-90 h 835 15
Kepler 87 Kepler-87 c 782 15
Kepler 69 Kepler-69 c 360 15
Kepler 235 Kepler-235 e 1.5 525 16
Kepler 283 Kepler-283 c 2.0 534.4 16
Kepler 298 Kepler-298 d 1.5 474.3 16
EPIC 201367065 EPIC 201367065 d 45 17
tau Ceti tau Ceti e 5.8 3.65 18

The radii of these planets are Earth’s, however, it is still too soon to exclude them from the list, according to Torres et al. 2015, since there are many uncertaintites in the modelling of the transition from rocky to hydrogen/helium planets, and these planets may be rocky.
References to ages: 1. The Extrasolar Planet Encyclopaedia (http://exoplanet.eu); 2. Angala-Escudé et al. 2012; 3. Anglada-Escudé et al. 2013; 4. Borucki et al. 2013; 5. Anglada-Escudé et al. 2014; 6. Mamajek & Hillenbrand 2008; 7. Tuomi & Anglada-Escudé 2013; 8. Open Exoplanet Catalogue (http://www.openexoplanetcatalogue.com); 9. Nordström et al. 2004; 10. Tuomi et al. 2013a; 11. Pepe et al. 2011; 12. Metcalfe 2013; 13. Wittenmyer et al. 2014; 14. Torres et al. 2015; 15. NASA Exoplanet Archive at http://exoplanetarchive.ipac.caltech.edu; 16. Gaidos 2013; 17. Crossfield et al. 2015; 18. Tuomi et al. 2013b.

Table 1: Host ages for confirmed potentially habitable planets.

The age of a planet is of primary importance for developing the future strategy of looking for life on PHPs. Since space programs are extremely expensive and require extensive valuable telescope time, it is crucial to know in advance which planets are more likely to host detectable life. Young planets will not have atmospheres abundant in products of photosynthetic processes, and many planets, though residing in the HZ, may not actually be habitable for life as we know it. For example, the host stars in the Degenerate Objects around Degenerate Objects (DODO) direct imaging search for sub-solar mass objects around white dwarfs (Hogan et al. 2009) are rather young with an average age of only 2.25 Gyr. The target star selection of the Darwin (ESA) mission is restricted to stars within pc (Kaltenegger & Fridlund 2005), and two space missions that are currently under study, the NASA Transiting Exoplanet Survey Satellite (TESS) mission and ESA’s PLAnetary Transits and Oscillations of stars (PLATO) mission, will only survey bright F, G, K stars and M stars within 50 pc (e.g. Lammer et al. 2013), sampling therefore only the thin Galactic disk stars — young Pop I hosts. The main focus of Exoplanet Characterization Observatory (EChO) (Drossart et al., 2013) is the observation of hot Jupiter and hot Neptune planets, limited due to the mission lifetime constraints to bright nearby M stars (Tinetti et al. 2012). Most known habitable planets cannot have an existing complex biosphere although they may develop it in the future, because most currently known PHPs are found around relatively young Pop I stars. We feel reasonable to fix a period of Gyr as the minimum necessary time for the formation of complex life forms at optimal conditions, as evidenced by the Earth’s biosphere. Direct observations of planetary atmospheres in IR and sub-mm wavebands would be a promising method for tracing biogenesis. Planned future IR and sub-mm observatories could provide such observations (see discussion in Sec. 6 below.)

In this context, we undertaken the project of updating the catalog of Nearby Habitable Systems (HabCat) constructed for SETI by Turnbull and Tarter (2003a) for the search for potentially habitable hosts for complex life. A complete characterization of all the stars within a few hundred (or even a few tens of) parsecs, including their masses, ages, and whether they have planetary systems (including terrestrial planets), was not realizable at that time. Our aim was to find out the information on these stars: their ages and whether they have planets and if they could be potentially habitable.

To begin with, we have taken the HabCat II, a “Near 100” subset – a list of the nearest 100 star systems of the original HabCat (Turnbull & Tarter, 2003b), as a basis for our project. These stars were scrutinized for information on their age, nearby planets etc., which were missing in the original catalogue but are important now due to their impact on selecting the targets for future space missions. Out of 100 nearby (within 10 pc) objects in the HabCat II, we have found the age data for 50 stars. This list is being cross-correlated with the Hypatia Catalog, which is a project to find abundances for 50 elements, specifically bio-essential elements, for the stars in the HabCat (Hinkel et al. 2014). Our goal is to compile a list of the most probable planets that may allow future missions to search our neighbourhood for habitable/inhabited planets more efficiently. The preliminary result of this project is presented in Table A.2 in Appendix B.

5 Old Planetary Systems

5.1 General census

Most of the old planetary systems were discovered serendipitously. Only in 2009 were targeted surveys of metal-poor stars initiated (Setiawan et al. 2010). In spite of that, quite a few old ( Gyr) planetary systems are currently known. Shchekinov, Safonova & Murthy (2013) attempted to compile a list of such system (see their Table 1) on the basis of metallicity, considering stars . They, however, missed many previously known systems with ages determined by several different methods, including metallicity abundances, chromospheric activity, rotation and isochrones. Combining their table with other studies (Saffe et al. 2005; Haywood 2008 and latest updates of online expolanet catalogs) brings the census of planetary systems with ages Gyr to 116 planets (90 host stars; see Appendix A for the table of these systems). It is possible that the number of such hosts is much larger since we have counted only those stars where estimates from different methods were comparable. For example, in the list of NASA Exoplanet Archive candidates to PHPs, out of 62 hosts with estimated ages, 28 are older than 10 Gyr.

The majority of old planets was detected by the radial velocity (RV) method which is biased to detect preferentially massive planets due to a limited sensitivity. Continuously increasing precision of radial-velocity surveys may in future change this picture, and the first example of that is the detection in mid-2014 of the terrestrial planet ( 5 Earth masses) orbiting extremely old (10–12 Gyr) Kapteyn’s star (Anglada-Escudé et al. 2014). The most remarkable thing is that this planet lies in the HZ. The star also has another super-Earth outside the HZ.

