This finding could help explain how Earth’s magnetic field has lasted for billions of years, researchers added.
Scientists think Earth formed at about the same time as the sun and the rest of the solar system about 4.6 billion years ago from a giant, rotating cloud of gas and dust. Earth and the other rocky planets coalesced from smaller asteroid-sized bodies that accreted or stuck together to form ever-larger chunks of rock.
The meteorites that crash into Earth are usually thought to represent the building blocks that the planet grew from. However, Earth’s crust and mantle puzzlingly have a higher proportion of the element samarium to the element neodymium than seen in most meteorites.
New experiments now suggest that the addition of a sulfur-rich Mercury-like body to the early Earth could explain this anomaly. This research could also help solve another mystery — how the Earth’s magnetic field has lasted for billions of years.
“A Mercury-like body added to Earth during accretion would solve two important problems — that is, kill two birds with one stone,” study co-author Bernard Wood, a geochemist at the University of Oxford in England, told Space.com.
Cooking up the Earth’s core
The researchers performed experiments with samples of material under conditions mimicking those at which Earth formed — temperatures between 2,550 and 3,000 degrees Fahrenheit (1,400 and 1,640 degrees Celsius) and pressures of 1.5 gigapascals. For comparison, 1 gigapascal is nearly 10 times greater than the pressure at the bottom of the Mariana Trench, the deepest part of the ocean.
The samples of material the scientists tested contained traces of elements such as samarium, neodymium, and uranium. These elements are normally chemically attracted to silicate rock, which makes up most of the Earth’s crust and mantle. They do not usually dissolve in iron sulfide, which makes up a significant fraction of Earth’s outer core.
The scientists found that if the early Earth incorporated a rocky body like Mercury, which is high in sulfur, this could make samarium and neodymium dissolve better in iron sulfide. This in turn would make samarium and neodymium more likely to sink down toward Earth’s core.
However, samarium is more attracted to silicate rock than neodymium is. This would have made samarium a bit less likely to sink downward, which could explain why there is a greater proportion of samarium to neodymium in Earth’s crust and mantle.
These experiments could also help solve a mystery concerning Earth’s magnetic field.
Prior research suggests that Earth has possessed a magnetic field for at least 3.5 billion years. Earth’s magnetic field results from churning metal in the planet’s outer core, but it was uncertain how Earth’s core could have remained molten for so long.
The new experiments revealed that if the early Earth engulfed a sulfur-rich Mercury-like body, uranium could have dissolved better in iron sulfide. This in turn would help uranium sink toward Earth’s core. Uranium is a radioactive element that generates heat, which could have kept Earth’s core molten.
Wood and study lead author Anke Wohlers at the University of Oxford detailed their findings in the April 15 edition of the journal Nature.
A telescope will soon allow astronomers to probe the atmosphere of Earthlike exoplanets for signs of life. To prepare, astronomer Lisa Kaltenegger and her team are modeling the atmospheric fingerprints for hundreds of potential alien worlds. Here’s how:
The James Webb Space Telescope, set to launch in 2018, will usher a new era in our search for life beyond Earth. With its 6.5-meter mirror, the long-awaited successor to Hubble will be large enough to detect potential biosignatures in the atmosphere of Earthlike planets orbiting nearby stars.
And we may soon find a treasure-trove of such worlds. The forthcoming exoplanet hunter TESS (Transiting Exoplanet Survey Satellite), set to launch in 2017, will scout the entire sky for planetary systems close to ours. (The current Kepler mission focuses on more distant stars, between 600 and 3,000 light-years from Earth.) [The Search for Another Earth (Video)]
While TESS will allow for the brief detection of new planets, the larger James Webb will follow up on select candidates and provide clues about their atmospheric composition. But the work will be difficult and require a lot of telescope time.
“We’re expecting to find thousands of new planets with TESS, so we’ll need to select our best targets for follow-up study with the Webb telescope,” says Lisa Kaltenegger, an astronomer at Cornell University and co-investigator on the TESS team.
To prepare, Kaltenegger and her team at Cornell’s Institute for Pale Blue Dots are building a database of atmospheric fingerprints for hundreds of potential alien worlds. The models will then be used as “ID cards” to guide the study of exoplanet atmospheres with the Webb and other future large telescopes.
Kaltenegger described her approach in a talk for the NASA Astrobiology Institute’s Director Seminar Series last December.
“For the first time in human history, we have the technology to find and characterize other worlds,” she says. “And there’s a lot to learn.”
Detecting life from space
In its 1990 flyby of Earth, the Galileo spacecraft took a spectrum of sunlight filtered through our planet’s atmosphere. In a 1993paper in the journal Nature, astronomer Carl Sagan analyzed that data and found a large amount of oxygen together with methane — a telltale sign of life on Earth. These observations established a control experiment for the search of extraterrestrial life by modern spacecraft.
“The spectrum of a planet is like a chemical fingerprint,” Kaltenegger says. “This gives us the key to explore alien worlds light years away.”
Current telescopes have picked up the spectra of giant, Jupiter-like exoplanets. But the telescopes are not large enough to do so for smaller, Earth-like worlds. The James Webb telescope will be our first shot at studying the atmospheres of these potentially habitable worlds.
Some forthcoming ground-based telescopes — including the Giant Magellan Telescope (GMT), planned for completion in 2020, and the European Extremely Large Telescope (E-ELT), scheduled for first light in 2024 — may also be able to contribute to that task. [The Largest Telescopes on Earth: How They Compare]
And with the expected discovery by TESS of thousands of nearby exoplanets, the James Webb and other large telescopes will have plenty of potential targets to study. Another forthcoming planet hunter, the Planetary Transits and Oscillations of stars (PLATO), a planned European Space Agency mission scheduled for launch around 2022-2024, will contribute even more candidates.
However, observation time for follow-up studies will be costly and limited.
“It will take hundreds of hours of observation to see atmospheric signatures with the Webb telescope,” Kaltenegger says. “So we’ll have to pick our targets carefully.”
Getting a head start
To guide that process, Kaltenegger and her team are putting together a database of atmospheric fingerprints of potential alien worlds. “The models are tools that can teach us how to observe and help us prioritize targets,” she says.
To start, they have modeled the chemical fingerprint of Earth over geological time. Our planet’s atmosphere has evolved over time, with different life forms producing and consuming various gases. These models may give astronomers some insight into a planet’s evolutionary stage.
Other models take into consideration the effects of a host of factors on the chemical signatures — including water, clouds, atmospheric thickness, geological cycles, brightness of the parent star, and even the presence of different extremophiles.
