Habitable PlanetsEvery substance can exist in different“phases,” which depend on thetemperature. As it cools, the•substance will undergo a transitionfrom the gas, to liquid, to solid phaseat certain critical temperatures. Eachsubstance has its own criticaltemperatures.For life, we need the temperature tobe low enough for complex molecules toform, so this requires temperatures below~ 500 K. But it is difficult to imagine lifewithout a liquid to serve a large numberof functions. And there are very strongarguments that water is an amazinglyunique liquid for this purpose.Several substances remain liquid over a fairly large temperaturerange and are abundant enough so that they might form oceans. (Thisis why Titan, a moon of Saturn, is of such great interest.) But wateris the hands-down winner in several other respects…The temperature of a planet’s surface is mostly controlled by it’s distance toit’s parent star, because that determines how much energy it receives. Theillustration below shows the Sun as it would appear from Pluto: Way too coldfor liquid water Ÿ Pluto is far outside the “habitable zone.”Inside, outside, and within the liquid water habitable zoneWe can see the main effects related to the habitable zone here in our Solar System: Look whathappened to Venus! (Fig. 9.3 in text) Consider how reversed has occurred on MarsA calculation of the continuously habitable zone for the Sun. Notice that theEarth barely is inside!Actually the answer isnot so clear--depends alot on the climate modeland the assumptions.This illustration showsthe results for twochoices of assumptions(Fig. 9.4 in textbook).Time evolution of the Sun’s habitable zone--moves further from Sun as the Sunages and brightens, soon leaving the Earth behind.More complicated version from your textbook (Fig. 9.5). Notice that in the “optimistic”choice, Earth will remain in the habitable zone for 3-4 more billion years.Stars come in many varieties--how should the habitable zone look for each ofthese classes of stars? How long do these different classes or phases last?Which type of star is the most or least numerous?Some properties of main sequence stars of different spectral types (masses). Noticethe huge variation in luminosity and lifetime. These quantities control our decisionsabout which stars we should inspect for terrestrial-mass planets and biomarkers.The stellar luminosity-mass relation.Relative fraction ofdifferent types of stars.Choice seems obvious,but there are someproblems with searchesfor Earth-like planetsaround red dwarfs(spectral class M mainsequence stars).M dwarf habitable zone compared to that of a G-type (solar-like) starLiquid water habitable zone for stars ofdifferent masses (spectral types,luminosities)Habitable Zone (blue band) for different stellar masses (vertical axis). Note line for “synchronous rotation” (tidal locking)M star planets: No longer worried about synchronous rotation/tidallocking/atmospheric freezout, but many M stars are thousands or even millionsof times more active (in flares, etc.) than the SunActive Sun in X-rays M star flares?Don’t forget thepotential influenceof our large moon onhabitability (be ableto name a couple ofits most importanteffects). But ifformed by impact,probably a veryfreakish event, sothis would greatlyreduce the chancesfor life-bearingplanets.The presence of a giant planetaffects the stability of the orbit of aterrestrial-like planet in the habitablezone, if the giant planet orbit issufficiently eccentric.(But recall that an outer giant planetcan also protect inner terrestrial-likeplanets by keeping most of thecomets away, reducing the numberof sterilizing impacts.)An outer giant planet can also affect the rate at which asteroids or comets invade theinner parts of the planetary system. This is a picture of asteroid oribts in our SolarSystem--if not for Jupiter’s strong influence, their eccentricities would be muchsmaller. But Jupiter also keeps comets OUT of the inner solar system, protecting usfrom too many mass extinctions! So the presence of a giant planet, and its properties,may play a large role in determining habitability.Should we search for life, or signals, from binary star systems? There is apotential for unstable planetary orbits, and intolerable climate variation.(Figure is from your textbook.)Binary parent stars again: The “five-to-one rule”--orbits outside the hatchedregions will be greatly perturbed by the companion, leading to irregular,eccentric orbits, or even ejectionA “galactic habitable zone?”--maybe some parts of our Galaxy are morefavorable to planet formation or life than others. (Very speculative).Some ways in which certain locations in our Galaxy might have low probabilitiesof planet formation or might be hazardous for
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