5.2 Potential habitability of old planetary systems

The improved precision has also resulted in the rejection of three previously reported old planets HIP 13044 b and HIP 11952 b,c (e.g. Setiawan et al., 2010, 2012) as a genuine signal (Jones & Jenkins 2014). However, it still leaves the number of old planets of at least 117 (92 hosts, see Table 2 in the Appendix) with 11 super-Earths (namely, Kepler-18 b; 55 Cnc e; Kapteyn’s b,c; MOA-2007-BLG-192L b, OGLE-2005-BLG-390L b and five planets of Kepler-444) and all the rest gas giants, which do not fall into the category of habitable planets. However, because giant planets typically harbor multiple moons, the moons may be habitable and may even lie in the domain of a higher habitability, or even “superhabitability” (Heller & Armstrong 2014a). For example, Schulze-Makuch et al. (2011) estimate the PHI for Jupiter to be only 0.4, while it is around 0.65 for Titan. There are 33 potentially habitable exomoons with habitable surfaces listed by HEC (excluding possibility of subsurface life), which have on average ESI higher than the potentially habitable planets. Heller et al. (2014) have shown that the number of moons in the stellar HZ may even outnumber planets in these circumstellar zones, and that massive exomoons are potentially detectable with current technology (Heller 2014). Even though Population II (Pop II) stars are normally two order of magnitude less abundant in metals, they may harbor up to 10 potentially habitable rocky Earth-size subsolar objects each (Shchekinov, Safonova & Murthy, 2013), either as planets or as moons orbiting gaseous giants. Planets can form at metallicities as low as due to the centrifugal accumulation of dust (Shchekinov, Safonova & Murthy, 2013). However, Pop II stars could have formed in the metals-enriched pockets resulting from a non-perfect mixing in young galaxies when the Universe was as young as a few hundreds of Myr (Dedikov & Shchekinov, 2004; Vasiliev et al., 2009). They would be able to form planets in a traditional way, and our Galaxy may have a vast number of rocky planets residing in habitable zones. Such planets had longer time for developing biogenesis. Recently discovered 5 rocky planets orbiting 11.2 Gyr old star Kepler-444 (Campante et al. 2015) seems to confirm the previously suggested (Shchekinov, Safonova & Murthy, 2013) hypothesis.

Direct measurements of metallicities and abundance pattern in the early Universe have recently become possible with the discovery of extremely metal-poor (EMP) stars with metallicities as low as of the solar value — these objects are believed to represent the population next after the Population III stars (Beers & Christlieb, 2005). The relative abundances observed in the EMP stars are shown to stem from the explosions of Population III intermediate-mass SNe with an enhanced explosion energy around erg (Umeda & Nomoto, 2006). These stars are also often found to be overabundant in CNO elements. Interestingly, their relative abundance (Aoki et al., 2006; Ito et al., 2013) is consistent with the abundance pattern of the Earth crust (Taylor & McLennan, 1995; Yanagi, 2011) and the chemical composition of the human body (see, e.g. Nielsen, 1999).

Though Earth is rich in chemistry, living organisms use just a few of the available elements: C, N, O, H, P and S, in biological macromolecules: proteins, lipids and DNA, which can constitute up to 98% of an organisms’ mass (e.g., Alberts et al. 2002). Apart from hydrogen, these ‘biogenic’ elements are all produced by the very first massive pop III stars. Detection of substantial amount of CO and water in the spectrum of quasar SDSS J1148+5251 shows, for example, that at Myr after the Big Bang, all the ingredients for our carbon-based life were already present. The initial episode of metal enrichment is believed to have occurred when the Universe was about 500–700 Ma — the absorption spectra of high-redshift galaxies and quasars show significant amount of metals, in some cases up to 0.3 of the solar metallicity (e.g., Savaglio et al., 2000; Finkelstein et al., 2013). The abundance pattern of heavy elements in this initial enrichment contains a copious amount of elements sufficient for rocky planets to form within the whole range of masses (Bromm, Coppi & Larson, 1999; Abel, Bryan & Norman, 2000; Clark et al., 2011; Stacy et al., 2011).

Therefore, planets formed in the early Universe and observed now as orbiting very old ( Gyr) Pop II stars, may have developed and sustained life over the epochs when our Solar System had only started to form. In this way, the restricted use of six ‘biogenic’ elements may be considered as a fossil record of an ancient life — it is well known that at the molecular level, living organisms are strongly conservative. The general direction of the biological evolution is in the increase of complexity of species rather than (chemical) diversity (Mani 1991). For example, paradoxically, both oxygen and water are destructive to all forms of carbon-based life (e.g. Bengston 1994). The presence of water reduces the chance of constructing nucleic acids and most other macromolecules (Schulze-Makuch & Irwin, 2006). The toxic nature of oxygen necessitated the evolution of a complex respiratory metabolism, which again shows the strong chemical conservatism at the molecular level in that the living organisms developed the protection mechanisms to circumvent these problems rather than use other compounds.

6 Observational Prospects

Recently, a 13.6 Gyr star was detected placing it as the oldest star in the Universe (SMSS J031300.36−670839.3, Keller et al. 2014); the age was estimated by its metallicity [Fe/H]. In spite of that, this star, believed to have formed from the remnants of the first-generation SN, was found to contain carbon, metals like lithium, magnesium, calcium, and even methylidyne (CH). It is quite possible that such stars have planets that are directly observable in micron wavelength range. Such EMP stars are known to have low masses and, as such, the orbiting planets could be seen directly in the IR.

