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1.
Jianpo Guo Fenghui Zhang Xianfei Zhang Zhanwen Han 《Astrophysics and Space Science》2010,325(1):25-30
Ultraviolet radiation is a double-edged sword to life. If it is too strong, the terrestrial biological systems will be damaged.
And if it is too weak, the synthesis of many biochemical compounds cannot go along. We try to obtain the continuous ultraviolet
habitable zones, and compare the ultraviolet habitable zones with the habitable zones of host stars. Using the boundary ultraviolet
radiation of ultraviolet habitable zone, we calculate the ultraviolet habitable zones of host stars with masses from 0.08
to 4.00 M
⊙. For the host stars with effective temperatures lower than 4,600 K, the ultraviolet habitable zones are closer than the habitable
zones. For the host stars with effective temperatures higher than 7,137 K, the ultraviolet habitable zones are farther than
the habitable zones. For a hot subdwarf as a host star, the distance of the ultraviolet habitable zone is about ten times
more than that of the habitable zone, which is not suitable for the existence of life. 相似文献
2.
A star will become brighter and brighter with stellar evolution, and the distance of its habitable zone will become larger
and larger. Some planets outside the habitable zone of a host star during the main sequence phase may enter the habitable
zone of the host star during other evolutionary phases. A terrestrial planet within the habitable zone of its host star is
generally thought to be suitable for the existence of life. Furthermore, a rocky moon around a giant planet may be also suitable
for life to survive, provided that the planet–moon system is within the habitable zone of its host star. Using Eggleton’s
code and the boundary flux of the habitable zone, we calculate the habitable zone of our Solar system after the main sequence
phase. It is found that Mars’ orbit and Jupiter’s orbit will enter the habitable zone of the Solar system during the subgiant
branch phase and the red giant branch phase, respectively. And the orbit of Saturn will enter the habitable zone of Solar
during the He-burning phase for about 137 million years. Life is unlikely at any time on Saturn, as it is a giant gaseous
planet. However, Titan, the rocky moon of Saturn, may be suitable for biological evolution and become another Earth during
that time. For low-mass stars, there are similar habitable zones during the He-burning phase as our Solar, because there are
similar core masses and luminosities for these stars during that phase. 相似文献
3.
4.
Rory Barnes 《Celestial Mechanics and Dynamical Astronomy》2017,129(4):509-536
Potentially habitable planets can orbit close enough to their host star that the differential gravity across their diameters can produce an elongated shape. Frictional forces inside the planet prevent the bulges from aligning perfectly with the host star and result in torques that alter the planet’s rotational angular momentum. Eventually the tidal torques fix the rotation rate at a specific frequency, a process called tidal locking. Tidally locked planets on circular orbits will rotate synchronously, but those on eccentric orbits will either librate or rotate super-synchronously. Although these features of tidal theory are well known, a systematic survey of the rotational evolution of potentially habitable exoplanets using classic equilibrium tide theories has not been undertaken. I calculate how habitable planets evolve under two commonly used models and find, for example, that one model predicts that the Earth’s rotation rate would have synchronized after 4.5 Gyr if its initial rotation period was 3 days, it had no satellites, and it always maintained the modern Earth’s tidal properties. Lower mass stellar hosts will induce stronger tidal effects on potentially habitable planets, and tidal locking is possible for most planets in the habitable zones of GKM dwarf stars. For fast-rotating planets, both models predict eccentricity growth and that circularization can only occur once the rotational frequency is similar to the orbital frequency. The orbits of potentially habitable planets of very late M dwarfs ( Open image in new window ) are very likely to be circularized within 1 Gyr, and hence, those planets will be synchronous rotators. Proxima b is almost assuredly tidally locked, but its orbit may not have circularized yet, so the planet could be rotating super-synchronously today. The evolution of the isolated and potentially habitable Kepler planet candidates is computed and about half could be tidally locked. Finally, projected TESS planets are simulated over a wide range of assumptions, and the vast majority of potentially habitable cases are found to tidally lock within 1 Gyr. These results suggest that the process of tidal locking is a major factor in the evolution of most of the potentially habitable exoplanets to be discovered in the near future. 相似文献
5.
