Centauri Dreams
Imagining and Planning Interstellar Exploration
A Brown Dwarf ‘Laboratory’ for Planet Formation
Detecting planets around brown dwarfs is tricky business, but it’s worth pursuing not only for its own sake but because planetary systems around brown dwarfs can tell us much about planet formation in general. A new paper from Andrzej Udalski (Warsaw University Observatory) and colleagues makes this point while noting four brown dwarf planets we’ve thus far found, all of them much larger than Jupiter. An extremely large planet well separated from a brown dwarf suggests a scaled-down binary star system rather than one growing out of an accretion disk.
Fortunately, we can use gravitational microlensing to go after much smaller worlds around brown dwarfs, a method that is not compromised by the faintness of both planet and dwarf. In microlensing we don’t ‘see’ the planet but can infer its presence by observing how light from a more distant star is affected as a brown dwarf system passes in front of it. Udalski and team have used microlensing to discover OGLE-2013-BLG-0723LB/Bb, which appears to be a Venus-mass planet orbiting a brown dwarf.
Image: A brown dwarf in relation to the Sun, a smaller star and planets. Credit: Jon Lomberg.
Andrew Tribick, a Centauri Dreams regular who passed along the link to this paper, notes that the discovery blurs the line between conventional star/planet and planet/satellite configurations. What that suggests is that similar processes are at work within the accretion disks that form around stars and those found around brown dwarfs and even planets. Here’s how the paper reports this:
OGLE-2013-BLG-0723LBb is a missing link between planets and moons. That is, its host OGLE-2013-BLG-0723LB, being a brown dwarf in orbit around a self-luminous star, is intermediate between stars and planets, in both size and hierarchical position. Moreover, the scaled mass and host companion separation of OGLE-2013-BLG-0723LB/Bb are very similar to both planets and moons in the solar system…
As the snip from the paper shows, the brown dwarf in question is itself accompanied by a low-mass M-dwarf star separated some 1.7 AU from the brown dwarf. The planet and brown dwarf, meanwhile, are separated by 0.34 AU. The system is about 1600 light years away in the direction of galactic center. The paper continues by noting similarities to planets and moons in the Solar System:
Both Uranus and Callisto are believed to have formed in the cold outer regions of their respective accretion disks, and are mostly composed of the raw materials of such regions: ice with some rock. In the case of Uranus, it is believed to have been formed closer to the current location of Saturn (10 AU) and to have migrated outward. In the table [showing the physical parameters of the brown dwarf system], the companion-host separations are scaled to the host mass. This is appropriate because the “snow line”, the inner radius at which icy solids can form (2.7 AU in the solar system) increases with host mass, probably roughly linearly. A plausible inference… is that these processes scale all the way from solar-type stars hosting planets, to brown dwarfs hosting “moon/planets”, to giant planets hosting moons.
Several issues remain to be resolved, however. While the researchers believe that the Venus-class planet is orbiting the brown dwarf, this does not guarantee that it was born in an accretion disk around it — planets in close binaries can become perturbed and move from one star to another. If this is the case here, the planet would have similarities to Triton, which is evidently a captured satellite — the authors add that the Neptune-Triton system is scaled to roughly the same parameters as OGLE-2013-BLG-0723LB/Bb.
The other issue is that there is evidence, in the form of excess light in the detection aperture, for a fourth member of this system, one that is likely more massive and luminous than the other three, and separated from them by roughly 100 AU. The presence of this fourth object would obviously affect the system dynamics at work here, complicating the issue of the Venus-class planet’s origin. What we’re left with as this question is followed up is a roughly terrestrial-mass planet orbiting a brown dwarf, a configuration that may be common, with the implication of a formation process that scales down to large planets and their own family of satellites.
The paper is Udalski et al., “A Venus-Mass Planet Orbiting a Brown Dwarf: Missing Link between Planets and Moons” (preprint).
Orbital Change at Ceres (and a Note on the Euphrosynes)
As we close in on perihelion at Comet 67P/Churyumov-Gerasimenko, the Dawn spacecraft continues its operations at Ceres. The contrast between Dawn’s arrival at Ceres in March and New Horizons’ flyby of Pluto/Charon could not have been more striking. With Dawn’s gentle ion push, we watched Ceres gradually grow in the skies ahead, and then settle into focus as the spacecraft began orbital operations. New Horizons was a thrilling, high-velocity fling, with a sudden transition to a backlit Pluto as we settled in to wait for months of data return.