The number of EMP stars is estimated to be around 250,000 within 500 pc in SDSS database (Aoki et al., 2006), so the mean distance between them is about 10 pc. If each EMP star hosts an Earth-size planet, the flux from the planet at a distance in the IR range (m) evaluated at the peak frequency (Wien’s law) , is

(7)

We can rewrite this flux as

(8)

where is the equilibrium temperature of a planet and is its radius. For the Sun/Earth system, the ratio of the fluxes at a distance of 10 pc is

(9)

However, if we consider a super-Earth with , and K, orbiting the star with K and – an M dwarf, we get an improvement of

(10)

It seems challenging to detect such a weak contribution to a total flux from a planet even in the IR. There is, however, a possibility to distinguish the emission from the planet in IR molecular features, such as CH or O, tracing either initiated biogenesis or developed metabolism. Detection of direct IR emission from O on exoplanets going through the initial epoch of biogenesis, or which are already at a stage with developed biota, was discussed in Churchill & Kasting (2000) and Rodler & López-Moralles (2013), respectively. Rich IR to sub-mm spectra of methane (Niederer 2011, Hilico et al. 1987) also allow to optimistically view the future detection of this biosignature. Even at the low temperatures of EMP stars, K, these molecules are unlikely to survive in sufficient amount in their atmospheres. Therefore, if such emission is observed from an EMP star, it should be considered as a direct indication of an orbiting rocky planet that has already entered the habitable epoch with growing (Eq. 6). The most promising way to identify habitable (inhabited) planets seems to look for simultaneous presence of water, O, O, CH and NO in atmospheric spectra (e.g. Selsis et al. 2002, Kiang et al. 2007, Kaltenegger et al. 2007). Though such observations can be used to detect planets with highly developed habitability orbiting old EMP stars, the expected fluxes in the IR are still below current sensitivity limits and might be only possible in the future. For example, the future Millimetron space observatory planned for launching in next decade (estimated launch 2025) will have the detection limit of 0.1 Jy in 1 hour observation in 50-300 m range (Kardashev et al 2014). A molecular CH absorptions at m can be detected by Millimetron in 3 hours observations (Eq. 10) if a nearby (within 10 pc) habitable super-Earth planet transits an M-dwarf.

7 Summary

  • Age of a planet is an essential attribute of habitability along with such other factors as liquid water (or an equivalent solvent), rocky mantle, appropriate temperature, extended atmosphere, and so forth. The knowledge of the age of a “habitable” planet is an important factor in developing a strategy to search for complex (developed) life;

  • Nearly half of the confirmed PHPs are young (with ages less than Gyr) and may not have had enough time for evolution of sufficiently complex life capable of changing its environment on a planetary scale;

  • Planets do exist around old Pop II stars, and recently discovered EMP stars (belonging presumably to an intermediate Pop II.5) are good candidates for direct detection of orbiting planets in the IR and sub-mm wavelengths. Though currently only very few such potentially habitable planets are known, old giant planets may have habitable worlds in the form of orbiting moons;

  • IR and sub-mm observations of terrestrial planets orbiting low-mass old stars is a promising way to trace biogenetic evolution on exoplanets in the solar neighbourhood.

8 Acknowledgments

YS acknowledges the hospitality of RRI and IIA, Bangalore, when this work has been initiated. The authors thank Tarun Deep Saini for his useful comments, IIA Ph. D. student A. G. Sreejith for help with graphics and IIA internship student Anuj Jaiswal for his contribution in the project of updating the HabCat. The authors also thank the referees for their valuable comments which led to considerable improvement in the paper.

This research has made use of the Extrasolar Planets Encyclopaedia at http://www.exoplanet.eu, Exoplanets Data Explorer at http://exoplanets.org, NASA Exoplanet Archive at http://exoplanetarchive.ipac.caltech.edu and NASA Astrophysics Data System Abstract Service.