Rami T.F. Rekola 《Planetary and Space Science》2009,57(4):430-433
Currently we are aware of only one biosphere in the entire Universe, our own. Various ongoing observational programmes are, however, attempting to locate more. These searches for extraterrestrial life are among the most challenging and interesting tasks of modern science. The Universe is immense, and even the distances to the nearest stars are beyond our present capabilities to traverse, so that search strategies must be thought through carefully in terms of how, where and what to search for. Life is undoubtedly more likely in some environments than others, and environmental criteria must be fulfilled for life to arise, survive, evolve and thrive. As search resources are limited we should concentrate our search on habitable zones that are suitable for the kind of life we can most easily recognise, in other words, searches should be guided by our own biosphere. 相似文献
6.
Owen T 《The Planetary report》1987,7(6):16-18
Many space scientists think that the chemical conditions today on planets and moons of the outer solar system are similar to conditions on Earth soon after it formed. If so, we can learn much about the chemistry that led to life on this planet. We can also speculate about exotic habitats that might have given rise to other types of life. And if we are able to discern the chemical reactions now occurring in the outer solar system, we may be able to extrapolate these rules to other solar systems, and so define the habitable zones around other stars where the potential for life is high. 相似文献
7.
To determine where to search for life in our solar system or in other extrasolar systems, the concept of habitability has
been developed, based on the only sample we have of a biological planet—the Earth. Habitability can be defined as the set
of the necessary conditions for an active life to exist, even if it does not exist. In astronomy, a habitable zone (HZ) is
the zone defined around a sun/star, where the temperature conditions allow liquid water to exist on its surface. This habitability
concept can be considered from different scientific perspectives and on different spatial and time scales. Characterizing
habitability at these various scales requires interdisciplinary research. In this article, we have chosen to develop the geophysical,
geological, and biological aspects and to insist on the need to integrate them, with a particular focus on our neighboring
planets, Mars and Venus. Important geodynamic processes may affect the habitability conditions of a planet. The dynamic processes,
e.g., internal dynamo, magnetic field, atmosphere, plate tectonics, mantle convection, volcanism, thermo-tectonic evolution,
meteorite impacts, and erosion, modify the planetary surface, the possibility to have liquid water, the thermal state, the
energy budget, and the availability of nutrients. They thus play a role in the persistence of life on a planet. Earth had
a liquid water ocean and some continental crust in the Hadean between 4.4 and 4.0 Ga (Ga: billions years ago), and may have
been habitable very early on. The origin of life is not understood yet; but the oldest putative traces of life are early Archean
(~3.5 Ga). Studies of early Earth habitats documented in the rock record hosting fossil life traces provide information about
possible habitats suitable for life beyond Earth. The extreme values of environmental conditions in which life thrives today
can also be used to characterize the “envelope” of the existence of life and the range of potential extraterrestrial habitats.
The requirement of nutrients by life for biosynthesis of cellular constituents and for growth, reproduction, transport, and
motility may suggest that a dynamic and rocky planet with hydrothermal activity and formation of relief, liquid water alteration,
erosion, and runoff is required to replenish nutrients and to sustain life (as we know it). The concept of habitability is
very Earth-centric, as we have only one biological planet to study. However, life elsewhere would most probably be based on
organic chemistry and leave traces of its past or recent presence and metabolism by modifying microscopically or macroscopically
the physico-chemical characteristics of its environment. The extent to which these modifications occur will determine our
ability to detect them in astrobiological exploration. Looking at major steps in the evolution of life may help determining
the probability of detecting life (as we know it) beyond Earth and the technology needed to detect its traces, be they morphological,
chemical, isotopic, or spectral. 相似文献
8.