Dawn is now heading for its third science orbit, gradually descending through 1900 kilometers toward an eventual 1500 kilometer altitude above the surface — this is fully three times closer to Ceres than the previous orbit. Again, the gentle nature of ion propulsion is evident, for the spacecraft will reach the new orbit in mid-August, when data operations and imagery again flow. Bear in mind as you think about Pluto and Ceres that the latter is about forty percent the size of Pluto, another dwarf planet (if you’re willing to buy the nomenclature).
Paul Schenk, a geologist at the Lunar and Planetary Institute in Houston, sees a different comparison, however, based on the nature of the surface Dawn has revealed. We’re seeing as much as 15 kilometers difference between crater bottoms and mountain peaks, according to this JPL news release. Says Schenk:
“The craters we find on Ceres, in terms of their depth and diameter, are very similar to what we see on Dione and Tethys, two icy satellites of Saturn that are about the same size and density as Ceres. The features are pretty consistent with an ice-rich crust.”
Image: A portion of the northern hemisphere of Ceres from an altitude of 4,400 kilometers. The image, with a resolution of 410 meters per pixel, was taken on June 25, 2015. Much closer images are on the way once the new science orbit is achieved. Credit: NASA/JPL.
NASA has released a topographic map based on images from Dawn’s framing camera taken at changing viewing angles and Sun positions. It’s a striking reminder of how much we’ve clarified what’s on the surface of the tiny world.
The process of turning terrain into features and thence into names is well advanced, with the International Astronomical Union’s recent approval of names like Occator, the crater in which we find the brightest of Ceres’ mysterious spots. Occator is about 90 kilometers in diameter and 4 kilometers deep. The name comes from a Roman agricultural deity, in keeping with the agriculture theme that begins with the name Ceres itself, Ceres being the Roman goddess of agriculture. A historical footnote: When Giuseppe Piazzi discovered Ceres in 1801, his own suggestion for naming it was Cerere Ferdinandea — Cerere (in Italian) for Ceres, Ferdinandea for King Ferdinand of Sicily. The dual name, thankfully, did not catch.
We also get craters like Haulani, which now designates the smaller of the craters with bright material, a 30-kilometer crater colder than the terrain around it. Other interesting picks: The crater Dantu, after a Ghanaian god, and Ezinu, after the Sumerian goddess of grain. We also have Yalode, a crater named for a Dahomey goddess, and Kerwan, a Hopi name associated with the spirit of sprouting maze. We’re learning a good deal about these craters already.
Enter the Euphrosyne Asteroids
It was not Dawn but the NEOWISE mission (Near-Earth Object Wide-field Infrared Survey Explorer) that helped us understand the group of asteroids known as the Euphrosynes, objects with orbital trajectories that move well above the ecliptic. The eponymous Euphrosyne (you-FROH-seh-nee) is about 260 kilometers across, one of the ten largest asteroids in the main belt. According to this JPL news release, researchers believe it to be a remnant of a collision some 700 million years ago that formed the entire family of smaller asteroids.
The JPL work with NEOWISE was conducted in an attempt to learn more about their relationship with Near Earth Objects, those that have the potential to become problematic because of their close approaches to Earth. Gravitational interactions with Saturn are evidently the reason why the Euphrosynes are a source of some NEOs found on highly inclined orbits. We’re looking at a family of asteroids that can evolve into NEOs given enough time.
“The Euphrosynes have a gentle resonance with the orbit of Saturn that slowly moves these objects, eventually turning some of them into NEOs,” said Joseph Masiero, JPL’s lead scientist on the Euphrosynes study. “This particular gravitational resonance tends to push some of the larger fragments of the Euphrosyne family into near-Earth space.”