References

  • (1)
  • Abel, Bryan & Norman (2000) Abel, T., Bryan, G. L., & Norman, M. L., The Formation and Fragmentation of Primordial Molecular Clouds. ApJ, 540, 39 (2000)
  • Alberts et al. (2007) Alberts, B., Johnson, A,. Lewis, J., et al. Molecular Biology of the Cell. 4th edition, New York: Garland Science; 2002.
  • Anbar et al. (2007) Anbar, A. D., Duan, Y., Lyons, T. W., et al. A Whiff of Oxygen Before the Great Oxidation Event? Science, 317, 1903 (2007).
  • Anglada-Escudé et al. (2012) Anglada-Escudé, G., Arriagada, P., Vogt, S. S., et al. A Planetary System around the nearby M Dwarf GJ 667C with At Least One Super-Earth in Its Habitable Zone. Astrophys. J. Lett., 751, L16 (2012).
  • Anglada-Escudé et al. (2013) Anglada-Escudé, G., Tuomi, M., Gerlach, E., et al. A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone. Astron. Astrophys., 556, A126 (2013).
  • Anglada-Escudé et al (2014) Anglada-Escudé, G., Arriagada, P., Tuomi, M., et al. Two planets around Kapteyn’s star: a cold and a temperate super-Earth orbiting the nearest halo red dwarf. Mon. Not. R. Astron. Soc., 443, L89 (2014).
  • Aoki et al. (2006) Aoki, W., Frebel, A., Christlieb, N., et al.  HE 1327-2326, an Unevolved Star with [Fe/H]. I. A Comprehensive Abundance Analysis. Astrophys. J., 639, 897 (2006).
  • Bassham et al. (1950) Bassham, J., Benson, A., Calvin, M., The path of carbon in photosynthesis, J. Biol. Chem., 185, 781 (1950).
  • Beers & Christlieb (2005) Beers, T. C. & Christlieb, N.  The Discovery and Analysis of Very Metal-Poor Stars in the Galaxy. Ann. Rev. Astron. Astrophys., 43, 531 (2005).
  • Bengston (1994) Bengston, S. Early life on Earth. Nobel Symposium Proceedings (Columbia University Press, 1994), ISBN-10#0231080883.
  • Benson (1994) Benson, A. A., Bassham, J. A., Calvin, M., Goudate, T. C., Haas, U. A., Stepka, W. The path of carbon in photosynthesis. 5. Paper chromatography and radioautography of the products. J. Amer. Chem. Soc., 12, 1710 (1950).
  • Brack et al. (2010) Brack, A., Horneck, G., Cockell, C. S., et al. Origin and Evolution of Life on Terrestrial Planets. Astrobiology, 10, 69-76 (2010).
  • Borucki et al. (2013) Borucki, W.J., Agol, E., Fressin, F., Kaltenegger, L., et al. Kepler-62: a five-planet system with planets of 1.4 and 1.6 Earth radii in the habitable zone. Science, 340:587-590 (2013).
  • Bouwens et al. (2008) Bouwens, R. J., Illingworth, G. D., Franx, M., Ford, H.  UV Luminosity Functions at z 4, 5, and 6 from the Hubble Ultra Deep Field and Other Deep Hubble Space Telescope ACS Fields: Evolution and Star Formation History. Astrophys. J., 670, 928 (2007).
  • Bromm, Coppi & Larson (1999) Bromm, V., Coppi, P. S., & Larson, R. B.  Forming the First Stars in the Universe: The Fragmentation of Primordial Gas. Astrophys. J., 527, L5 (1999).
  • Buchhave et al. (2014) Buchhave, L. A., Bizzarro, M., Latham, D. W., et al. Three regimes of extrasolar planet radius inferred from host star metallicities. Nature, 509, 593 (2014)
  • Campante et al. (2015) Campante, T. L., Barclay, T., Swift, J. J., et al. An Ancient Extrasolar System with Five Sub-Earth-size Planets. Astrophys. J., 799, 170 (2015)
  • Carraro et al. (2007) Carraro, G., Geisler, D., Villanova, S., et al. Old open clusters in the outer Galactic disk. Astron. Astrophys., 476:217-227 (2007).
  • Chen et al. (2003) Chen, L., Hou, J. L., & Wang, J. J.  On the Galactic Disk Metallicity Distribution from Open Clusters. I. New Catalogs and Abundance Gradient. Astronom. J., 125, 1397 (2003).
  • Christensen & Pearl (1997) Christensen, P. R., and Pearl, J. C.  Initial data from the Mars Global Surveyor thermal emission spectrometer experiment: Observations of the Earth. Journal of Geophysical Research, 102, 10875 (1997).
  • Churchill & Kasting (2000) Churchill, D., and Kasting, J. F. Nitrous Oxide in the Early Atmosphere: A Marker for Life? in Proc. of the Conference ’Darwin and astronomy - the infrared space interferometer’, Stockholm, Sweden, 17-19 November 1999. (Noordwijk, the Netherlands: European Space Agency, 2000), ESA SP 451, 183 (2000).
  • Chyba & Hand (2005) Chyba, C. F., and Hand, K. P.  ASTROBIOLOGY: The Study of the Living Universe. Ann. Rev. Astron. Astrophys., 43, 31 (2005).
  • Clark et al. (2011) Clark P. C., Glover S. C. O., Smith R. J., et al.  The Formation and Fragmentation of Disks Around Primordial Protostars. Science, 331, 1040 (2011).
  • Crick & Orgel (1973) Crick, F. H. C., and Orgel, L. E. Prebiotic Activation Processes. Icarus, 19, 341 (1973).
  • Crossfield et al. (2015) Crossfield, I. J. M., Petigura, E., Schlieder, J. E., et al. A nearby M star with three transiting super-Earths discovered by K2. Astrophys. J., 804, 10 (2015).
  • Davies et al. (2009) Davies, P. C. W., Benner, Steven A., Cleland, Carol E., et al. Signatures of a Shadow Biosphere. Astrobiology, 9, 241 (2009)
  • Dedikov & Shchekinov (2004) Dedikov, S. Yu. & Shchekinov, Yu. A. Mixing of Metals during Stripping of Galactic Gaseous Halos. Astr. Rept., 48, 9 (2004).
  • Domagal-Goldman et al. (2011) Domagal-Goldman, S. D., Meadows, V. S., Claire, M. W., Kasting, J. F. Using biogenic sulfur gases as remotely detectable biosignatures on anoxic planets. Astrobiology, 11, 419-441 (2011).
  • Drossart et al. (2013) Drossart, P., Hartogh, P., Isaak, K., et al.  The Exoplanet Characterisation Observatory (EChO): an ESA mission to characterize exoplanets. AAS/Division for Planetary Sciences Meeting Abstracts, 45, #211.25 (2013).
  • Etiope & Sherwood Lollar (2013) Etiope, G., & Sherwood Lollar, B. Abiotic Methane on Earth.  Reviews of Geophysics, 51, 276-299 (2013).
  • Farquhar et al. (1980) Farquhar, G. D., von Caemmerer, S., Berry, J. A. A biochemical model of photosynthetic CO 2 assimilation in leaves of C 3 species. Planta, 149, 78 (1980).
  • Finkelstein et al. (2013) Finkelstein, S. L., Papovich, C., Dickinson, M., et al.  A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51. Nature, 502, 524 (2013).
  • France et al. (2013) France, K., Froning, C. S., Linsky, J. L., et al.  The Ultraviolet Radiation Environment around M dwarf Exoplanet Host Stars. Astrophys. J., 763, 149 (2013).
  • Fomina & Biel (2014) Fomina, I., Biel, K. Photosynthetic Carbon Metabolism: Strategy of Adaptation. In Contemporary Problems of Photosynthesis, eds. Allakhverdiev, S. I., Rubin, A. B. and Shuvalov, V. A., Institute of Computer Science, Izhevsk–Moscow, 2, 415–483 (2014) [in Russian].