Jianpo Guo Fenghui Zhang Xuefei Chen Zhanwen Han 《Astrophysics and Space Science》2009,323(4):367-373
With more and more exoplanets being detected, it is paid closer attention to whether there are lives outside solar system. We try to obtain habitable zones and the probability distribution of terrestrial planets in habitable zones around host stars. Using Eggleton’s code, we calculate the evolution of stars with masses less than 4.00 M ⊙. We also use the fitting formulae of stellar luminosity and radius, the boundary flux of habitable zones, the distribution of semimajor axis and mass of planets and the initial mass function of stars. We obtain the luminosity and radius of stars with masses from 0.08 to 4.00 M ⊙, and calculate the habitable zones of host stars, affected by stellar effective temperature. We achieve the probability distribution of terrestrial planets in habitable zones around host stars. We also calculate that the number of terrestrial planets in habitable zones of host stars is 45.5 billion, and the number of terrestrial planets in habitable zones around K type stars is the most, in the Milky Way. 相似文献
9.
During the last decade there was a change in paradigm, which led to consider that terrestrial-type planets within liquid-water habitable zones (LW-HZ) around M stars can also be suitable places for the emergence and evolution of life. Since many dMe stars emit large amount of UV radiation during flares, in this work we analyze the UV constrains for living systems on Earth-like planets around dM stars. We apply our model of UV habitable zone (UV-HZ; Buccino, A.P., Lemarchand, G.A., Mauas, P.J.D., 2006. Icarus 183, 491–503) to the three planetary systems around dM stars (HIP 74995, HIP 109388 and HIP 113020) observed by IUE and to two M-flare stars (AD Leo and EV Lac). In particular, HIP 74995 hosts a terrestrial planet in the LW-HZ, which is the exoplanet that most resembles our own Earth. We show, in general, that during the quiescent state there would not be enough UV radiation within the LW-HZ to trigger the biogenic processes and that this energy could be provided by flares of moderate intensity, while strong flares do not necessarily rule-out the possibility of life-bearing planets. 相似文献
10.
Habitable zones around main sequence stars 总被引：1，自引：0，他引：1
A one-dimensional climate model is used to estimate the width of the habitable zone (HZ) around our Sun and around other main sequence stars. Our basic premise is that we are dealing with Earth-like planets with CO2/H2O/N2 atmospheres and that habitability requires the presence of liquid water on the planet's surface. The inner edge of the HZ is determined in our model by loss of water via photolysis and hydrogen escape. The outer edge of the HZ is determined by the formation of CO2 clouds, which cool a planet's surface by increasing its albedo and by lowering the convective lapse rate. Conservative estimates for these distances in our own Solar System are 0.95 and 1.37 AU, respectively; the actual width of the present HZ could be much greater. Between these two limits, climate stability is ensured by a feedback mechanism in which atmospheric CO2 concentrations vary inversely with planetary surface temperature. The width of the HZ is slightly greater for planets that are larger than Earth and for planets which have higher N2 partial pressures. The HZ evolves outward in time because the Sun increases in luminosity as it ages. A conservative estimate for the width of the 4.6-Gyr continuously habitable zone (CHZ) is 0.95 to 1.15 AU. Stars later than F0 have main sequence lifetimes exceeding 2 Gyr and, so, are also potential candidates for harboring habitable planets. The HZ around an F star is larger and occurs farther out than for our Sun; the HZ around K and M stars is smaller and occurs farther in. Nevertheless, the widths of all of these HZs are approximately the same if distance is expressed on a logarithmic scale. A log distance scale is probably the appropriate scale for this problem because the planets in our own Solar System are spaced logarithmically and because the distance at which another star would be expected to form planets should be related to the star's mass. The width of the CHZ around other stars depends on the time that a planet is required to remain habitable and on whether a planet that is initially frozen can be thawed by modest increases in stellar luminosity. For a specified period of habitability, CHZs around K and M stars are wider (in log distance) than for our Sun because these stars evolve more slowly. Planets orbiting late K stars and M stars may not be habitable, however, b ecause they can become trapped in synchronous rotation as a consequence of tidal damping. F stars have narrower (log distance) CHZ's than our Sun because they evolve more rapidly. Our results suggest that mid-to-early K stars should be considered along with G stars as optimal candidates in the search for extraterrestrial life. 相似文献
11.