Image: The asteroid Euphrosyne glides across a field of background stars in this time-lapse view from NASA’s WISE spacecraft. WISE obtained the images used to create this view over a period of about a day around May 17, 2010, during which it observed the asteroid four times. Because WISE (renamed NEOWISE in 2013) is an infrared telescope, it senses heat from asteroids. Euphrosyne is quite dark in visible light, but glows brightly at infrared wavelengths. This view is a composite of images taken at four different infrared wavelengths: 3.4 microns (color-coded blue), 4.6 microns (cyan), 12 microns (green) and 22 microns (red). Credit: NASA/JPL-Caltech.
Remember that the WISE instrument, having surveyed the entire sky at infrared wavelengths, was put into hibernation in 2011 after cataloguing over 750 million asteroids, stars and galaxies. The spacecraft was re-purposed in the summer of 2013, focusing on asteroids. The JPL study took in 1400 Euphrosyne asteroids, finding them to be dark and in highly inclined, elliptical orbits. Because of their unique nature, says JPL’s Massiero, “…we are able to draw a likely path for some of the unusual, dark NEOs we find back to the collision in which they were born.”
Rosetta’s Comet Nears Perihelion
With the fanfare of the New Horizons flyby of Pluto/Charon, we learned that public interest in space can be robust, at least to judge from the number of people I spoke to who had never previously seemed aware of the subject. Here’s hoping that interest continues to be piqued — as it should be — by the ongoing events at Ceres and on Comet 67P/Churyumov-Gerasimenko. With Ceres we have another exploration of a hitherto unknown surface, while the Rosetta spacecraft is watching surface activity on a comet of the kind we’ve never seen up close.
We’ve already spent a year at the comet since Rosetta’s arrival on August 6 of last year, examining the object’s frozen ices and dust as they vaporize with increasing warmth from the Sun. The gas and dust ‘atmosphere’ thus created, called the coma, can produce the kind of spectacular tails we’ve long associated with comet observations from Earth. Perihelion occurs on August 13, when the comet reaches a distance of 186 million kilometers from the Sun.
Image: The orbit of Comet 67P/Churyumov-Gerasimenko and its approximate location around perihelion, the closest the comet gets to the Sun. The positions of the planets are correct for 13 August 2015. Credit: ESA.
Comet 67P is hardly a Sun-grazer. Its orbit takes six and a half years, taking it to an aphelion of 850 million kilometers (just outside the orbit of Jupiter), while its perihelion is between the orbits of Mars and the Earth. Nonetheless, we’ve already seen increasing activity on the surface as frozen gases sublimate. No one can be sure what will happen as perihelion approaches, but this commentary on the Rosetta blog notes the 500-meter long fracture on the surface of the comet that will bear watching during peak activity. 67P is unlikely to break up (it has survived many previous orbits), but breakups do occur, as happened with Comet C/2012 S1 ISON in 2013.
It will be interesting to see how closely controllers bring Rosetta as perihelion approaches. The craft has been operating no closer than 150 kilometers in the last few months as a precaution against damage from the dust surrounding the nucleus, and because the distance depends on surface conditions, we don’t know just where Rosetta will be on August 13. We should have interesting imagery from perihelion passage relatively soon after the event. The Philae lander, meanwhile, has had only intermittent communications with controllers since regaining the link on June 13. An operational Philae at perihelion would be a bonus.
With just eight days left, keep an eye on the Rosetta blog, whose most recent entry covered the first release of pre-landing phase data from four of Rosetta’s instruments. The Archive Image Browser has also been updated with images from Rosetta’s NAVCAM and includes OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) images from the Earth, Mars and asteroid flybys that occurred enroute to the comet, between 2005 and 2010. You’ll also want to track Rosetta on Twitter @esa_rosetta and there is a Facebook page as well.
To get you in the proper frame of mind, ESA has released this animation.
Image: Images taken by Philae’s ROsetta Lander Imaging System, ROLIS, trace the lander’s descent to the first landing site, Agilkia, on Comet 67P/Churyumov-Gerasimenko on 12 November 2014. The first image was taken just over 3 km from the comet, and indicates the position of Agilkia and the area covered by the next image in the sequence, taken just 67 m away. The six images that follow were taken at approximately 10 second intervals prior to landing, with the final image of the sequence acquired 9 m above the touchdown site. The time the images were acquired, along with distance from the surface and image resolution, are marked on each image. The final slide is annotated with the estimated touchdown position and orientation of Philae, which has been calculated to within ±20 cm. Credit: ESA.