  • Haywood (2008) Haywood, M. A peculiarity of metal-poor stars with planets? Astron. Astrophys., 482, pp.673-676 (2008).
  • Heger & Woosley (2002) Heger A. & Woosley S. E.  The Nucleosynthetic Signature of Population III. Astrophys. J., 567, 532 (2002).
  • Heller & Armstrong (2014) Heller, R., & Armstrong, J. Superhabitable Worlds. Astrobiology, 14, 50 (2014).
  • Heller (2014) Heller, R. Detecting Extrasolar Moons Akin to Solar System Satellites with an Orbital Sampling Effect. Astrophys. J., 787, 14 (2014).
  • Heller et al. (2014) Heller, R., Williams, D., Kipping, D., et al. Formation, Habitability, and Detection of Extrasolar Moons. Astrobiology, 14, 798-835 (2014).
  • Hikosaka et al. (2006) Hikosaka, K., Ishikawa, K., Borjigidai, A., et al.  Temperature acclimation of photosynthesis: mechanisms involved in the changes in temperature dependence of photosynthetic rate. J. Exp. Botany, 57, 291 (2006).
  • Hilico et al. (1987) Hilico, J. H., Loete, M., Champion, J. P., The millimiter-wave spectrum of Methane. J. Molec. Spectr., 122, 381 (1987).
  • Hinkel et al. (2014) Hinkel, N. R., Timmes, F. X., Young, P. A., Pagano, M. D., & Turnbull, M. C. Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog. Astronom. J., 148, 54 (2014)
  • Hogan et al. (2009) Hogan, E., Burleigh, M. R. & Clarke, F. J.  The DODO survey - II. A Gemini direct imaging search for substellar and planetary mass companions around nearby equatorial and Northern hemisphere white dwarfs. Mon. Not. R. Astron. Soc., 396, 2074 (2009).
  • Huang (1959) Huang, S.-S.  The problem of life in the universe and the mode of star formation. PASP, 71:421-424 (1959).
  • Irwin et al. (2014) Irwin L. N., Méndez A., Fairén A. G., Schulze-Makuch D.  Assessing the Possibility of Biological Complexity on Other Worlds, with an Estimate of the Occurrence of Complex Life in the Milky Way Galaxy. Challenges, 5, 159 (2014).
  • Ito et al. (2013) Ito, H., Aoki, W., Beers, T. C. et al.  Chemical Analysis of the Ninth Magnitude Carbon-enhanced Metal-poor Star BD+44-493. Astrophys. J., 773, 33 (2013).
  • Jones & Jenkins (2014) Jones, M. I., & Jenkins, J. S. No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044. Astron. Astrophys., 562, A129 (2014).
  • Kaltenegger et al. (2005) Kaltenegger, L. & Fridlund, M. The Darwin mission: Search for extrasolar planets. Advances in Space Research, 36, 1114-1122 (2005).
  • Kaltenegger et al. (2007) Kaltenegger, L., Traub, W. A., & Jucks, K. W. Spectral Evolution of an Earth-like Planet. Astrophys. J., 658, 598 (2007).
  • Kardashev et al. (2014) Kardashev, N. S., Novikov, I. D., Lukash, V. N. et al, Review of Scientific Topics for the Millimetron Space observatory. Physics – Uspekhi, 57, 1199-1228 (2014).
  • Kasting (1993) Kasting J. Earth’s Early Atmosphere. Science, 259, 920 (1993).
  • Kasting et al. (2014) Kasting J. F., Kopparapu, R., Ramirez, R. M. and Harman, C. E. Remote life-detection criteria, habitable zone boundaries, and the frequency of Earth-like planets around M and late K stars. PNAS, 111, 12641-12646 (2014).
  • Kharecha et al. (2014) harecha, P., J. Kasting, and J. Siefert, A coupled atmosphere-ecosystem model of the early Archean Earth. Geobiology, 3, 53-76 (2005).
  • Kiang et al. (2007) Kiang, N. Y., Segura, A., Tinetti, G., et al. Spectral signatures of photosynthesis. II. Coevolution with other stars and the atmosphere on extrasolar worlds, Astrobiology, 7, 252 (2007).
  • Keller et al. (2014) Keller, S. C., Bessell, M. S., Frebel, A., et al.  A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36-670839.3. Nature, 506, 463 (2014).
  • Kopparapu et al. (2014) Kopparapu, R. K., Ramirez, R. M., SchottelKotte, J., et al. Habitable Zones around Main-sequence Stars: Dependence on Planetary Mass, Astrophys. J. Lett., 787, L29 (2014).
  • Lammer et al. (2009) Lammer, H., Bredehöft, J. H., Coustenis, A., et al. What makes a planet habitable? Astron. Astrophys. Rev., 17, 181 (2009)
  • Lammer et al. (2013) Lammer, H., Blanc, M., Benz, W., et al.  The Science of Exoplanets and Their Systems. Astrobiology, 13:793-813 (2013).
  • Lasaga et al (1971) Lasaga, A. C., Holland, H. D., & Dwyer, M. J. Primordial Oil Slick. Science, 174, 53 (1971)
  • Lin et al. (2014) Lin, H. W., Gonzalez Abad, G., & Loeb, A. Detecting Industrial Pollution in the Atmospheres of Earth-like Exoplanets. Astrophys. J. Lett., 792, LL7 (2014)
  • Lisse et al. (2012) Lisse, C. M., Wyatt, M. C., Chen, C. H., et al.  Spitzer Evidence for a Late-heavy Bombardment and the Formation of Ureilites in eta Corvi at Gyr. Astrophys. J., 747, 93L (2012).
  • Maher & Stevenson (1988) Maher K. A. & Stevenson D. J. Impact frustration of the origin of life. Nature, 331, 612 (1988).
  • Mani (1991) Mani, G.S., in Evolutionary Theories of Economic and Technological Change - Present Status and Future Prospects. Eds. Saviotti, P. P. and Metcalfe, J. S. (Harwood Academic Publishers, U.K., 1991).
  • Melosh & Vickery (1989) Melosh, H.J. and Vickery, A.M., Impact erosion of the primordial atmosphere of Mars. Nature338, 487 (1989)
  • Méndez (2013) Méndez, A., González, Z., Jimenez, S. A. Pérez, W., Bracero, K. The Visible Paleo-Earth Project: A look from space to the evolution of a habitable planet. [in preparation] (2013).
  • Metcalfe (2013) Metcalfe,T. S., Asteroseismology – A Tool for Characterizing Exoplanet Host Star, invited talk at NASA Exoplanet Exploration Program Analysis Group (Long Beach, CA, USA), (2013).
  • Moynier et al. (2009) Moynier, F., Koeberl, C., Quitté, G., & Telouk, P.  A tungsten isotope approach to search for meteoritic components in terrestrial impact rocks. Earth and Planet Sci. Lett., 286, 35 (2009).
  • Nieder (2011) Niederer, J. M. G. The Infrared Spectrum of Methane. Dissertation ETH Nr. 19829, Eidgenössische Technische Hochschule Zürich (ETH Zürich), Zürich, DOI:10.3929/ethz-a-007316862, Verlag Dr. Hut, München (2012).
  • Nielsen (1999) Nielsen F. H. Beyond copper, iodine, selenium and zinc: other elements that will be found important in human nutrition by the year 2000. Proc. of 9th Int. Symp. on Trace Elements in Man and Animals (TEMA-9), Banff, Alberta, Canada, May 19-24, 1996. Eds. Peter W. F. Fischer, Mary R. L’Abbé, Kevin A. Cockell, Rosalind S. Gibson (Ottawa: NRC Research Press, 1997).
  • Pepe et al. (2011) Pepe, F., Lovis, C., Ségransan, D. et al. The HARPS search for Earth-like planets in the habitable zone. Astron. Astrophys., 534, A58 (2011).