“It’s important to do this wide range of modeling right now,” Kaltenegger said, “so we’re not too startled if we detect something unexpected. A wide parameter space can allow us to figure out if we might have a combination of these environments.”
She added: “It can also help us refine our modeling as fast as possible, and decide if more measurements are needed while the telescope is still in space. It’s basically a stepping-stone, so we don’t have to wait until we get our first measurements to understand what we are seeing. Still, we’ll likely find things we never thought about in the first place.”
A new research center
The spectral database is one of the main projects undertaken at the Institute for Pale Blue Dots, a new interdisciplinary research center founded in 2014 by Kaltenegger. The official inauguration will be held on May 9, 2015.
“The crux of the institute is the characterization of rocky, Earth-like planets in the habitable zone of nearby stars,” Kaltenergger said. “It’s a very interdisciplinary effort with people from astronomy, geology, atmospheric modeling, and hopefully biology.”
She added: “One of the goal is to better understand what makes a planet a life-friendly habitat, and how we can detect that from light years away. We’re on the verge of discovering other pale blue dots. And with Sagan’s legacy, Cornell University is a really great home for an institute like that.”
A new study sheds light on how exoplanets in tightly-packed solar systems interact with each other gravitationally by affecting one another’s climates and their abilities to support alien life.
Because the exoplanets are so close to one another in these compact solar systems, they have tidal influence, much like the Earth and the moon have on each other. The tides modify the spin rates, axial tilts and orbits of these planets over time, and therefore alter their climates.
The study examines two exo-solar systems — Kepler-62 and Kepler-186 — that have made headlines for hosting worlds orbiting in the “habitable zone,” the potentially life-friendly band where water can remain liquid on a planetary surface. The findings show that tidal evolution can profoundly impact a world’s climate
“We wanted to investigate the question of the influence of tidal dynamics on the climate of ‘habitable’ planets,” said lead author Emeline Bolmont, a post-doctoral research scientist at the University of Bordeaux in France at the time when the research was conducted, and now at the University of Namur in Belgium.
The findings can help astrobiologists understand how habitability is affected by the complex gravitational interplay of neighboring planets. The paper were published in March 2015 in the book “Complex Planetary Systems (IAU S310),” a publication of the International Astronomical Union (IAU).
Almost half of the 1,100-plus exoplanetary systems now known contain multiple planets in the manner of our solar system. Because our ability to discover exoplanets is still at an early stage, our instruments are biased towards detecting planets that closely orbit their host stars. As a result, many of these multi-planet systems we know of look like scrunched-up versions of our solar system. These compact solar systems often have several planets whirling around in orbits within the same distance as Mercury is to the sun.
The proximity of these planets causes them to exert tidal influences on each other, modifying their rotations and axial tilts. The moon’s gravity has similarly acted like a brake on Earth’s rotation, slowing it from a primordial six hour day to the just-shy of the 24 hours we set our clocks to in modern times. The moon’s stabilizing mass also helps maintain Earth’s axial tilt of 23.44 degrees, which gives us our seasons and moderates the planet’s overall temperature, much to life’s benefit.
In the solar systems Kepler-62 and Kepler-186, tidal effects from their various planets and host stars similarly impact the planets’ rotation and axial tilt. The general effect is slowed-down planetary spin rates, as well as axial tilts that are regularized in such a way as to spin perpendicular to the plane of their orbits (they have zero axial tilt). The new study evaluated how the gravity of closely interacting exoplanets might modify these two climate-determining parameters over billions of years. The study also briefly assessed the bigger-picture factors of planets’ orbital shapes and distances to see how stable these would remain in compact multi-planet solar systems. Both variables, of course, have a fundamental impact on a planet’s climatic characteristics.
“The presence of liquid water on a planet’s surface depends on many different parameters, some of which are the orbital distance, the shape of the orbit, the direction of the rotation axis of the planet and the rotation period of the planet,” said Bolmont. “All these quantities are influenced by dynamics and in particular by tidal dynamics.”
The study ran computer simulations of the Kepler-62 and Kepler-186 solar systems using to the best data available. Each system’s star is a red dwarf, which is smaller and dimmer than the sun, and hosts at least five planets. The exoplanets Kepler-62e and Kepler-62f, both super-Earths, orbit in the habitable zone. Kepler-186f, meanwhile, is the first approximately Earth-sized exoplanet discovered in a habitable zone. It is therefore widely considered among the best candidates yet spotted for harboring extraterrestrial life.
The computer simulations focused on how the gravitational push-and-pull of the overall system affected these three exoplanets of interest. For the masses of the exoplanets in their models — which determines the planets’ gravitational attraction — Bolmont and her colleagues assumed Earth-like compositions for all five Kepler-62 worlds. For the Kepler-186 system, the researchers played with the compositions to get different masses to see what would happen. The compositions ranged from pure, low-density ice to pure, high-density iron (higher density packs in more mass to the same volume). [Exoplanet Quiz: Test Your Alien Planet Smarts]
An innovative aspect to the computer simulations is a new code developed by Bolmont and colleagues. The code calculates the gravitational interactions between the stars and the planets in Kepler-62 and Kepler-168, computing the resulting orbital evolution of the planets.
The code is more sophisticated physics-wise than those that have powered prior simulations. It adds to the key tidal effects previously discussed, as well as rotational flattening (spinning bodies bulge at their centers, influencing their orbital evolution) and even Einstein’s general relativity, a more accurate description of gravitation than simple Copernican physics, often used in similar simulations.
“We try to take into account the most important dynamical processes for the evolution of a system,” said Bolmont.
The code will be publicly released soon so other scientists can run simulations and tinker with it.
The Bolmont simulations showed that tidal effects in general can help make compact, multi-planet solar systems more stable. The gravitational interplay in simpler runs of the model, without the added-in, relevant physics, worked in setting planets on wild orbits. The system would destabilize, with planets colliding or getting flung right out of the solar system. A destabilization scenario would almost surely be lethal for whatever life might have gotten going in tight, multi-planet systems.
But the addition of tidal effects and the other physics previously mentioned kept the worlds snugly in their respective orbital lanes, at least for the simulation’s duration. The additional gravitational checks and balances help preserve a solar system, it would appear.
That’s a good sign for life if compressed multi-planet systems can remain together for long periods. Life took several hundred million years to develop on Earth, and a few billion to develop complexity.
Individually, the axial tilts and spin rates of Kepler-62e and Kepler-62f did evolve considerably, and in varying ways, over the course of seven billion years.