The coarse regolith seen close to touchdown shows grain sizes of 10 to 50 centimeters, and in the closest image, granules less than 10 cm across. Researchers believe the regolith extends to 2 meters deep in places and is free from fine-grained dust deposits. The large boulder visible in the early part of the animation is about 5 meters high. ESA points to its “peculiar bumpy structure and fracture lines running through it that suggest erosional forces are working to fragment the comet’s boulders into smaller pieces.” The trail of debris behind it shows us how particles move about on the surface of the eroding comet.
A ‘Rosetta Stone’ for Super-Earths
The discovery and confirmation of the exoplanet HD 219134b give us a useful touchstone relatively close to the Solar System. At 21 light years away in the constellation Cassiopeia, HD 219134b distinguishes itself by being the closest exoplanet to Earth to be detected using the transit method. That’s useful indeed, because we’ll be able to use future instruments like the James Webb Space Telescope to learn about the composition of any atmosphere there.
Image: This sky map shows the location of the star HD 219134 (circle), host to the nearest confirmed rocky planet found to date outside of our solar system. The star lies just off the “W” shape of the constellation Cassiopeia and can be seen with the naked eye in dark skies. It actually has multiple planets, none of which are habitable. Credit: NASA/JPL-Caltech/DSS.
Too close to its star to be considered a candidate for life, the new world is a ‘super-Earth,’ sighted by the HARPS-North instrument using radial velocity techniques, which measure the pull of the planet on its host star. HARPS-N was built by researchers at the University of Geneva and installed at the 3.6-meter Telescopio Nazionale Galileo on La Palma, in the Canary Islands. Ati Motalebi (UNIGE), lead author of the paper on this work, knew the significance of a potential transit in a world this close, a transit that radial velocity methods couldn’t uncover:
“When the first HARPS-N radial-velocity measurements indicated the presence of a 3-day planet around HD 219134, we immediately asked NASA for Spitzer space telescope time,” said Motalebi. “The idea was to check for a potential transit of the planet in front of the star, a mini eclipse, that would allow us to measure the size of the planet. To do this, we needed to go to space to reach the required precision.”
Initial readings were of a planet with a mass 4.5 times that of the Earth, orbiting the star — a K-dwarf a bit cooler and less massive than the Sun — in three days. Data from the Spitzer instrument then revealed the transit, its measurements indicating the planet to be about 1.6 times larger than the Earth. Combined with the earlier mass calculation, this radius yields a density of six grams per cubic centimeter, pointing to the possibility that this is a rocky planet. Michael Gillon (University of Liege), who led the Spitzer work, calls HD 219134b “a kind of Rosetta Stone for the study of super-Earths.”
HD 219134 turned out to host other worlds as well, with three additional longer-term planets discovered from the radial velocity work. The first of these is 2.7 times as massive as Earth, orbiting in a 6.8 day orbit. A second has 8.7 times Earth’s mass and orbits in 46.8 days. There is also a Saturn-class gas giant at 2.1 AU, orbiting the star in about 3 years.
The possibility exists that the two other inner planets are also transiting worlds, a prospect that has driven planning for future observations. Stéphane Udry (also at UNIGE) considers the potential:
“In particular, the future CHEOPS satellite of the European Space Agency (ESA), developed under Swiss leadership with a strong involvement of UNIGE and of the University of Bern, will provide the perfect tool for such observations. Being able to characterise three transiting super-Earths in a single bright and close system would provide incomparable constraints for planet formation and composition models, in particular for super-Earths.”
Image: Lightcurve of HD 219134b. Credit: UNIGE/NASA/JPL-Caltech.
So HD 219134b, and perhaps its two inner-orbit cousins, could turn out to be a goldmine for future study as we turn CHEOPS as well as the JWST instrument toward them. JWST should be able to use transmission spectroscopy techniques to analyze starlight passing through any planetary atmosphere, while ground-based high-resolution spectroscopy should tell us still more, and there is the prospect of direct imaging of the outer planet in a system this close with the planned giant telescopes in the planning stage, including the European Extremely Large Telescope, the Giant Magellan Telescope, and the Thirty Meter Telescope.