  • Petigura et al. (2013) Petigura, E. A., Howard, A. W., & Marcy, G. W. Prevalence of Earth-size planets orbiting Sun-like stars. PNAS, 110, 19273 (2013)
  • Robbins & Hynek (2012) Robbins, S. J. & Hynek, B. M.  Impact History of Large Bollides at Mars: Implications for the Late Heavy Bombardment and Isochron Uncertainties. 43rd Lunar and Planetary Science Conference, #1649 (2012).
  • Rodler & López-Moralles (2013) Rodler, F., & Lopez-Morales, M. Feasibility Studies for the Detection of O in an Earth-like Exoplanet. Astrophys. J., 781, 54 (2014).
  • Saffe et al. (2005) Saffe, C., Gómez, M., & Chavero, C. On the ages of exoplanet host stars. Astron. Astrophys., 443, 609-626 (2005).
  • Sagan (1974) Sagan, C. The origin of life in a cosmic context. Orig. Life Evol. Biosph., 5, 497 (1974).
  • Sagan (1993) Sagan, C., Thompson, W. R., Carlson, R., Gurnett, D., Hord, C. A search for life on Earth from the Galileo spacecraft, Nature, 365, 715 (1993).
  • Santos et al. (2010) Santos, N. C., Mayor, M., Benz, W., et al. The HARPS search for southern extra-solar planets. XXI. Three new giant planets orbiting the metal-poor stars HD 5388, HD 181720, and HD 190984. Astron. Astrophys., 512, AA47 (2010).
  • Savaglio et al. (2000) Savaglio, S. GRBs as cosmological probes — cosmic chemical evolution. New Journal of Physics, 8, 195 (2006).
  • Schoenberg et al. (2002) Schoenberg, R., Kamber, B. S., Collerson, K. D., & Moorbath, S. Tungsten isotope evidence from -Gyr metamorphosed sediments for early meteorite bombardment of the Earth. Nature, 418, 403 (2002).
  • Schulze-Makuch & Irwin (2006) Schulze-Makuch, D., & Irwin, L. N. The prospect of alien life in exotic forms on other worlds. Naturwissenschaften, 93:155-172 (2006).
  • Schulze-Makuch et al. (2011) Schulze-Makuch, D., Méndez, A., Fairén, A. D, et al. A Two-Tiered Approach to Assessing the Habitability of Exoplanets. Astrobiology, 11:1041-1052 (2011).
  • Selsis et al. (2002) Selsis, F., Despois, D. & Parisot, J. P. Signature of life on exoplanets: Can Darwin produce false positive detections? Astron. Astrophys., 388, 985 (2002).
  • Seager et al. (2012) Seager, S., Schrenk, M., Bains, W., An astrophysical view of Earth-based metabollic biosignature gases, Astrobiology, 12, 61-82 (2012).
  • Setiawan et al. (2010) Setiawan, J., Klement, R. J., Henning, Th., et al. Giant Planet Around a Metal-Poor Star of Extragalactic Origin. Science, 330, 1642 (2010).
  • Setiawan et al. (2012) Setiawan, J., Roccatagliata, V., Fedele, D., et al. Planetary companions around the metal-poor star HIP 11952. Astron. Astrophys., 540, 141 (2012).
  • Shchekinov, Safonova & Murthy (2013) Shchekinov, Yu., Safonova, M., & Murthy, J. Planets in the Early Universe. Astrophys. Space Sci., 346:31-40 (2013).
  • Schindler & Kasting (2000) Schindler, T. L., & Kasting, J. F. Synthetic Spectra of Simulated Terrestrial Atmospheres Containing Possible Biomarker Gases. Icarus, 145, 262-271 (2000).
  • Shizgal & Arkos (1996) Shizgal, B. D. & Arkos, G. G. Nonthermal escape of the atmospheres of Venus, Earth, and Mars. Rev. Geophys., 34, 483 (1996).
  • Solomatov (2000) Solomatov, V. S. Fluid Dynamics of a Terrestrial Magma Ocean. In Origin of the Earth and Moon, eds. Canup, R. M. and Righter, K. and et al. (Tucson, Univ. Arizona Press, 2000), pp. 323.
  • Song et al. (2005) Song, I., Zuckerman, B., Weinberger, A. J., & Becklin, E. E. Extreme collisions between planetesimals as the origin of warm dust around a Sun-like star. Nature, 436, 363 (2005).
  • Stacy et al. (2011) Stacy, A., Bromm, V., & Loeb, A. Rotation speed of the first stars. Mon. Not. R. Astron. Soc., 413, 543 (2011).
  • Swain et al. (2010) Swain, M. R. Finesse – A New Mission Concept For Exoplanet Spectroscopy. Bulletin of the American Astronomical Society, 42, 1064 (2010).
  • Taylor & McLennan (1995) Taylor, S. R., & McLennan, S. M., Review of Geophysics, 33, 241 (1995).
  • Toole & Toole (1997) Toole, G., & Toole, S. Advance Human and Social Biology (Stanley Thornes Ltd., 1997).
  • Torres et al. (2015) Torres, G., Kipping, D. M., Fressin, F. et al. Validation of Twelve Small Kepler Transiting Planets in the Habitable Zone. arXiv:1501.01101 ApJ, accepted (2015)
  • Tuomi et al. (2013a) Tuomi, M., Anglada-Escudé, G., Gerlach, E., et al. Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307. Astron. Astrophys., 549, A48 (2013).
  • Tuomi et al. (2013b) Tuomi, M., Jones, H., Jenjkins, J. et al.  Signals embedded in the radial velocity noise. Periodic variations in the tau Ceti velocities. A&A, 551, A79 (2013).
  • Tuomi & Anglada-Escudé (2013) Tuomi, M., & Anglada-Escudé, G. Up to four planets around the M dwarf GJ 163. Sensitivity of Bayesian planet detection criteria to prior choice. Astron. Astrophys., 556, A111 (2013).
  • Turnbull & Tarter (2003a) Turnbull, M. C., & Tarter, J. C. Target Selection for SETI. I. A Catalog of Nearby Habitable Stellar Systems. ApJS, 145, 181 (2003)
  • Turnbull & Tarter (2003b) Turnbull, M. & Tarter, J. Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars. ApJS, 149, 423 (2003)
  • Tutukov & Fedorova (2012) Tutukov, A. V., & Fedorova, A. V. Formation of planets during the evolution of single and binary stars. Astr. Rept., 56, 305 (2012).
  • Umeda & Nomoto (2006) Umeda H., & Nomoto K.  Variations in the Abundance Pattern of Extremely Metal-Poor Stars and Nucleosynthesis in Population III Supernovae. Astrophys. J., 619, 427 (2005)
  • Vasiliev et al. (2009) Vasiliev, E. O., Dedikov, S. & Shchekinov, Yu. A. Chemical inhomogeneity of the post-reionization universe.Astrophysical Bulletin, 64, 317 (2009)
  • Wille et al. (2007) Wille, M., Kramers, J. D., Nägler, T. F., et al. Evidence for a gradual rise of oxygen between 2.6 and 2.5 Ga from Mo isotopes and Re-PGE signatures in shales. Geochimica et Cosmochimica Acta, 71, 2417-2435 (2007).
  • Wittenmyer et al. (2014) Wittenmyer, R. A., Tuomi, M., Butler, R. P., et al. GJ 832c: A super-earth in the habitable zone. Astrophys. J., 791, 114 (2014).
  • Wyatt et al. (2007) Wyatt, M. C., Smith, R., Greaves, J. S., et al. Transience of Hot Dust around Sun-like Stars. Astrophys. J., 658, 569 (2007).
  • Webster et al. (2013) Webster, C. R., Mahaffy, P. R., Flesch, G. J., et al., Isotope Ratios of H, C, and O in CO2 and H2O of the Martian Atmosphere, Science, 341, 260 (2013)
  • Yanagi (2011) Yanagi, T., Arc Volcano in Japan, Lecture Notes in Earth Sciences, Springer-Verlag Berlin Heidelberg (2011).