“We found that Kepler-62e and f are likely to have different climates,” said Bolmont,
Kepler-62e, according to the simulation, is likely to have a very small axial tilt, thanks to the braking as well as accelerative effects from the other planets in its solar system. Lacking much tilt, Kepler-62e would not experience seasons and its poles would be quite cold. Earth, with its seasons, has cold poles too, of course, when compared to its hot equatorial regions. But the difference in temperature on Kepler-62e between its equator and poles would be far more pronounced.
The exoplanet’s rotation would possibly slow to a day-length equivalent of 125 or so Earth days. A planet’s rotation also contributes to moderating its surface temperatures, like a roast turned on a spit, such that one portion of the meat does not singe black while the rest is merely warmed. In the case of Kepler-62e, with its very slow turning, the side of the planet facing its star heats up considerably more than the night side, plunged into darkness for a third of an Earth-year.
Kepler-62f, on the other hand, is located farther out in the exo-solar system than planet ‘e.’ The gravitational perturbation from the star and inner planets would not be as strong in the outer reaches. Even after seven billion years, Kepler-62f would not have had its axial tilt abolished by the solar system’s other bodies. Kepler-62f should therefore still have an axial tilt, and thus seasons, and a day length perhaps broadly similar to Earth’s.
“Kepler-62f is located farther and wouldn’t have had time to tidally evolve,” said Bolmont.
The case for Kepler-186f is less clear-cut. We know the age of the Kepler-62 solar system, but do not know it yet for Kepler-186. That data is important because the tidal evolution dynamics require long time scales to bring about significant changes in a planet’s parameters. By making some assumptions, though, the Kepler-186 system model can still offer insight.
Assuming that the whole system is older than four billion years, as a separate recent study has suggested, then the four innermost planets in Kepler-186, being located so close to their star, will likely have had any axial tilt to be erased. In the case of Kepler-186f, the outermost planet and the one of interest in its potential habitability, an old solar system would mean it, too, has little to no axial tilt and a day-length of approximately 125 Earth-days.
If the Kepler-186 system is less than a billion years, Kepler-186f might still have a high axial tilt and a fast spin rate, more like Earth’s. The axial tilt might be so high, the models showed, on the order of 80 degrees, that the planet could be spinning on its “side,” as it were, like Uranus in our solar system. (Uranus is thought to have been knocked on its side by a collision at some point in its planetary lifetime. The world is too isolated for the Sun or other planets to tidally “right” the planet back up.) Under that scenario, Kepler-186f would develop a very cold hemisphere that is pointed away from the star, and a possibly too-warm hemisphere facing the star.
Given the holes in the data, the jury is very much still out on how much Kepler-186f’s evolution is tidally influenced.
“We don’t have enough data, such as the age of the system,” said Bolmont.
The overall takeaway from the study is that planets can indeed gravitationally influence each other in compact solar systems in ways that heavily influence climate and therefore habitability. Much more work needs to be done in this area, said Bolmont, to better learn how orbital shapes and distances change over time.
“These are still open questions,” said Bolmont. “There is a lot of diversity in the orbits of the habitable zone planets, and thus in the climate of habitable worlds.”
Scientists searching for signs of intelligent extraterrestrial life in the universe have a new telescope tool to aid them in their hunt for potential alien civilizations.
Called NIROSETI, short for Near-Infrared Optical Search for Extraterrestrial Intelligence, the instrument saw its “first light” this month at the University of California’s Lick Observatory atop Mt. Hamilton east of San Jose. It is built to record levels of light over time so that patterns can be analyzed for potential signals of alien life.
For more than five decades, scientists have been on the lookout for radio signals from other starfolk. But instruments capable of capturing pulses of infrared light have only recently become available. The NIROSETI instrument is attached to the Lick Observatory’s Nickel 1-meter telescope, with months of fine-tuning to follow its first-light observation on March 15
Shelley Wright, an Assistant Professor of Physics at the University of California, San Diego, led the development of NIROSETI while at the University of Toronto’s Dunlap Institute for Astronomy & Astrophysics.
Infrared light penetrates farther through gas and dust than visible light. So this new search will extend to stars thousands rather than merely hundreds of light-years away.
NIROSETI could uncover new information about the physical universe as well – as well as help shape an answer to some big questions: Are we alone? Just how crowded is it out there?
The group making the NIROSETI campaign possible also includes SETI pioneer Frank Drake of the SETI Institute and UC Santa Cruz who serves as a senior advisor to both past and future projects and is an active observer at the telescope.
Regarding use of NIROSETI there is one downside, according to Drake.
“The extraterrestrials would need to be transmitting their signals in our direction,” Drake said in a UC San Diego statement, although he sees a positive side to that limitation. “If we get a signal from someone who’s aiming for us, it could mean there’s altruism in the universe. I like that idea. If they want to be friendly, that’s who we will find.”
Funding for the project comes from the financial support of Bill and Susan Bloomfield.
Astronomers have spotted a fourth star in a planetary system called 30 Ari, bringing the number of known planet-harboring quadruple-sun systems to two. Numerous two- and three-star exoplanets have been identified.
“Star systems come in myriad forms. There can be single stars, binary stars, triple stars, even quintuple star systems,” study lead author Lewis Roberts, of NASA’s Jet Propulsion Laboratory in Pasadena, California, said in a statement. “It’s amazing the way nature puts these things together.”
30 Ari lies 136 light-years from the sun in the constellation Aries. Astronomers discovered a giant planet in the system in 2009; the world is about 10 times more massive than Jupiter and orbits its primary star every 335 days. A second pair of stars lies approximately 1,670 astronomical units (AU) away. (1 AU is the distance between Earth and the sun — about 93 million miles, or 150 million kilometers).
Roberts and his colleagues used the new “Robo-AO” adaptive optics system at the Palomar Observatoryin California to sweep the sky, examining hundreds of stars each evening for signs of multiplicity. This search identified a fourth star in close proximity to 30 Ari’s primary star.
The newfound star circles its companion once every 80 years, at a distance of just 22 AU, but it does not appear to affect the exoplanet’s orbit despite such proximity. This is a surprising result that will require further observations to understand, researchers said.
To a hypothetical observer cruising through the giant planet’s atmosphere, the sky would appear to host one small sun and two bright stars visible in daylight. With a large enough telescope, one of the bright stars could be resolved into a binary pair.
The discovery marks just the second time a planet has been identified in a four-star system. The first four-star planet, PH1b or Kepler-64b, was spotted in 2012 by citizen scientistsusing publicly available data from NASA’s Kepler mission.