From the paper:
The quality of the measurements of the radius, mass and then mean density actually foreshadows what can be expected from the future transit missions in preparation that will target bright stars (CHEOPS, TESS, PLATO). We also know from Kepler results that multi-transiting systems of small-size planets are numerous. It is then now highly suitable to search for traces of transits of the other planets in the systems. Finally, even if a potential atmosphere around the planet is expected a priori to be tiny, the brightness of the system makes it worth trying to detect features of this atmosphere in the UV, visible and NIR, from space and from the ground, especially in preparation for future measurements with larger facilities…
The paper is Motalebi et al., “The HARPS-N Rocky Planet Search I. HD219134b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun,” accepted at Astronomy & Astrophysics (preprint). Both JPL and UNIGE offer news releases.
Envisioning Starflight Failing
Science fiction has always had its share of Earthside dystopias, but starflight’s allure has persisted, despite the dark scrutiny of space travel in the works of writers like J. G. Ballard. But what happens if we develop the technologies to go to the stars and find the journey isn’t worth it? Gregory Benford recently reviewed a novel that asks these questions and more, Kim Stanley Robinson’s Aurora (Orbit Books, 2015). A society that reaches the Moon and then turns away from it may well prompt questions on how it would react to the first interstellar expedition. Benford, an award-winning novelist, has explored star travel in works like the six novels of the Galactic Center Saga and, most recently, in the tightly connected Bowl of Heaven and Shipstar. His review is a revised and greatly expanded version of an essay that first ran in Nature.
by Gregory Benford
Human starflight yawns as a vast prospect, one many think impossible. To arrive in a single lifetime demands high speeds approaching lightspeed, especially for target stars such as Tau Ceti, about twelve light years away.
Generation ships form the only technically plausible alternative method, implying large biospheres stable over centuries. Or else a species with lifetimes of centuries, which for fundamental biological reasons seems doubtful. (Antagonistic plieotropy occurs in evolution, ie, gene selection resulting in competing effects, some beneficial in the short run for reproduction, but others detrimental in the long.) So for at least for a century or two ahead of us, generation ships (“space arks”) may be essential.
Aurora depicts a starship on a long voyage to Tau Ceti four centuries from now. It is shaped like a car axle, with two large wheels turning for centrifugal gravity. The biomes along their rims support many Earthly lifezones which need constant tending to be stable. They’re voyaging to Tau Ceti, so the ship’s name is a reference to Isaac Asimov’s The Robots of Dawn, which takes place on a world orbiting Tau Ceti named Aurora. Arrival at the Earthlike moon of a super-Earth primary brings celebration, exploration, and we see just how complex an interstellar expedition four centuries from now can be, in both technology and society.
In 2012, Robinson declared in a Scientific American interview that “It’s a joke and a waste of time to think about starships or inhabiting the galaxy. It’s a systemic lie that science fiction tells the world that the galaxy is within our reach.” Aurora spells this out through unlikely plot devices. Robinson loads the dice quite obviously against interstellar exploration. A brooding pessimism dominates the novel.
There are scientific issues that look quite unlikely, but not central to the novel’s theme. A “magnetic scissors” method of launching a starship seems plagued with problems, for example. But the intent is clear through its staging and plot.
I’ll discuss the quality of the argument Aurora attempts, with spoilers.
Plot Fixes
The earlier nonfiction misgivings of physicist Paul Davies (in Starship Century) and biologist E.O. Wilson (in The Meaning of Human Existence) about living on exoplanets echo profoundly here. As a narrator remarks, “Suspended in their voyage as they had been, there had never been anything to choose, except methods of homeostasis.” Though the voyagers in Aurora include sophisticated biologists, adjusting Earth life to even apparently simple worlds proves hard, maybe impossible.
The moon Aurora is seemingly lifeless. Yet it has Earth-levels of atmospheric oxygen, which somehow the advanced science of four centuries hence thinks could have survived from its birth, a very unlikely idea (no rust?—this is, after all, what happened to Mars). Plot fix #1.
This elementary error, made by Earthside biologists, brings about the demise of their colony plans, in a gripping plot turn that leads to gathering desperation.