Exo-zodiacal dust, exozodi for short, is warm (～300 K) or hot (up to ～2000 K) dust found in the inner regions of planetary systems around main sequence stars. In analogy to our own zodiacal dust, it may be located in or near the habitable zone or closer in, down to the dust sublimation distance. The study of the properties, distribution, and evolution of exozodis can inform about the architecture and dynamics of the innermost regions of planetary systems, close to their habitable zones. On the other hand, the presence of large amounts of exo-zodiacal dust may be an obstacle for future space missions aiming to image Earth-like exoplanets. The dust can be the most luminous component of extrasolar planetary systems, but predominantly emits in the near- to mid-infrared where it is outshone by the host star. Interferometry provides a unique method of separating the dusty from the stellar emission. We discuss the prospects of exozodi observations with the next generation VLTI instruments and summarize critical instrument specifications. 相似文献
12.
Thermal evolution models for carbonaceous asteroids that use new data for permeability, pore volume, and water circulation as input parameters provide a window into what are arguably the earliest habitable environments in the Solar System. Plausible models of the Murchison meteorite (CM) parent body show that to first-order, conditions suitable for the stability of liquid water, and thus pre- or post-biotic chemistry, could have persisted within these asteroids for tens of Myr. In particular, our modeling results indicate that a 200-km carbonaceous asteroid with a 40% initial ice content takes almost 60 Myr to cool completely, with habitable temperatures being maintained for ∼24 Myr in the center. Yet, there are a number of indications that even with the requisite liquid water, thermal energy sources to drive chemical gradients, and abundant organic “building blocks” deemed necessary criteria for life, carbonaceous asteroids were intrinsically unfavorable sites for biopoesis. These controls include different degrees of exothermal mineral hydration reactions that boost internal warming but effectively remove liquid water from the system, rapid (1-10 mm yr−1) inward migration of internal habitable volumes in most models, and limitations imposed by low permeabilities and small pore sizes in primitive undifferentiated carbonaceous asteroids. Our results do not preclude the existence of habitable conditions on larger, possibly differentiated objects such as Ceres and the Themis family asteroids due to presumed longer, more intense heating and possible long-lived water reservoirs. 相似文献
13.
Nader Haghighipour Sabrina Kirste 《Celestial Mechanics and Dynamical Astronomy》2011,111(1-2):267-284
We present the results of an extensive study of the detectability of Earth-sized planets and super-Earths in the habitable zones of cool and low-mass stars using transit timing variation method. We have considered a system consisting of a star, a transiting giant planet, and a terrestrial-class perturber, and calculated TTVs for different values of the parameters of the system. To identify ranges of the parameters for which these variations would be detectable by Kepler, we considered the analysis presented by Ford et?al. (Transit timing observations from Kepler: I. Statistical analysis of the first four months. ArXiv:1102.0544, 2011) and assumed that a peak-to-peak variation of 20 s would be within the range of the photometric sensitivity of this telescope. We carried out simulations for resonant and non-resonant orbits, and identified ranges of the semimajor axes and eccentricities of the transiting and perturbing bodies for which an Earth-sized planet or a super-Earth in the habitable zone of a low-mass star would produce such TTVs. Results of our simulations indicate that in general, outer perturbers near first- and second-order resonances show a higher prospect for detection. Inner perturbers are potentially detectable only when near 1:2 and 1:3 mean-motion resonances. For a typical M star with a Jupiter-mass transiting planet, for instance, an Earth-mass perturber in the habitable zone can produce detectable TTVs when the orbit of the transiting planet is between 15 and 80 days. We present the details of our simulations and discuss the implication of the results for the detection of terrestrial planets around different low-mass stars. 相似文献
14.
