astronomy

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Astronomers found ultra-hot, Earth-sized exoplanet with a lava hemisphere

astronomy, astrophysics, exoplanets, lava worlds, Physics, Science, Transiting Exoplanet Survey Satellite / /
Like Kepler-10 b, illustrated above, the exoplanet HD 63433 d is a small, rocky planet in a tight orbit of its star.

Enlarge / Like Kepler-10 b, illustrated above, newly discovered exoplanet HD 63433 d is a small, rocky planet in a tight orbit of its star.

NASA/Ames/JPL-Caltech/T. Pyle

Astronomers have discovered an unusual Earth-sized exoplanet they believe has a hemisphere of molten lava, with its other hemisphere tidally locked in perpetual darkness. Co-authors and study leaders Benjamin Capistrant (University of Florida) and Melinda Soares-Furtado (University of Wisconsin-Madison) presented the details yesterday at a meeting of the American Astronomical Society in New Orleans. An associated paper has just been published in The Astronomical Journal. Another paper published today in the journal Astronomy and Astrophysics by a different group described the discovery of a rare small, cold exoplanet with a massive outer companion 100 times the mass of Jupiter.

As previously reported, thanks to the massive trove of exoplanets discovered by the Kepler mission, we now have a good idea of what kinds of planets are out there, where they orbit, and how common the different types are. What we lack is a good sense of what that implies in terms of the conditions on the planets themselves. Kepler can tell us how big a planet is, but it doesn’t know what the planet is made of. And planets in the “habitable zone” around stars could be consistent with anything from a blazing hell to a frozen rock.

The Transiting Exoplanet Survey Satellite (TESS) was launched with the intention of helping us figure out what exoplanets are actually like. TESS is designed to identify planets orbiting bright stars relatively close to Earth, conditions that should allow follow-up observations to figure out their compositions and potentially those of their atmospheres.

Both Kepler and TESS identify planets using what’s called the transit method. This works for systems in which the planets orbit in a plane that takes them between their host star and Earth. As this occurs, the planet blocks a small fraction of the starlight that we see from Earth (or nearby orbits). If these dips in light occur with regularity, they’re diagnostic of something orbiting the star.

This tells us something about the planet. The frequency of the dips in the star’s light tells us how long an orbit takes, which tells us how far the planet is from its host star. That, combined with the host star’s brightness, tells us how much incoming light the planet receives, which will influence its temperature. (The range of distances at which temperatures are consistent with liquid water is called the habitable zone.) And we can use that, along with how much light is being blocked, to figure out how big the planet is.

But to really understand other planets and their potential to support life, we have to understand what they’re made of and what their atmosphere looks like. While TESS doesn’t answer those questions, it’s designed to find planets with other instruments that could answer them.

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Astronomers think they finally know origin of enormous “cosmic smoke rings“

astronomy, astrophysics, galactic winds, Odd Radio Circles, Physics, Science / /

Space oddity —

Massive stars burn out quickly. When they die, they expel their gas as outflowing winds.

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Odd radio circles, like ORC 1 pictured above, are large enough to contain galaxies in their centers and reach hundreds of thousands of light years across.

Enlarge / Odd radio circles are large enough to contain galaxies in their centers and reach hundreds of thousands of light years across.

Jayanne English / University of Manitoba

The discovery of so-called “odd radio circles” several years ago had astronomers scrambling to find an explanation for these enormous regions of radio waves so far-reaching that they have galaxies at their centers. Scientists at the University of California, San Diego, think they have found the answer: outflowing galactic winds from exploding stars in so-called “starburst” galaxies. They described their findings in a new paper published in the journal Nature.

“These galaxies are really interesting,” said Alison Coil of the University of California, San Diego. “They occur when two big galaxies collide. The merger pushes all the gas into a very small region, which causes an intense burst of star formation. Massive stars burn out quickly, and when they die, they expel their gas as outflowing winds.”