Appendix A. The list of stars with estimated ages Gyr.

Star name Age Planets Refs., notes
16CygB=HD217014 9-10 2.3J Saffe et al.’05, isoch, Li
GJ86=HR637 12.5 4J -”-, Fe/H
rho Crb=HD143761 11.9-12.1 1J -”-,isoch, Fe/H
HD4208 12.4 0.8J -”-, Fe/H
HD16141=79Ceti 11.2 S=0.2J -”-, isoch
HD41004A 9.5 J -”-, Fe/H
HD45350 12.6 J -”-, isoch
HD65216 10.2 J -”-, Fe/H
HD73526 10.3 bJ;cJ -”-, isoch
HD76700 11.5 hot J -”-, isoch
HD89307 12.2 J -”-, Fe/H
HD108874 10.7-14.1 b,cJ -”-, isoch
HD114386 9.2 1.2J -”-, Fe/H
HD114729 11.9-12.5 1J -”-, isoch
HD134987 11.1 b=0.8J;c=1.5J -”-, isoch
HD142022 9.4-17.2 J -”-, isoch
HD154857 13.1 2 giants -”-, Fe/H
HD162020 9.5 14.4J -”-, Fe/H
HD168443 10.6 bJ;cJ -”-, isoch
HD168746 9.2-16 gas giant -”-,isoch, Fe/H
HD190228 12.5 giant -”-, Fe/H
HD195019 10.6 3.7J -”-, isoch
HD208487 10.8 1J -”-, Fe/H
HD216437 8.7 2J -”-, isoch
HD217107 9.5-9.9 1J
HD181720=HIP95262 9.4-12.1 gas giant Santos et al. 2010 HAPRS
HD4308=HIP3497 11.5 N=14E Haywood 2008
HD6434=HIP5054 10.4 J -”-
HD37124=HIP26381 14.7 b,c,dJ -”-
HD47536=HIP31688 b=5J,c=7J -”-, Silva et al. 2006
HD111232=HIP62534 12.0 J -”-
HD114762=HIP64426 12.4 J -”-
Kapteyn’s 10-12 b,c=sE+sE -”-
PSR-B1620-26 (M4) 2.5J SSM
BD20-2457 12.7 b=12.47J,c=21.42J SSM
HD155358 11.9 b=0.85J,c=0.82J SSM
HAT-P-26 9 8J exoplanets.eu
HD102365 9 N=16E -”-
HD96063 9 0.9J -”-
HD103197 9.1 gas giant, 31E -”-
HD154672 9.28 5J -”-
KOI-1257a 9.3 1.45J -”-
HD47536 9.33 b=5J,c=7J -”-
HD4203 9.41 b=1.2J,c=2J -”-
42Dra=hd170693 9.49 J
HD11964 9.56 b=0.1J(N),c=0.6J -”-
HD88133 9.56 J -”-
HATS-2 9.7 1.3J -”-
HD87883 9.8 J -”-
Kepler-46 9.9 b=S,c=0.37J -”-
Kepler-18 10 6.9E=sE;17E=N;16E=N -”-
V391Peg 10 J -”-
HAT-P-38 10.1 0.27J=S -”-
55Cnc=HD75732 10.2 0.8J=S,J=S,3.8J,8.63E=sE,J=S
HAT-P-21 10.2 4J -”-
HD109749 10.3 J=S -”-
Kepler-10 10.6 b=3.3J,c=17J -”-
CoRoT-17 10.7 hot 2.4J -”-
CoRoT-24 11 b,c=N,N -”-
WASP-37 11 1.8J -”-
WASP-6 11 0.88J -”-
WASP-11-HAT-P-10 11.2 0.8J -”-
WASP-19 11.5 J -”-
WASP-97 11.9 hot 1.3J -”-
HD152581 12 1.5J -”-
HD190360=Gl777a 12.11 0.06J=N,J -”-
HD99109 12.2 0.5J -”-
HAT-P-18 12.4 0.1J=S -”-
HAT-P-22 12.4 2J -”-
PSR1719-14 12.5 J -”-
HD164922 13.4 J=S -”-
WASP-29 15 0.25J=S -”-
rho Indus 12.959 2J exoplanet.eu + exoplanets.org
SAO38269=BD=48738 12.217 J -”-
OGLE2005-BLG-071L 11.404 3J -”-
DP Leonis 11.23 6J -”-
HD37605 10.712 b,c=J,J -”-
OGLE2003-BLG-235L 10.471 2J -”-
MOA2007-BLG-192L 10.42 3E=sE -”-
MOA2009-BLG-387L 10.266 J -”-
NN Serpent’s 10.153 b=7J,c=2J -”-
iota Draco=12 Dra 10.015 12J -”-
Gliese 649 9.998 1S -”-
18 Delphini 9.897 10J -”-
OGLE2005-BLG-390L 9.587 5.5E=sE -”-
WASP-5 9.582 1.6J -”-
Gliese 253 9.451 b,c=N,N -”-
HD1690 9.332 6J -”-
WASP-33=HD15082 9.106 J -”-
WASP-23 9.033 -”-
OGLE2005-BLG-169L 9.623 1U -”-
Kepler-108=KOI119.02 8E NASA Exoplanet archive
Kepler-444 b,c,d,e,f – all Venus Campante et al. 2015, astroseismology
Table 2: Stars with measured/estimated masses of Gy. Where possible, the mass of the planet is given, where the following abbreviations are used: J - Jupiter mass, S - Saturnian mass, N - Neptunian mass, E - Earth mass, sE - super-Earth. Along with the reference for the age, the method of determination is given, where possible.