Planets with multiple suns have become less of a novelty in recent years, as astronomers have found a number of real worlds that resemble Tatooine, Luke Skywalker’s home planet in the Star Warsfilms.
Indeed, binary stars are more commonthan their singleton counterparts. And the new study suggests that more planetary systems with two pairs of binary stars may be discovered down the road.
“About four percent of solar-type stars are in quadruple systems, which is up from previous estimates because observational techniques are steadily improving,” co-author Andrei Tokovinin, of the Cerro Tololo Inter-American Observatory in Chile, said in the same statement.
In addition to finding a fourth star around 30 Ari, the team also found a third star in a planetary system previously thought to have only two suns.
This system, known as HD 2638, was already known to host a planet with half the mass of Jupiter rushing around its primary star once every 3.4 days, while a second star lies about 44,000 AU, or 0.7 light-years, away. The newly discovered third star sits just 28 AU from the primary star, and it appears to have influenced the orbit of the gaseous planet, researchers said.
The more scientists learn about Mars, the more intriguing the Red Planet becomes as a potential haven for primitive life in the ancient past … and perhaps even the present.
A study released today (March 23) reports that ancient Mars harbored a form of nitrogen that could potentially have been used by microbes, if any existed, to build key molecules such as amino acids. An unrelated study suggests that atmospheric carbon monoxide has been a feasible energy source for microbes throughout the Red Planet’s history. Both papers were published today in the journal Proceedings of the National Academy of Sciences (PNAS).
“It’s more support for this environment that would have had the ingredients that life would have needed,” said Jennifer Stern of NASA’s Goddard Space Flight Center in Greenbelt, Maryland, lead author of the nitrogen study. [The Search for Life on Mars: A Photo Timeline]
All life on Earth requires nitrogen, which is a critical component of amino acids and other biomolecules. But microbes can’t just pull their nitrogen straight out of the air; atmospheric, or molecular, nitrogen (N2) features two atoms of the stuff linked in a tight triple bond, making it relatively inert and inaccessible.
Before life-forms can incorporate nitrogen into their metabolic processes, that bond must be broken; nitrogen must be “fixed” into different, more chemically reactive compounds, such as nitrate (NO3).
That process did indeed occur on Mars, Stern and her team reported in their study, which looked at measurements made by the Sample Analysis at Mars (SAM) instrument aboard NASA’s Mars rover Curiosity.
SAM found significant concentrations of nitrate in soil and rock samples that Curiosity collected at three different spots near its landing site — Rocknest, John Klein and Cumberland.
The John Klein and Cumberland samples, which were drilled from a sedimentary mudstone, had previously allowed rover team members to conclude that, billions of years ago, the area was part of a potentially life-supporting lake-and-stream system. The discovery of fixed nitrogen contributes to this habitability picture.
“Had life been there, it would have been able to use this nitrogen,” Stern told Space.com.
While much of the nitrogen fixation on Earth is biological, Curiosity’s discovery isn’t evidence of Martian life. Nitrogen-nitrogen bonds can also be broken by the thermal shocks caused by lightning and asteroid or comet impacts.
Indeed, the Red Planet’s fixed nitrogen may have been generated primarily by the numerous powerful impacts that occurred (on Mars and other bodies in the inner solar system) about 4 billion years ago, during a period known as the Late Heavy Bombardment, Stern said.
But nitrogen may get fixed on modern Mars as well. In 2005, Europe’s Mars Express orbiter detected nitrogen oxide (NO) high in the Red Planet’s atmosphere. It likely formed after sunlight split apart oxygen, carbon dioxide and molecular nitrogen, Stern and her co-authors said.
“This suggests that N is currently being fixed in the Martian thermosphere, although it is unknown how much, if any, is transported to the lower atmosphere and surface,” the researchers wrote in their PNAS paper.
Curiosity hasn’t been able to get to the bottom of this question so far.
“Right now, our experiment is not targeted to get us a nitrate signal big enough to get, for example, any nitrogen isotope data,” Stern said. (Isotopes are versions of an element that contain different numbers of neutrons in their nuclei.)
“If you had a nitrogen isotope composition of the modern [Martian] atmosphere, which would be very different than the primordial atmosphere, that would tell us about whether it was being formed today or not,” she added. “So it would be great to be able to target an experiment where we could get enough of a signal in the instrument to get that data.”
Energy source for Martian life?
Life as we know it needs certain basic building chemical blocks (such as carbon and fixed nitrogen), liquid water and an energy source. In the other new PNAS paper, Gary King of Louisiana State University suggested that carbon monoxide (CO) could serve as an energy source on Mars, from ancient epochs all the way up to the present day.
While CO is toxic to many organisms, including humans, here on Earth, some microbes use it to drive their metabolism, gaining energy by oxidizing the substance into carbon dioxide (CO2).
Such life-forms are taking advantage of a relatively scarce resource, as Earth’s atmosphere is just 0.3 parts per million (ppm) or so CO by volume. The Martian atmosphere, in comparison, contains 800 ppm CO currently, and concentrations of the stuff may have been much higher in the past. Therefore, CO seems like a plausible candidate for an energy source for Mars life, but the possibility hasn’t drawn much scholarly attention, King wrote in the PNAS paper.
King set out to determine if Earth microbes could indeed utilize CO under conditions approximating those found on the modern Martian surface — low pressure, high CO2 concentrations (CO2 makes up 95 percent of the Red Planet’s atmosphere), low oxygen levels and low to moderate temperatures, among other characteristics.
King specifically targeted the conditions that might prevail at features known as recurring slope lineae (RSL), seasonal dark streaks that have been observed by NASA’s Mars Reconnaissance Orbiter in a number of locales. Some scientists think these streaks are caused by salty water at or near the Red Planet’s surface.
He found that soil samples collected in three different salty systems on Earth — the Big Island of Hawaii, Chile’s Atacama Desert and the Bonneville Salt Flats in Utah — did indeed take up CO under putative RSL conditions.
Other experiments, using the salt-loving (halophilic) microbes Alkalilimnicola ehrlichii MLHE-1 and Halorubrum str. BV1, demonstrated this capacity at the organismal level. A. ehrlichii MLHE-1, in fact, tolerated concentrations of the chemical perchlorate similar to those found in Martian soil.
“These results collectively establish the potential for microbial CO oxidation under conditions that might obtain at local scales (e.g., RSL) on contemporary Mars and at larger spatial scales earlier in Mars’ history,” King wrote in the new study.