As reported previously, the discovery arose from the Evolutionary Map of the Universe (EMU) project, which aims to take a census of radio sources in the sky. Several years ago, Ray Norris, an astronomer at Western Sydney University and CSIRO in Australia, predicted the EMU project would make unexpected discoveries. He dubbed them “WTFs.” Anna Kapinska, an astronomer at the National Radio Astronomy Observatory (NRAO) was browsing through radio astronomy data collected by CSIRO’s Australian Square Kilometer Array Pathfinder (ASKAP) telescope when she noticed several strange shapes that didn’t seem to resemble any known type of object. Following Norris’ nomenclature, she labeled them as possible WTFs. One of those was a picture of a ghostly circle of radio emission, “hanging out in space like a cosmic smoke ring.”

Other team members soon found two more weird round blobs, which they dubbed “odd radio circles” (ORCs). A fourth ORC was identified in archival data from India’s Giant MetreWave Radio Telescope, and a fifth was discovered in fresh ASKAP data in 2021. There are several more objects that might also be ORCs. Based on this, the team estimates there could be as many as 1,000 ORCs in all.

While Norris et al. initially assumed the blobs were just imaging artifacts, data from other radio telescopes confirmed they were a new class of astronomical object. They don’t show up in standard optical telescopes or in infrared and X-ray telescopes—only in the radio spectrum. Astronomers suspect the radio emissions are due to clouds of electrons. But that wouldn’t explain why ORCs don’t show up in other wavelengths. All of the confirmed ORCs thus far have a galaxy at the center, suggesting this might be a relevant factor in how they form. And they are enormous, measuring about a million light-years across, which is larger than our Milky Way.

As for what caused the explosions that led to the formation of ORCs, new data reported in 2022 was sufficient to rule out all but three possibilities. The first is that ORCs are the result of a shockwave from the center of a galaxy, perhaps arising from the merging of two supermassive black holes. Alternatively, they could be the result of radio jets spewing particles from active galactic nuclei. Finally, ORCs may be shells caused by starburst events (“termination shock”), which would produce a spherical shock wave as hot gas blasted out from a galactic center.

A simulation of starburst-driven winds at three different time periods, starting at 181 million years. The top half of each image shows gas temperature, while the lower half shows the radial velocity.

Enlarge / A simulation of starburst-driven winds at three different time periods, starting at 181 million years. The top half of each image shows gas temperature, while the lower half shows the radial velocity.

Cassandra Lochhaas / Space Telescope Science Institute

Coil et al. were intrigued by the discovery of ORCs. They had been studying starburst galaxies, which are noteworthy for their very high rate of star formation, making them appear bright blue. The team thought the later stages of those starburst galaxies might explain the origin of ORCs, but they needed more than radio data to prove it. So the team used the integral field spectrograph at the W.M. Keck Observatory in Hawaii to take a closer look at ORC 4, the first radio circle observable from the Northern Hemisphere. That revealed a much higher amount of bright, heated, compressed gas than one would see in an average galaxy. Additional optical and infrared imaging data revealed that the stars in the ORC 4 galaxy are about 6 billion years old. New star formation seems to have ended some billion years ago.

The next step was to run computer simulations of the odd radio circle itself spanning the course of 750 million years. Those simulations showed an initial 200-million-year period with powerful outflowing galactic winds, followed by a shock wave that propelled very hot gas out of the galaxy to create a radio ring. Meanwhile, a reverse shock wave sent cooler gas back into the central galaxy.

“To make this work, you need a high-mass outflow rate, meaning it’s ejecting a lot of material very quickly. And the surrounding gas just outside the galaxy has to be low density, otherwise the shock stalls. These are the two key factors,” said Coil. “It turns out the galaxies we’ve been studying have these high-mass outflow rates. They’re rare, but they do exist. I really do think this points to ORCs originating from some kind of outflowing galactic winds.” She also thinks that ORCs could help astronomers understand more about galactic outflowing winds since it enables them to “see” those winds through radio data and spectrometry.