Dusty water-ice snowpacks on Mars may provide a habitable zone for DNA based photosynthetic life. Previous work has over estimated the depths and thicknesses of such photohabitable zones by not considering the effect of red dust within the snowpack. For the summer solar solstice, at 80°N and a surface albedo of 0.45, there is a calculated photohabitable zone in the snowpack between depths of 5.5 and 7.5 cm. For an albedo of 0.62, there is a calculated photohabitable zone in the snowpack between depths of 8 and 11 cm. A coupled atmosphere-snow radiative-transfer model was set to model the Photosynthetic Active Radiation and DNA dose rates through water-ice snow at the north polar region of Mars. The optical properties of the polar caps were determined by creating a laboratory analogue to the Mars north polar deposits, and directly measuring light penetration and albedo. It is important for future exobiology missions to the polar regions of Mars to consider the implications of these findings, as drilling to depths of ∼11 cm should be sufficient to determine whether life exists within the martian snows, whether it is photosynthetic or otherwise, as at this depth the snow cover will provide a permanent protection from DNA damaging UV radiation. 相似文献
15.
Dave Waltham 《Icarus》2011,215(2):518-521
The Earth may have untypical characteristics which were necessary preconditions for the emergence of life and, ultimately, intelligent observers. This paper presents a rigorous procedure for quantifying such “anthropic selection” effects by comparing Earth’s properties to those of exoplanets. The hypothesis that there is anthropic selection for stellar mass (i.e. planets orbiting stars with masses within a particular range are more favourable for the emergence of observers) is then tested. The results rule out the expected strong selection for low mass stars which would result, all else being equal, if the typical timescale for the emergence of intelligent observers is very long. This indicates that the habitable zone of small stars may be less hospitable for intelligent life than the habitable zone of solar-mass stars. Additional planetary properties can also be analyzed, using the approach introduced here, once relatively complete and unbiased statistics are made available by current and planned exoplanet characterization projects. 相似文献
16.
Climatic models are increasingly being used to answer “cosmic questions” such as the possibility of an ice-covered Earth or a runaway greenhouse effect, or to examine the coevolution of climate and life. Conclusions from these models on such issues, of course, rest on the physical parameterizations of the models. Some of the basic parameterizations are reexamined quantitatively, and it is concluded that presently believed uncertainties in these parameterizations lead to an order-of-magnitude uncertainty in estimates of the sensitivity of the present Earth's climate to external forcings (like a change in solar constant). However, seasonal simulations with present Earth models suggest that estimates of the overall sensitivity of the climate to external forcing may be narrowed (over decadal time scales) to, perhaps, a factor of 2. But the effects of glaciers, continental locations, and atmospheric composition, all of which can change on geological time scales, further enhance the uncertainties in long-term climatic sensitivity estimates from state-of-the-art models. But it is precisely these long-term estimates of climatic sensitivity which support quantitative conclusions on, for example, the possible existence of continuously habitable zones around main-sequence stars. We believe that those who draw cosmic conclusions from climatic models should at least attempt to bracket the final results by repeating their calculations over a plausible range of uncertainty in basic model parameterizations. 相似文献
17.
H. Lammer J. H. Bredehöft A. Coustenis M. L. Khodachenko L. Kaltenegger O. Grasset D. Prieur F. Raulin P. Ehrenfreund M. Yamauchi J.-E. Wahlund J.-M. Grießmeier G. Stangl C. S. Cockell Yu. N. Kulikov J. L. Grenfell H. Rauer 《Astronomy and Astrophysics Review》2009,17(2):181-249
This work reviews factors which are important for the evolution of habitable Earth-like planets such as the effects of the
host star dependent radiation and particle fluxes on the evolution of atmospheres and initial water inventories. We discuss
the geodynamical and geophysical environments which are necessary for planets where plate tectonics remain active over geological
time scales and for planets which evolve to one-plate planets. The discoveries of methane–ethane surface lakes on Saturn’s
large moon Titan, subsurface water oceans or reservoirs inside the moons of Solar System gas giants such as Europa, Ganymede,
Titan and Enceladus and more than 335 exoplanets, indicate that the classical definition of the habitable zone concept neglects
more exotic habitats and may fail to be adequate for stars which are different from our Sun. A classification of four habitat
types is proposed. Class I habitats represent bodies on which stellar and geophysical conditions allow Earth-analog planets
to evolve so that complex multi-cellular life forms may originate. Class II habitats includes bodies on which life may evolve
but due to stellar and geophysical conditions that are different from the class I habitats, the planets rather evolve toward
Venus- or Mars-type worlds where complex life-forms may not develop. Class III habitats are planetary bodies where subsurface
water oceans exist which interact directly with a silicate-rich core, while class IV habitats have liquid water layers between
two ice layers, or liquids above ice. Furthermore, we discuss from the present viewpoint how life may have originated on early
Earth, the possibilities that life may evolve on such Earth-like bodies and how future space missions may discover manifestations
of extraterrestrial life. 相似文献
18.