King believes his results are also relevant to discussions of the human exploration of Mars. CO-oxidizing organisms such as A. ehrlichii MLHE-1 could be part of an effort to transform the Red Planet into a place more hospitable to humans, he said.
“In order to develop any kind of a soil system that could support anything complex, you would have to have a complex microbial community,” King told Space.com.
“You would need a variety of biosynthetic capabilities. You would need a variety of different elemental transformation capabilities — maybe nitrogen fixers,” he added. “These halophiles would be part of that.”
Based on the orbits of these planets, 18th century European astronomers invented what is now called the Titius-Bode relation. It’s a simple empirical relation that describes the relative distances between the planets and the sun. It predicted the orbit of another planet beyond Saturn and another planet in the gap between Mars and Jupiter.
In 1781, William Herschel found Uranus – without relying on the Titius-Bode relation – but he found it in the orbit beyond Saturn where the Titius-Bode relation said it would be.
After this success, astronomers started looking for a planet between Mars and Jupiter in the orbit predicted by the Titus-Bode relation.
In 1801, Giuseppi Piazzi found a planet in the predicted position and called it Ceres. The Titius-Bode relation was on a roll.
But when Neptune was found in 1846 it wasn’t exactly where the Titus-Bode relation predicted it would be. And over the years so many small bodies have been found in orbits between Mars and Jupiter that Ceres was plutoed – demoted to an “asteroid”.
And so the Titus-Bode relation lost its shine. And like an old horse, it was put out to pasture. It was only taken seriously by numerologists and cranks.
The search for extrasolar planets
But then along came NASA’s Kepler Space Telescope. Over the past few years Kepler has been able to detect thousands of exoplanets and hundreds of multi-exoplanet systems.
Along with my PhD student Tim Bovaird and Master’s student Steffen Jacobsen, we reasoned that if the TB relation had been such a useful (if somewhat imperfect) guide for predicting planets in our solar system, maybe it would be useful in predicting planets in the new exoplanetary systems detected by Kepler.
We checked the hundred or so systems where Kepler had found at least a few planets and we found that the majority of these exoplanetary systems adhered to the Titus-Bode relation even somewhat better than our solar system did.
Thus, we became convinced that the horse still had some miles left in her – that the semi-taboo Titus-Bode relation could provide useful hints about the periods of as-yet-undetected planets around other stars.
Last year we used a generalised Titus-Bode relation to analyse 68 multi-planet systems with four or more detected exoplanets. We made predictions for the existence of more planets in these systems, based on the Titus-Bode relation.
So far, 5% of our predictions have been confirmed. This may sound like a small percentage, but given the inability of the Kepler telescope to see Earth-sized planets or smaller, a 5% detection rate is what you would expect to see if all the predictions were true.
Almost all of the exoplanets detected by Kepler are larger than Earth and very close to their host stars. This is almost certainly a selection bias.
It is very difficult for the Kepler telescope to spot planets that are far enough away from their host stars to be in the habitable zone (where the temperatures are in the range where H2O will be liquid water).
Using the Titus-Bode relation is a controversial indirect technique, but I think it’s the best one we have if we are interested in answering the question: How many planets (on average) are in the habitable zones of stars?
How many potentially habitable planets?
Our answer to this question is 2 ± 1 and was published this week in the Monthly Notices of the Royal Astronomical Society. The figures (above and below) illustrate our result.
With about 300 billion stars in our galaxy, our result means there are 600 ± 300 billion planets in circumstellar habitable zones in our galaxy.
In the observable universe there are about 100 billion galaxies. Thus there are approximately 1022 stars in the observable universe and twice that many planets in circumstellar habitable zones in the universe.
That’s a lot of real estate for alien development. Not all of these habitable zone planets will be wet and rocky like the Earth, but a fair fraction (about 30%) should be. Now we need some zippy interstellar spaceships to colonise and over-populate all these worlds before the aliens do.
This article was originally published on The Conversation. Read the original article. Follow all of the Expert Voices issues and debates — and become part of the discussion — on Facebook, Twitter and Google +. The views expressed are those of the author and do not necessarily reflect the views of the publisher. This version of the article was originally published on Space.com.
The space agency is using glasses from Osterhout Design Group (ODG), a San Francisco-based company that develops wearables for enterprises and government use. NASA engineers and astronauts are set to test the company’s smart glasses, which are equipped with augmented reality and virtual reality technologies. The glasses are being tested using NASA applications and software.
“The intended purpose and usefulness of glasses like this are unlimited,” said Jay Bolden, a NASA spokesman, in an email to Computerworld. “Advanced glasses could aid in navigation, where cockpit displays are broadcast on the goggles in much the same way fighter pilot heads up displays operate today.”
Bolden also noted that astronauts on a journey to an asteroid or Mars could use the smart glasses to access chart, map and technical information, instead of having to carry many pounds of technical journals and papers with them.
“For a two-hour flight on a 737 from Cleveland to Dallas, each pilot carries 15 pounds of manuals and that weight isn’t really a big deal in the grand scheme,” he noted. “However, for a multiple-week mission to an asteroid or the moon, or a multi-year mission to Mars, every pound saved means additional life-critical supplies — food, water, oxygen, or fuel — can be shipped in their place.”
The smart glasses also could give more information to NASA engineers and scientists working on Earth.
“Real time applications also include the ability for ground support teams to see first hand what astronauts discover and video,” Bolden said. “Instead of bringing a 50-pound boulder back for ground analysis, the astronaut can use glasses to scan, measure and catalog where it was found and then chip off a 5-pound sample for ground analysis.”
NASA’s prolific Kepler space telescope, which has discovered more than half of all known planets beyond our solar system, just celebrated six years in space.
The $600 million Kepler mission blasted off atop a United Launch Alliance Delta II rocket from Florida’s Cape Canaveral Air Force Station on the night of March 6, 2009 (March 7 GMT). After a two-month commissioning phase, Kepler began searching for exoplanets — and began etching its name into the history books.
Kepler finds alien worlds by watching for the tiny brightness dips they cause when they cross the face of their host stars from the spacecraft’s perspective. (During its original mission, Kepler stared at more than 150,000 stars simultaneously.)
This technique has been incredibly successful. To date, the sun-orbiting spacecraft has discovered 1,019 exoplanets, with more than 3,100 additional “candidates” awaiting confirmation by follow-up observations or analysis. Mission scientists expect that around 90 percent of these potential planets will end up being the real deal.