Nature, 2024. DOI: 10.1038/s41586-023-06752-8  (About DOIs).

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Seeking another Earth? Look for low carbon dioxide

astronomy, carbon dioxide, exoplanets, habitability, liquid water, Science / /

Where’d all the CO2 go? —

In our own Solar System, Earth has far lower CO2 concentrations than its neighbors.

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Image of a series of planets with different surfaces, arrayed in front of a star.

What do we need to find if we want to discover another Earth? If an exoplanet is too far away for even the most powerful telescopes to search directly for water or certain biosignatures, is there something else that may tell us about the possibility of habitability? The answer could be carbon dioxide.

Led by Amaury Triaud and Julien de Wit, an international team of researchers is now proposing that the absence of CO2 in a planet’s atmosphere potentially increases the chances of liquid water on its surface. Earth’s own atmosphere is depleted of CO2. Unlike dry Mars and Venus, which have high concentrations of CO2 in their atmospheres, oceans on our planet have taken immense amounts of carbon dioxide out of the atmosphere because the gas dissolves in water. CO2 deficits in exoplanet atmospheres might mean the same.

Another molecule could be a sign of a habitable planet: ozone. Many organisms on Earth (especially plants) breathe carbon dioxide and release oxygen. This oxygen reacts with sunlight and becomes O3, or ozone, which is easier to detect than atmospheric oxygen. The presence of ozone and the absence of carbon dioxide could mean a habitable, and even inhabited, planet.

Anyone—or anything—out there?

There is a difference between a planet orbiting within what is considered a habitable zone and actual habitability. Habitability is defined by the researchers as “a planet’s capacity to retain large reservoirs of surface liquid water,” as they state in a study recently published in Nature Astronomy.

Proving that water actually exists could hypothetically be done in many ways. The problem is that most existing telescopes, no matter how advanced, are incapable of pulling them all off. Finding liquid water from light years away is not as easy as seeing the glimmer of a lake, though that is possible at short distances, like those within our own Solar System. (When sunlight reflects off a body of surface liquid, what scientists refer to as a “glint” can be seen, which is how the lakes and oceans on Saturn’s moon Titan were discovered.)

Beyond water, other factors could determine habitability. Besides atmospheric properties, these include (but are not limited to) the orbit of a planet, plate tectonics, magnetic fields, and how it is affected by its star.

When less is more

Triaud, de Wit, and their team argue that it’s worth trying to identify potentially habitable planets that belong to a system similar to ours. If there is a system with several terrestrial planets that are close in size and have atmospheres, this makes it possible to compare carbon dioxide content in their atmospheres and see if there is a significant deficit in one or more planets compared to the others.

While a CO2 deficit does not guarantee that there is liquid water on the surface, it should give scientists a reason to observe the planet or planets in question more closely. We don’t have to look far from Earth to see why this makes sense. Not only has most of the carbon dioxide in our planet’s atmosphere been depleted by its oceans, but plate tectonics also bury it in the crust. The amount of early Earth’s atmospheric carbon dioxide that ended up trapped in rocks is almost equal to the amount of CO2 in the entire atmosphere of Venus.

There is another advantage to searching for this deficit. Because it’s an especially strong infrared light absorber, CO2 is rather easy to detect. Telescopes that are around today, including NASA’s James Webb Telescope and ESO’s Very Large Telescope, as well as ESO’s upcoming Extremely Large Telescope, have infrared vision that can easily search for CO2 signatures.

So what if we did find a planet that showed a deficit of CO2 and the presence of ozone? The researchers think the combination of both could mean not just a few microbial life forms but, at least hypothetically, a planet alive with organisms.

“Life on Earth is planet-shaping,” the team said in the same study. “Planet-shaping life is really what astronomers are after.”