The lovingly described moon holds some nanometers-sized mystery organism that is “Maybe some interim step toward life, with some of the functions of life, but not all…in a good matrix they appear to reproduce. Which I guess means they’re a life-form. And we appear to be a good matrix.” So a pathogen evolved on a world without biology? Plot fix #2.
Plans go awry. Backup plans do, too. “Vector, disease, pathogen, invasive species, bug; these were all Earthly terms…various kinds of category error.”
What to do? Factions form amid the formerly placid starship community of about 2000. Until then, the crew had felt themselves to be the managers of biomes, farming and fixing their ship, with a bit of assistance from a web of AIs, humming in the background.
Robinson has always favored collective governance, no markets, not even currencies, none of that ugly capitalism—yet somehow resources get distributed, conflicts get worked out. No more. Not here, under pressure. The storyline primarily shows why ships have captains: stress eventually proves highly lethal. Over half the crew gets murdered by one faction or another. There is no discipline and no authority to stop this.
Most of the novel skimps on characters to focus on illuminating and agonizing detail of ecosphere breakdown, and the human struggle against the iron laws of island biogeography. “The bacteria are evolving faster than the big animals and plants, and it’s making the whole ship sick!” These apply to humans, too. “Shorter lifetimes, smaller bodies, longer disease durations. Even lower IQs, for God’s sake!”
Robinson has always confronted the nasty habit of factions among varying somewhat-utopian societies. His Mars trilogy dealt with an expansive colony, while cramped Aurora slides toward tragedy: “Existential nausea comes from feeling trapped… that the future has only bad options.”
Mob Rules
Should the ship return to Earth?
Many riots and murders finally settle on a bargain: some stay to terraform another, Marslike world, the rest set sail for Earth. The ship has no commander or functional officers, so this bloody result seems inevitable in the collective. Thucydides saw this outcome over 2000 years ago. He warned of the wild and often dangerous swings in public opinion innate to democratic culture. The historian described in detail explosions of Athenian popular passions. The Athenian democracy that gave us Sophocles and Pericles also, in a fit of unhinged outrage, executed Socrates by a majority vote of one of its popular courts. (Lest we think ourselves better, American democracy has become increasingly Athenian, as it periodically whips itself up into outbursts of frantic indignation.)
When discord goes deadly in Aurora, the AIs running the biospheres have had enough. At a crisis, a new character announces itself: “We are the ship’s artificial intelligences, bundled now into a sort of pseudo-consciousness, or something resembling a decision-making function.” This forced evolution of the ship’s computers leads in turn to odd insights into its passengers: “The animal mind never forgets a hurt; and humans were animals.” Plot Fix #3: sudden evolution of high AI function that understands humans and acts like a wise Moses.
This echoes the turn to a Napoleonic figure that chaos often brings. As in Iain Banks’ vague economics of a future Culture, mere humans are incapable of running their economy and then, inevitably, their lives. The narrative line then turns to the ship AI, seeing humans somewhat comically, “…they hugged, at least to the extent this is possible in their spacesuits. It looked as if two gingerbread cookies were trying to merge.”
Governance of future societies is a continuing anxiety in science fiction, especially if demand has to be regulated without markets, as a starship must. (Indeed, as sustainable, static economies must.) As far back as in Asimov’s Foundation, Psychohistory guides, because this theory of future society is superior to mere present human will. (I dealt with this, refining the theory, in Foundation’s Fear. Asimov’s Psychohistory resembled the perfect gas law, which makes no sense, since it’s based on dynamics with no memory; I simply updated it to a modern theory of information.) The fantasy writer China Mieville has similar problems, with his distrust of mere people governing themselves, and their appetites, through markets; he seems to favor some form of Politburo. (So did Lenin, famously saying “A clerk can run the State.”)
Aurora begins with a society without class divisions and exploitation in the Marxist sense, and though some people seem destined to be respected and followed, nothing works well in a crisis but the AIs—i.e., Napoleon. The irony of this doesn’t seem apparent to the author. Similar paths in Asimov, Banks and Mieville make one wonder if similar anxieties lurk. Indeed, Marxism and collectivist ideas resemble the similar mechanistic theory of Freudian psychology (both invented by 19th C. Germans steeped in the Hegelian tradition)—insightful definitions, but no mechanisms that actually work. Hence the angst when things go wrong with a supposedly fundamental theory.