To put Kepler’s tally into perspective: Scientists have discovered a total of about 1,800 alien planets. (The number varies a bit depending upon which database is consulted.)
But Kepler has never just been about raw numbers. The main goal of its original mission was to help researchers determine how common Earth-like planets are throughout the Milky Way galaxy. And the spacecraft’s observations suggest that worlds like our own are very common indeed: About one in five sunlike stars probably harbors an Earth-size planet in its “habitable zone,” the range of distances that could support the exsitence of liquid water.
Many more potentially habitable worlds circle red dwarfs, the small, dim stars that make up 70 percent of the Milky Way’s stellar population. So our galaxy apparently teems with tens of billions of rocky, habitable-zone planets, researchers say.
Kepler’s original planet hunt ended in May 2013, when the second of the spacecraft’s four orientation-maintaing reaction wheels failed, robbing Kepler of its ultraprecise pointing ability.
But the telescope continues to study the heavens during a new mission called K2, which NASA approved in May 2014. K2 calls for a compromised Kepler to observe broader patches of sky for a variety of celestial objects and phenomena, including faraway supernova explosions, comets and asteroids in our own solar system — and exoplanets.
K2 has shown that Kepler can still find alien worlds with just two working reaction wheels: Researchers announced the new mission’s first exoplanet in December 2014.
Curiosity, the robotic rover that has been working on the surface of Mars since August 2012, finally successfully moved a sample of powdered rock from its drill to onboard scientific instruments after the rover had sat motionless — with the powder — for 13 days.
That said, the rover is not yet able to drill for new powder. NASA engineers are still figuring out a fix for the short circuit, and until they do, the drill isn’t operational. But the rover can move around.
And move it will. Now that Curiosity has been taken out of safe mode, it will soon continue on its journey, heading further up the 18,000-foot Mount Sharp, which has always been its ultimate destination.
The robotic rover ran into trouble on Feb. 27 when it was in the process of moving the rock powder from its arm into the analytical instruments. A short circuit caused the machine to stop working and put itself into a safe mode, alerting NASA that there was a problem.
According to NASA, the problem was found to be a transient short in the motor for the drill’s hammering action. The drill, with both a rotary and hammering action, sits on the robot’s arm.
The hunt for signs of life on planets beyond our solar system should cast as wide a net as possible, some researchers stress.
Scientists scanning the atmospheres of exoplanets for gases produced by alien life should look for more than just oxygen, methane and the other familiar biosignatures that swirl about in Earth’s air, Sara Seager and William Bain, both of MIT, wrote in a review article published today (March 6) in the journal Science Advances.
“We know there will not be huge numbers of accessible planets,” Seager told Space.com via email. “We want to make sure we do not miss any signatures, by trying our best to think outside the box. Oxygen is a great biosignature gas for Earth, but what are the chances it will be present on an exoplanet?”
A diversity of worlds
To date, scientists have discovered more than 1,800 alien planets, most of which are very different from the worlds in our solar system.
“A specific, astonishing finding is that the most common type of planet in our galaxy are those with sizes between those of Earth and Neptune — a new class of planet that is neither terrestrial nor giant and one without an accepted theory for its formation,” Seager and Bain wrote.
The diversity of exoplanets reinforces the very real possibility that alien life may be quite different from life on Earth, even if it inhabits a rocky world like our own. For example, what might live on “exo-Earths” whose atmospheres are dominated by molecular hydrogen instead of nitrogen and oxygen, as Earth’s is?
“Although not yet observed, such planets are theoretically anticipated,” Seager and Bains wrote.
Based on that reasoning, the researchers advocate an open-minded approach that would first identify “all viable biosignature gases, through a systematic, exhaustive study both from the view of molecules (there is no shortage) and of planetary environments and where the candidate biosignature gas molecules would accumulate and survive,” they wrote.
“The near-term goal is to understand which molecules could be biosignature gases in atmospheres of exoplanets; a systematic table of chemicals made by life will give a starting point for predicting which molecules are stable, volatile and detectable remotely by space telescopes,” Seager and Bains added.
Such a challenging project would likely take years to complete, Seager told Space.com. But researchers can spare the time because a systematic search for signs of life on alien worlds is probably at least a decade away, she and Bains wrote.
Ramping up the search
Scientists have already begun probing exoplanet atmospheres, using instruments such as the European Southern Observatory’s Very Large Telescope in Chile.
And the effort will kick into higher gear soon, with the launch of NASA’s Transiting Exoplanet Survey Satellite (TESS) in 2017 and the agency’s James Webb Space Telescope (JWST) in 2018. TESS should find a number of nearby rocky planets whose atmospheres JWST can investigate. (Most exoplanets found to date, including those found by NASA’s prolific Kepler space telescope, are too far away for such follow-up study.)
Massive ground-based telescopes, such as the Giant Magellan Telescope, Thirty Meter Telescope and European Extremely Large Telescope — which boast light-collecting surfaces 80 feet (24 meters), 98 feet (30 m) and 128 feet (39 m) wide, respectively — will boost the search further when they come online in the mid-2020s.
But Seager and many other experts say that the biosignature search really needs a space telescope with a mirror in the 33- to 39-foot (10 to 12 m) range — something like the proposed Advanced Technology Large-Aperture Space Telescope, or ATLAST.
Such an instrument could potentially analyze enough exoplanet atmospheres for researchers to do some number crunching. And that’s important; the biosignature hunt will probably center on probabilistic inference because a slam-dunk detection will be difficult, if not impossible, to make, Seager and Bains wrote.
“I see the future for biosignature gases akin to Kepler’s findings,” Seager told Space.com. “Kepler told us that small planets are very common. We have some specifics (specific small planets in stars’ habitable zones), but the information most useful was statistical. If we find that so many planets have unusual gases, we may be able to convince ourselves that life beyond Earth exists, but not necessarily [on] any one planet specifically.”
Further research to refine these maps could help guide the quest to identify underground reservoirs on Mars, the scientists added. A new NASA video describes the ancient ocean on Mars.
Although the Martian surface is now cold and dry, there is plenty of evidence suggesting that rivers, lakes and seas covered the Red Planet billions of years ago. Since there is life virtually wherever there is liquid water on Earth, some researchers have suggested that life might have evolved on Mars when it was wet, and life could be there even now, hidden in subterranean aquifers.
Much remains unknown about how Mars lost its water and how much liquid water might remain in underground reservoirs. One way to solve these mysteries is to analyze the kinds of water molecules in the Martian atmosphere.