Nature Astronomy, 2023.  DOI:  10.1038/s41550-023-02157-9

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Researchers argue back and forth about whether we’ve spotted an exomoon

astronomy, exomoons, exoplanets, kepler, Kepler telescope, Science / /

That’s no moon! —

Years after Kepler shut down, people are arguing over whether it spotted exomoons.

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Image of two planets orbiting together around a distant star.

In 2017, the astronomy world was abuzz at the announcement that exoplanet Kepler-1625b potentially had its own moon—an exomoon. This was the first hint anyone had seen of an exomoon, and was followed five years later by another candidate around the planet Kepler-1708b.

There are over five thousand exoplanets discovered so far, and we don’t know for certain whether any have moons orbiting, which is what made these announcements so exciting. Exomoons provide more potentially habitable areas in which we can search for extraterrestrial life, and the study of moons can be a valuable window into the formation of the host planet.

But there has been much debate about these exomoon candidates, with multiple groups combing through the data obtained from the Kepler and Hubble space telescopes.

The most recent paper on the topic, published by astronomers in Germany, has come to the conclusion that the exomoon candidates around Kepler-1625b and Kepler-1708b are unlikely. Previous work has also cast doubt on the exomoon candidate around Kepler-1625b.

This is not a clear cut case, though. David Kipping, the leader of the group that made both original discoveries, and assistant professor of astronomy at Columbia University, disagrees with the new analysis. He and his group are in the process of preparing a manuscript that responds to the latest publication.

A needle in a haystack

The most common method of detecting exoplanets is the transit method. This technique measures the brightness of a star, and looks for a small dip in brightness that corresponds to a planet transiting in front of the star.

Stellar photometry can be extended to look for exomoons, an approach pioneered by Kipping. As well as the main dip caused by the planet, if a moon is orbiting the planet you should be able to see an additional, smaller dip   caused by the moon also shielding some of the star’s light.

An example of what a transit detection of an exomoon might look like.

As moons are smaller they generate a smaller signal, making them more challenging to spot. But what makes this particular case even more challenging is that the host stars Kepler-1625 and Kepler-1708 aren’t that bright. This makes the light dip even fainter—in fact these systems   have to have large moons to be within the threshold of what the Kepler space telescope can detect.

Models, models, models

Until scientists get more data from James Webb, or future missions such as ESA’s PLATO launch, it’s all down to what they can do with the existing numbers.

“The aspects here that are relevant are how the data itself is processed, what physics you put in when you’re modelling that data, and then what possible false positive signals might be out there that could reproduce the sort of signal that you’re looking for,” Eamonn Kerins, senior lecturer in astronomy at the University of Manchester who was not involved with the study, told Ars. “I think this whole debate centers around those questions essentially,” he added.

One key phenomenon that needs accurate modelling is known as the stellar limb darkening effect. Stars, including our Sun, appear dimmer at their edge than at the centre due to effects of the stellar atmosphere. As this affects the apparent brightness of the star, it’s clearly important to understand in the context of searching for exomoons by measuring a star’s brightness.

“We have models for this, but we don’t really know exactly how a specific star behaves in terms of this stellar limb darkening effect,” said René Heller, lead author of the study and astrophysicist at the Max Planck Institute for Solar System Research, in an interview for Ars. How specific stars behave can be deduced, but this isn’t always trivial. By including improved models for stellar limb darkening, the authors found that they can explain signals previously attributed to an exomoon.

Data processing is also paramount, especially a type of processing known as detrending. This takes into account long-term variability in the brightness data that is caused by random stellar variation and instrument variability, among other things. The new research shows that the statistical outcome, moon or no moon, is extremely dependent on how you carry out this detrending.

What’s more, the authors say that the data obtained from the Hubble telescope, which is primarily where the claim for the moon around Kepler-1625b comes from, can’t be properly detrended and thus shouldn’t be relied on for exomoon searches.

Two sides

Until more data is obtained, this is likely to remain an ongoing scientific discussion with no definitive conclusion.