The AIs, as revealed through an evolving and even amusing narrative voice, follow human society with gimlet eyes and melancholy insights. The plot armature turns on a slow revelation of devolution in the ship biosphere, counterpointed with the AI’s upward evolution—ironic rise and fall. “It was an interrelated process of disaggregation…named codevolution.” The AIs get more human, the humans more sick.
Even coming home to an Earth still devastated by climate change inflicts “earthshock” and agoraphobia. Robinson’s steady fiction-as-footnote thoroughness brings us to an ending that questions generational, interstellar human exploration, on biological and humanitarian grounds. “Their kids didn’t volunteer!” Of course, immigrants to far lands seldom solicit the views of their descendants. Should interstellar colonies be different?
Do descendants as yet unborn have rights? Ben Finney made this point long ago in Interstellar Migration, without reaching a clear conclusion. Throughout human history we’ve made choices that commit our unborn children to fates unknown. Many European expeditions set sail for lands unseen, unknown, and quite hostile. Many colonies failed. Interstellar travel seems no different in principle. Indeed, Robinson makes life on the starship seem quite agreeable, though maybe tedious, until their colony goal fails.
The unremitting hardship of the aborted colony and a long voyage home give the novel a dark, grinding tone. We suffer along with the passengers, who manage to survive only because Earthside then develops a cryopreservation method midway through the return voyage. So the deck is stacked against them—a bad colony target, accidents, accelerating gear failures, dismay… until the cryopreservation that would lessen the burden arrives, very late, so our point of view characters do get back to Earth and the novel retains some narrative coherence, with character continuity. Plot Fix #4.
This turn is an authorial choice, not an inevitability. Earthsiders welcome the new cryopreservation technologies as the open door to the stars; expeditions launch as objections to generation ships go away. But the returning crew opposes Earth’s fast-growing expeditions to the stars, because they are just too hard on the generations condemned to live in tight environments—though the biospheres of the Aurora spacecraft seem idyllic, in Robinson’s lengthy descriptions. Plainly, in an idyllic day at the beach, Robinson sides with staying on Earth, despite the freshly opened prospects of humanity.
So in the end, we learn little about how our interstellar future will play out.
The entire drift of the story rejects Konstantin Tsiolkovsky’s “The Earth is the cradle of mankind, but humanity cannot live in the cradle forever.” – though we do have an interplanetary civilization. It implicitly undermines the “don’t-put-all-your-eggs-in-one-basket” philosophy for spreading humanity beyond our solar system. Robinson says in interviews this idea leads belief that if we destroy Earth’s environment, we can just move. (I don’t know anyone who believes this, much less those interested in interstellar exploration.) I think both ideas are too narrow; expansion into new realms is built into our evolution. We’re the apes who left Africa.
Robinson takes on the detail and science of long-lived, closed habitats as the principal concern of the novel. Many starship novels dealt with propulsion; Robinson’s methods—a “magnetic scissors” launch and a mistaken Oberth method of deceleration—are technically wrong, but beside the point. His agenda is biological and social, so his target moon is conveniently hostile. Then the poor crew must decide whether to seek another world nearby (as some do) or undertake the nearly impossible feat of returning to Earth. This deliberately overstresses the ship and people. Such decisions give the novel the feel of a fixed game. Having survived all this torment, the returning crew can’t escape the bias of their agonized experience.
Paul Davies pointed out in Starship Century that integrating humans into an existing alien biosphere (not a semi-magical disaster like his desolate moon with convenient oxygen) is a very hard task indeed, because of the probable many incompatibilities. That’s a good subject for another novel, one I think no one in science fiction has taken up. This novel avoids that challenge with implausible Plot fix #2.
Realistically considered, the huge problems of extending a species to other worlds can teach us about aliens. If interstellar expansion is just too hard biologically (as Paul Davies describes) then the Fermi paradox vanishes (except for von Neumann machines, as Frank Tipler saw in the 1970s). If aliens like us can’t travel, maybe they will expend more in SETI signaling? Or prefer to send machines alone? An even-handed treatment of human interstellar travel could shore up such ideas.