Normally, water molecules are each made up of two hydrogen atoms and one oxygen atom. However, one or both of these hydrogen atoms can be replaced with deuterium atoms to create deuterated water. (Deuterium, like hydrogen, has one proton, but also one neutron.)
Deuterated water is heavier than normal water, so it behaves differently. For example, it can be easier for normal water to escape Mars, since it can vaporize more easily in the Martian atmosphere. Solar radiation can break this water up into hydrogen and oxygen, and the hydrogen can then escape into space.
By studying the current ratio of deuterium to hydrogen in Martian water, researchers suggested they could estimate how much total water the Red Planet used to have. They constructed new maps of the ratio between hydrogen and deuterium in the water in the Martian atmosphere using data gathered from 2008 to 2014 by the Very Large Telescope in Chile, and the Keck Observatory and NASA’s InfraRed Telescope Facility in Hawaii.
They found the ratio between deuterated water and normal water in some regions of Mars was higher than thought, typically seven times higher than in Earth’s oceans. This high ratio suggests that Mars has lost a great deal of water over time.
“We can now get a pretty strong estimate of how much water was lost on the planet,” lead study author Geronimo Villanueva, a planetary scientist at NASA Goddard Space Flight Center in Greenbelt, Maryland,told Space.com.
Based on their findings, the scientists estimate that Mars might have had enough water to cover up to 20 percent of the planet about 4.5 billion years ago. They suggest the Red Planet could still possess substantial underground reservoirs of water.
Further refining maps of atmospheric water on Mars could help guide the search for these deep aquifers, Villanueva said. One would essentially look at such maps to see how much known sources of water such as Martian ice caps could account for this atmospheric water, “and any abnormalities might be released from hidden reservoirs,” he said.
Planets spinning on their sides were long thought to have climates too extreme for life as we know it on Earth, but now, scientists have found that some of these “rotisserie” worlds might be more hospitable.
If these alien planets, which rotate sideways like a pig on a spit, are covered in oceans, they could actually have a mild, springlike climate all year, scientists say, potentially expanding the number of potentially habitable planets where life may be found.
In the past two decades or so, astronomers have confirmed the existence of more than 1,800 worlds orbiting distant stars, raising the possibility that some of these exoplanets might be home to extraterrestrial life. The search for aliens often focuses on planets that resemble Earth, the only world known by humans to host life
One key factor affecting whether a planet might be habitable is its obliquity, the degree to which the axis on which the planet spins tilts.This influences the amount of sunlight any point on the planet experiences over the course of a year. The greater a world’s obliquity, the more extreme its seasons are.
Earth has a relatively low axial tilt of about 23.5 degrees. However, researchers suspect that exoplanets may display a range of obliquities, resembling anything from a vertical spinning top to a horizontal rotisserie.
Scientists had thought that the more extreme the tilt, the less habitable a world would be.
“The expectation was that such a planet would not be habitable — it would basically boil, and freeze, which would be really tough for life,” lead author of the exoplanet study David Ferreira, a climate scientist at the University of Reading in England, said in a statement.
However, Ferreira and his colleagues’ new findings challenge those expectations, showing that such extremely tilted planets may remain habitable if covered entirely by oceans. “In the search for habitable exoplanets, we’re saying, don’t discount high-obliquity ones as unsuitable for life,” Ferreira added in a statement.
To see what life might be like on habitable planets with extreme tilts, researchers simulated Earth-size planets covered entirely in water circling their stars at the same distance as Earth orbits the sun. The 3D models simulated circulation among the atmosphere, ocean and sea ice on “aquaplanets” with oceans 1.8 miles (3 kilometers) deep and “swamp” planets with relatively shallow oceans that were 33 feet (10 meters), 165 feet (50 m) or 655 feet (200 m) deep.
The investigators simulated planets at three obliquities. The first was 23.5 degrees, like Earth’s. The next was 54 degrees, the point at which the poles receive more annual sunlight on average than the equator. The last was 90 degrees, the point at which a planet is essentially lying on its side — the poles would each point at the star for a quarter of the year, and then away for another quarter, alternating between extremes of light and darkness.
Ferreira and his colleagues found that a global ocean would absorb enough solar energy from the star and release it back into the atmosphere for such a world to maintain a rather mild, springlike climate year round.
“We found that the ocean stores heat during summer and gives it back in winter, so the climate is still pretty mild, even in the heart of the cold polar night,” Ferreira said.
Even a shallow global oceanonly about 165 feet (50 m) deep would be enough to keep a high-obliquity planet at an average of about 60 degrees Fahrenheit (15.5 degrees Celsius) year-round.
“The most surprising result here is how little ocean is needed to maintain a mild climate at the poles, even in the heart of winter and summer times,” Ferreira told Space.com. “We were not expecting how efficient an ocean, even a shallow one, would be at mitigating temperature.”
Past research had suggested that great differences in temperature between the dark and light sides of a high-obliquity planet might lead to powerful weather. However, the scientists did not seea strong difference in the intensity of weather on such worlds compared to the weather on Earth. Instead, “at high obliquity, more active weather occurs in summer, while winters are quiet times in terms of storm activity,” Ferreira said. “That is the opposite of what happens on Earth.”
The simulations found that life could thrive on a highly tilted watery planet, but only up to a point. Waters up to 33 feet (10 m) deep would not absorb enough heat to help keep planetary climates habitable. Instead, as soon as ice formed on the dark side of such a planet, the ice would quickly spread. The resulting massive ice sheets would reflect the rays of the planet’s star, keeping the planet cold and helping the ice spread further. The resulting runaway effect would eventually envelop the planet in ice.
“Some people have thought that a planet with a very large obliquity could have ice just around the equator, and the poles would be warm,” Ferreira said in a statement. “But we find that there is no intermediate state. If there’s too little ocean, the planet may collapse into a snowball. Then it wouldn’t be habitable, obviously.”
In the future, the researchers may simulate worlds covered with both land and water. Ferreira and his colleagues — John Marshall, Paul O’Gorman and Sara Seager, all at MIT — detailed their findings in the Nov. 15 issue of the journal Icarus.
In the past two decades or so, researchers have confirmed the existence of more than 1,800 exoplanets orbiting distant stars. These discoveries have revealed very different kinds of planets from those seen in the solar system, such as super-Earths, which are rocky worlds up to 10 times the mass of Earth.
Unexpectedly, astronomers recently found a strange new class of alien planets — worlds in the Earth- to super-Earth size range whose orbits, which are tightly packed together very near their host stars, range from just 1 to 100 days long. Most of these planets are both far larger and much closer to their stars than Mercury, which is only about two-fifths the diameter of Earth and has an orbit 88 days long.