Kerins points out that Kipping and his team have been very measured in their announcements. “They’re very, very careful to not claim it as a cast-iron detection. They’ve done comprehensive testing of the data they’ve been given, and really I think the difference here is all about what physics you put in, how you process the data, and ultimately the fact that the Kepler data set is really on the edge of finding exomoons.”

Heller, though, remains unconvinced. “My impression is that in the Kepler data, we and also other teams have done what’s currently possible and there’s no compelling object that really sticks out.”

Moons far outnumber planets in our own Solar System—two hundred and ninety to eight to date—so it’s reasonable to assume that we will come across exomoons as we continue exploring the skies. “It would be quite extraordinary, I think, if we continue to go over the next few years and not find an exomoon,” said Kerins. “I think it can only be a matter of time.”

Nature Astronomy, 2023.  DOI: 10.1038/s41550-023-02148-w

Ivan Paul is a freelance writer based in the UK, finishing his PhD in cancer research. He is on Twitter @ivan_paul_.

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Galaxy-scale winds spotted in the distant Universe

astronomy, astrophysics, cosmology, Science, Space / /

Out in the wind —

These winds can drive gas out of galaxies, shaping their future evolution.

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Image of a galaxy with a purple blob superimposed on its center.

Enlarge / X-ray emissions (purple) superimposed on a visible light image of a galaxy shows the galaxy winds being launched. CREDIT: X-ray: NASA/CXC/Ohio StateH-alpha and Optical: NSF/NOIRLab/AURA/KPNO/CTIO; Infrared: NASA/JPL-Caltech/Spitzer/ Optical: ESO/La Silla Observatory.

One of the ways massive stars, those at least 10-times bigger than the Sun, reach their end is in a supernova—an enormous explosion caused by the star’s core running out of fuel.

One consequence of a supernova is the production of galactic winds, which play a key role in regulating star formation. Although galactic winds have already been observed in several nearby galaxies, a team of scientists has now made the first direct observations of this phenomenon in a large population of galaxies in the distant Universe, at a time when galaxies are in their early stages of formation.

Feedback

According to the study’s lead author, Yucheng Guo, of the Centre de Recherche Astrophysique de Lyon, galactic winds are an important part of the galaxy evolution models.

“It was assumed there should be galactic winds that can regulate galaxies’ growth. However, it was very difficult to directly observe these winds. With our study, we show that at the early stage of the Universe, every normal galaxy had such winds,” Guo said.

According to Guo, galactic winds form a key part of the so-called feedback process that is important in our understanding of galaxy evolution. “Galactic winds originate as a result of star formation activity. These winds inject a lot of energy and momentum into the gas, resulting in it [being] expelled from the galaxy. If there is not enough gas in the galaxy, the star formation stops. This is called the feedback process,” he said.

According to Guo, galactic winds also enable exchange of matter between galaxies and their surroundings. “Each galaxy is surrounded by a gas halo. Galaxies can breathe out as well as breathe in gas,” Guo said.

Hard to see

He said that traditionally it has been very difficult to observe galactic winds, because the gas halos are almost transparent.

Guo and his team overcame this hurdle by using the Multi-Unit Spectroscopic Explorer (MUSE) instrument on the Very Large Telescope. “The instrument is able to observe the galaxies at redshift z ≈ 1, which corresponds to 7 billion years of the cosmic evolution.” Guo said at that wavelength, the MUSE instrument is able to detect and directly observe the emission from magnesium atoms in the galactic winds.

He said the other important feature of the research is that they managed to observe the galactic winds in more than 100 galaxies. “We also managed to detect the average shape of these winds, which is like an ice cream cone,” he said.

Guo said the direct observation of the galactic winds outside the local Universe was the first step of their research. “We still don’t know about their physical properties such as size, power, and also how they change with time and in different kinds of galaxies.”

Nature, 2023. DOI: 10.1038/s41586-023-06718-w


Dhananjay Khadilkar is a journalist based in Paris.

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