Still, a compelling subject, well done in Robinson’s deft style. My unease with the novel comes from the stacked deck its author deals.
Reddish Arcs on Saturn’s Moon Tethys
Looking for a good science fictional link to Saturn’s moon Tethys (you’ll see why in a moment), I came up short until I recalled Harry Bates’ story ‘A Matter of Size.’ First appearing in the April, 1934 issue of Astounding Stories, the novelette tells the breathless tale of giant humanoid beings who live on Tethys, the descendants of a long lost Earth civilization, and their micro-scale counterparts, who keep science alive and kidnap earthmen to use as breeding stock. Poor Tethys, it deserves better at the hand of science fiction authors, though I do note that Healy and McComas incorporated the story in their Adventures in Time and Space (1946), and to be fair, its manic humor includes a sinister ‘marriage machine,’ surely a science fiction first, and a device calculated to strike terror in the hearts of young readers in Bates’ era.
If you know of more respectable appearances of Tethys in science fiction, let me know. Meanwhile, the actual moon is starting to get intriguing. Just over 1000 kilometers across, Tethys was the third of Saturn’s moons to be discovered (by none other than Giovanni Domenico Cassini in 1684). It’s heavily cratered and sports a 400-kilometer impact crater called Odysseus, along with a 2000-kilometer fault known as the Ithaca Chasma. Its high reflectivity and low density (0.98 g/cm3) tell us that it is primarily made of water ice.
Image: This enhanced-color mosaic of Saturn’s icy moon Tethys shows a range of features on the moon’s trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet. Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys’ surface at wavelengths not visible to human eyes. The moon’s surface is fairly uniform in natural color. Credit: NASA/JPL-Caltech/SSI.
Note the gradual color changes across the image, from yellowish to nearly white. A couple of things to keep in mind here: Tethys’ leading hemisphere, which is at the right side of the image, receives a bombardment of ice grains from Saturn’s E-ring. The moon is also subjected to charged particles from Saturn’s radiation belt on the trailing side, causing chemical changes and lowering the moon’s albedo by ten to fifteen percent. The pattern isn’t new — it appears on other Saturnian moons. What is new are arc-shaped reddish streaks now appearing on Tethys.
The unusual features show up in enhanced color imagery from the Cassini spacecraft, appearing as narrow, curved lines that this CICLOPS (Cassini Imaging Central Laboratory for Operations) news release likens to ‘graffiti sprayed by an unknown artist.’ A few of these red arcs show up in earlier observations, but the new images, made in April of this year, are the first to show the northern areas of Tethys under illumination bright enough to make out their extent.
Image: Unusual arc-shaped, reddish streaks cut across the surface of Saturn’s ice-rich moon Tethys in this enhanced-color mosaic. The red streaks are narrow, curved lines on the moon’s surface, only a few kilometers wide but several hundred kilometers long. The red streaks are among the most unusual color features on Saturn’s moons to be revealed by Cassini’s cameras. Credit: NASA/JPL-Caltech/SSI.
What exactly are we looking at? One possibility is that these are features associated with fractures that are below the resolution of the available images. Another idea: Exposed ice with chemical impurities, perhaps resulting from outgassing from within the moon. In any case, we don’t find reddish features anywhere else in the Saturnian system except in a few of Dione’s craters. Where reddish features do occur in large numbers, of course, is on Jupiter’s moon Europa, where the surface is geologically young, just like the surface of Tethys.
Paul Helfenstein (Cornell University) is a Cassini imaging scientist who helped plan the observations:
“The red arcs must be geologically young because they cut across older features like impact craters, but we don’t know their age in years. If the stain is only a thin, colored veneer on the icy soil, exposure to the space environment at Tethys’ surface might erase them on relatively short time scales.”
Interesting. Remember that Cassini has been orbiting Saturn for eleven years now, and it’s clear that we still have surprises ahead. Mission scientists say they are planning to take a closer look at the red arcs of Tethys in November, one that will return images of higher resolution. As the Saturn system has moved into northern hemisphere summer over the past few years, northern latitudes have become much better illuminated. We’re now looking at features of surprising extent whose origin may tell us about Tethys’ composition and its interactions with Saturn.