Charles S. Cockell Matt Balme John C. Bridges Alfonso Davila Susanne P. Schwenzer 《Icarus》2012,217(1):184-193
Investigations of Mars as a potential location for life often make the assumption that where there are habitats, they will contain organisms. However, the observation of the ubiquitous distribution of life in habitable environments on the Earth does not imply the presence of life in martian habitats. Although uninhabited habitats are extremely rare on the Earth, a lack of a productive photosynthetic biosphere on Mars to generate organic carbon and oxygen, thus providing a rapidly available redox couple for energy acquisition by life and/or a lack of connectivity between habitats potentially increases the scope and abundance of uninhabited habitats for much of the geological history of the planet. Uninhabited habitats could have existed on Mars from the Noachian to the present-day in impact hydrothermal systems, megaflood systems, lacustrine environments, transient melted permafrost, gullies and local regions of volcanic activity; and there may be evidence for them in martian meteorites. Uninhabited habitats would provide control habitats to investigate the role of biology in planetary-scale geochemical processes on the Earth and they would provide new constraints on the habitability of Mars. Future robotic craft and samples returned from Mars will be able to directly show if uninhabited habitats exist or existed on Mars. 相似文献
19.
We investigate whether Earth-type habitable planets can in principle exist in the planetary system of 47 UMa. The system of 47 UMa consists of two Jupiter-size planets beyond the outer edge of the stellar habitable zone, and thus resembles our own Solar System most closely compared to all exosolar planetary systems discovered so far. Our study of habitability deliberately follows an Earth-based view according to the concept of Franck and colleagues, which assumes the long-term possibility of photosynthetic biomass production under geodynamic conditions. Consequently, a broad variety of climatological, biogeochemical, and geodynamical processes involved in the generation of photosynthesis-driven life conditions is taken into account. The stellar luminosity and the age of the star/planet system are of fundamental importance for planetary habitability. Our study considers different types of planetary continental growth models and takes into account a careful assessment of the stellar parameters. In the event of successful formation and orbital stability, two subjects of intense research, we find that Earth-type habitable planets around 47 UMa are in principle possible! The likelihood of those planets is increased if assumed that 47 UMa is relatively young (?6 Gyr) and has a relatively small stellar luminosity as permitted by the observational range of those parameters. 相似文献
20.
The oxidation state of the Earth's surface is one of the most obvious indications of the effect of life on this planet. The surface of Mars is highly oxidized, as evidenced by its red color, but the connection to life is less apparent. Two possibilities can be considered. First, the oxidant may be photochemically produced in the atmosphere. In this case the fundamental source of O2 is the loss of H2 to space and the oxidant produced is H2O2. This oxidant would accumulate on the surface and thereby destroy any organic material and other reductants to some depth. Recent models suggest that diffusion limits this depth to a few meters. An alternative source of oxygen is biological oxygen production followed by sequestration of organic material in sediments--as on the Earth. In this case, the net oxidation of the surface was determined billions of years ago when Mars was a more habitable planet and oxidative conditions could persist to great depths, over 100 m. Below this must be a compensating layer of biogenic organic material. Insight into the nature of past sources of oxidation on Mars will require searching for organics in the Martian subsurface and sediments. 相似文献