Appendix B. The ‘‘ Near 100 ’’ — a subset from the nearest 100 star systems.

Star Age (Gyr) Planets Planet(s) Notes
GJ 338AB 0.025-0.3 No
GJ 1 No
GJ 406 0.1-0.35 No
GJ 873 0.1-0.9 No
GJ 876A 0.1-5.0 Yes, 4 J,c=0.714J,d=0.0215J,e=0.046J; 2 in HZ
GJ 1111 0.2 No
GJ 244A 0.2-0.3 No
GJ 244B 0.2-0.3 No
GJ 144 0.2-0.8 Yes, 1 J
GJ 566A 0.2 No
GJ 65A No
GJ 65B No
GJ 729 No
GJ 768 No
GJ 881 Yes, 1 J
GJ 674 Yes, 1 E
GJ 176 0.56 Yes, 1 E
GJ 663A No
GJ 280B 1.37 No
GJ 440 1.44 No
GJ 702A 1.9 No
GJ 667C 2-10, 2 Yes, 2 bE,cE; 1 in HZ
GJ 876 pop. I Yes, 4 b=J,c=J,d=E,e=E
GJ 280A 3 No
GJ 849 middle age dwarf Yes, 2 b=J,c=0.77J
GJ 35 4 No
GJ 764 4.7 No
GJ 551 4.85 No
GJ 442A 4.5-5.7 Yes, 1 J
GJ 71 5.8 Yes, 5 b=E,c=E,d=E,e=E,f=E
GJ 411 5.0-10.0 No
GJ 559A 5.0-7.0 No
GJ 559B 5.0-7.0 Yes, 1 1.13E, Outside HZ
GJ 34A No
GJ 1221 5.69 No
GJ 820A No
GJ 820B No
GJ 139 6.1-12.7 Yes, 3 sE bE,c,dE
GJ 506 6.1-6.6 Yes, 3 b=E, c=E,d=E
GJ 380 6.6 No
GJ 780 6.6-6.9 No Best SETI Target acc. To Turnbull&Tarter (2003)
GJ 223.2 No
GJ 785 7.5-8.9 Yes, 2 bE,cE
GJ 783A 7.7 No
GJ 581 Yes, 3 eE,bE,cE; 2 in HZ
GJ 832 9.24 Yes, 2 bJ,cE
GJ 191 10 Yes, 2 E
GJ 699 No
GJ 892 12.46 No

Note: Some of the catalogues used in the study: The Open Exoplanet Catalogue; Extrasolar Planets Encyclopaedia; NASA Exoplanet Archive; Exoplanets Data Explorer.

Table 3: Selection from the “Near 100” of the stars with estimated ages. Information on planetary systems is important in devising future space missions focussing on astrobiology, thus a column is included whether a particular star has a planet or not, with planetary mass(es).
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
232635
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description