“Almost 99 percent of the Vulcans are on orbits that are smaller than Mercury’s orbit,” said study co-author Jonathan Tan, an astrophysicist at the University of Florida in Gainesville. “Some are 100 times closer to their star than the Earth is to the sun.”
Scientists have nicknamed these large, hot, rocky worlds “Vulcan planets.” The name does not come from the home world of Spock’s race in “Star Trek,” but from the Roman god of fire, and it was also the name given to a planet that some astronomers had thought might exist inside Mercury’s orbit in our solar system. The temperatures of Vulcans can be as high as about 1,340 degrees Fahrenheit (725 degrees Celsius), “similar to that of molten lava,” Tan said. “Oceans of lava are a distinct possibility.”
These compact systems of Vulcan planets “appear to be very common,” Tan told Space.com. “Perhaps most planets in the galaxy are found in such systems.”
However, explaining how Vulcan worlds could have formed remains a challenge for scientists. Some theorists propose Vulcan planets may have originated farther from their host stars, and each other, than they exist today. They would have then spiraled in to their present orbits, explaining what astronomers see now. However, some details of the spacing between these tightly packed exoplanets do not fit the pattern one would expect if this migration scenario were true.
Another possibility is that Vulcan planets gradually formed where they are now from a disk of so-called planetesimals — rocks the size of asteroids and moons. However, to get Vulcan planets to form this way so near their stars, one would need disks of planetesimals at least 20 times more massive than the disk that gave rise to Earth and the other planets in the solar system — an unlikely scenario, researchers say.
Recently, Tan and his colleague Sourav Chatterjee proposed a theory known as “inside-out planet formation” that may solve the mystery of how Vulcans take shape. It suggests that these worlds originated in the scorching-close orbits they occupy now from a stream of pebbles and small rocks that spiraled inward from more distant parts of their system. These stones accumulate in a ring around their star, and are kept from getting any closer by pressure forces in the inner disk around the star.
“We hypothesize that a planet will eventually form from this ring and will keep growing,” Tan said.
Eventually, this planet grows massive enough to scoop up most of the matter near it, creating a mostly empty gap in the disk of gas and dust around the star. Pebbles and small rocks that continue to spiral inward from more distant parts of the system then form into a ring slightly farther away from the star, and this process of planetary formation begins anew.
“Planets form sequentially, one after another, from inner orbits to outer orbits, hence ‘inside-out,’” Tan said.
In a new study of 629 Vulcan planets, the researchers now find that the greater the distance of these exoplanets from their parent star, the larger their mass. This matches a prediction of inside-out planetary formation.
“I am very excited to see that the observations appear to match the prediction,” Tan said. “This may indicate that we are on the right track in understanding how they formed.”
There are many aspects of this new theory that still need to be worked out in detail, Tan said. “One big question is why don’t all disks form planets in this way — for example, why is our solar system different?”
Chatterjee and Tan detailed their findings online Dec. 29 in the Astrophysical Journal Letters.
For the first time, a litter of four infant star siblings have been seen gestating in the belly of a gas cloud. Researchers say the finding supports the theory that most stars do not begin their lives alone.
In the Perseus star-forming region, four stars are emerging from a single parent filament, and have been observed moving together as a family. Three of the siblings are balls of gas (within the larger gas filament) that researchers say are on the cusp of collapsing into stars, while the fourth sibling has already become a star.
Scientists estimate that more than half of all stars like our sun live with a partner star, and yet scientists have little observational evidence to suggest whether these stars are born together, like twins, or come together later in life. Double-star systems impact many areas of astronomy, including the search for black holes and for habitable exoplanets. The new findings could give scientists a better idea of how multi-star systems emerge.
The newly discovered star babies appear to be less than 100,000 years old, and may be the “youngest multiple star system,” ever observed, according to Kaitlin M. Kratter, an assistant professor astronomy at the University of Arizona, who was not affiliated with the new research.
The new research shows that these four stars are forming from the same gas filament, and are linked together in a single system. But the stars (or soon-to-be-stars) are separated by 3 to 4 thousand astronomical units or AU (the distance from the Earth to the sun), which the authors of the new work say is a very large distance for star binaries. Normally, star twins are separated by only 10 to 1 hundred AU.
“These objects are so far apart that previously we all thought they were unrelated,” said Jaime Pineda, a researcher at the Max Planck Institute of Theoretical physics and lead author on the new research. “But with the new observations, we can measure that these systems are really part of a whole. In this case it’s the first time we can say it’s like a family.”
The researchers used three different telescopes to study the stellar babes. To show that the stars are part of the same family, the researchers had to measure their velocity, and show that they were moving as a unit.
“If you don’t know at what velocity the gas is moving you can’t make this kind of study about the level of bound-ness of the system,” said Pineda, who completed the research at the University of Zurich.
Star sibling rivalry
More than half of the stars in the universe are thought to exist in multi-star systems. It is through observing the motion of binary stars that scientists have identified black holes that have masses close to that of our sun. Binary stars can create Type Ia supernova, which scientists use to measure distances in the universe. Binary star collisions may create gravitational waves, or ripples in the fabric of space-time. Scientists have found potentially habitable planets around binary star suns.
“And yet the origins of the all-too-normal population are mysterious,” said Kratter, in an article in the journal Nature discussing the new research.
Binary systems are highly common, but full-grown quadruple star systems are much rarer.
“Given the relative rarity of quadruple star systems at older ages, one might think this discovery improbable, or lucky,” Kratter said. “On the contrary, it supports predictions that most stars begin their lives in a litter.”
It’s likely that after multi-star systems form, a kind of sibling rivalry sets in: the gravitational pull of all the bodies creates a highly unstable environment. While the researchers cannot say for sure what will happen to the four star siblings, Pineda said it’s likely at least one of them will be ejected later on.
Kratter also notes that young stars have more bound companions than older stars, indicating that while stars may be born in groups, they eventually move away from home, leaving behind a smaller pool of siblings. Some double-star systems may contain stars that were born together, while ejected stars may form binaries somewhere else.
The new result is a tantalizing piece of evidence that could help astronomers understand how star families form. Based on the new finding, Pineda said, researchers may want to re-examine other groups of stars that were previously assumed to be part of separate systems, to see if they are, in fact, part of the same family.
“I think it’s very likely that […] there are regions where we can repeat this experiment and try to determine […] in a more general way if this is a common result,” Pineda said, “Or if we’re looking at an odd ball.”