A star's early chemistry shapes life-friendly atmospheres

Apr 23, 2014 by Elizabeth Howell
Artist's conception of a protoplanetary disc. Credit: University of Copenhagen/Lars Buchhave

Born in a disc of gas and rubble, planets eventually come together as larger and larger pieces of dust and rock stick together. They may be hundreds of light-years away from us, but astronomers can nevertheless watch these planets as they form.

One major point of interest is the chemistry of the rubble that forms around a star before a planetary system is formed, known as the protoplanetary disc.

The that float in the disc could eventually become part of the atmosphere of the planets. If these molecules contain oxygen or nitrogen, the odds increase of a life-friendly planet forming.

"It's very interesting to think about the molecular composition (of these discs)," said Catherine Walsh, an astronomer at Leiden Observatory in the Netherlands. "The molecules that are in those discs will make up the molecules in planetary atmospheres, and planetesimals such as comets."

Walsh led a new study, "Complex organic molecules in protoplanetary disks," which was published in February 2014 in the journal Astronomy and Astrophysics. In the study, the astronomers modeled how form in protoplanetary systems with the hopes of better understanding their observations.

Seeking high definition observations

Molecules in protoplanetary discs emit their light in the millimeter and sub-millimeter frequencies of light, which are between the observation ranges of radio telescopes and infrared telescopes. Until recently, however, there have been few observatories devoted to this particular band of light with the necessary capabilities to see complex molecules.

"There has been a lot of work done to date, mainly with single-dish submillimeter telescopes," Walsh said.

While any observation is helpful, the single dish meant that astronomers could not get the high spatial resolution and sensitivity that they need to see more complex molecules. This changed in 2013, however, when the Atacama Large Millimeter Array (ALMA) in Chile lighted up for the first time.

The observatory—described as the largest astronomical project that exists right now—will eventually include 66 antennas located at 5,000 meters altitude, which puts it above much of the section of the atmosphere that blocks millimeter light from arriving at the surface.

"This is really the next big thing in molecular astrophysics, and ALMA will give us orders of magnitude (of improvement) in sensitivity," Walsh said.

Although her team has submitted a proposal to examine molecules using the giant array, the popularity of the telescope (which brings many competing proposals) means she is not sure if they will succeed.

One aim of examining protoplanetary discs is to understand how complex molecules formed and changed during their evolution. Credit: NASA/FUSE/Lynette Cook

If they do manage to get a slot of time, the astronomers will have to work quickly to publish their results.

"One great benefit is all of the ALMA data will be publicly available after one year. We will end up having this huge archive. Anyone can access the data and publish science with that data," Walsh said.

Where to look first?

Complex molecules are considered "precursors" of prebiotic chemistry, or the chemistry that gives rise to the conditions needed for life.

A famous example of prebiotic chemistry took place in 1952, when scientists Stanley Miller and Harold C. Urey put the gas forms of methane, hydrogen, ammonia and water vapor into a sealed container, then struck the gas with electricity (an analog of lightning). After doing this for a week, the walls of the container contained an organic sludge that included several of the amino acids that life uses today.

The question, Walsh said, is which complex molecules are present in protoplanetary discs, and would ALMA be able to see them? Complex molecules are not only potential precursors of life, but the ices in which they are thought to form also acts as a coagulant for dust grains to stick together and form planets.

Her team's paper modeled the environment around T Tauri type stars, the phase that a young star goes through before turning into a star like our own Sun. Unlike stars that are older, the light that is emitted from these objects comes from gravitational contractions as the star draws material in from the surrounding disc.

Walsh's team used calculations to generate a model of the disc, focusing on the temperature, density, structure and the strength of ultraviolet light. They then used this model to compute the chemistry. With this information in hand, they ran another set of calculations to predict what ALMA would be able to see.

Molecules are visible from afar because their rotation produces distinctive spectra, or line emissions that can be seen from Earth. The model predicted formaldehyde, a molecule with four atoms in it, which was a good thing because the results confirmed what has been detected in previous observations of protoplanetary discs. However, astronomers would like to find a more complex molecule like methanol, a derivative of methane, which on Earth is naturally produced by bacteria. In space, methanol is formed slightly differently: it is a derivative of carbon monoxide.

Methanol hasn't been seen yet in protoplanetary discs. The more complex a molecule is, the less bright its spectrum appears in telescopes, making it harder to spot. Yet, Walsh said she's nevertheless sure that the ALMA telescope would be up to the task of spotting methanol, a "first rung on the ladder of complexity," and that could lead to the discovery of even more complex molecules, containing both oxygen and nitrogen.

The Atacama Large Millimeter/submillimeter Array (ALMA) in Chile is designed to search for astronomical phenomena such as complex molecules in protoplanetary discs. Credit: ALMA (ESO/NAOJ/NRAO)/B. Tafreshi (twanight.org)

If methanol is spotted, a next step would be to see where it occurs and study how it forms. In all likelihood, the molecule would form on the surface of dust grains because complex molecules are thought to have inefficient gas-phase routes to formation because of the low gas densities in space.

The next research step is to find glycine—the simplest amino acid and a building block for proteins—in protoplanetary discs. Walsh characterized glycine as "the holy grail" of research, and noted its "prebiotic significance" as one of the building blocks of life. But could ALMA detect glycine?

"I like to err on the cautious side," she said. "It's possibly beyond the capabilities of the telescope."

But then again, it's hard to predict what sort of technology will be available in the future, she added.

One possibility is the Square Kilometer Array, a set of radio telescopes under construction in both Australia and South Africa, so named because the collecting area would be about a square kilometer (0.4 miles) in size. Construction of the telescope is scheduled to begin in 2018 and be finished by the mid-2020s.

The array will pick up a set of complex molecules with longer wavelengths and lower frequencies than ALMA.

"It's possible we can see more prebiotic molecules with something like the Square Kilometer Array," she added.

Learning more about these complex molecules will also teach us about the ingredients which are available during the planet formation process, which will help astronomers understand how the molecular composition of the Earth, and the other Solar System planets, came to be, Walsh said.

"We've now seen thousands of exoplanets and we know that planet formation is ubiquitous," she said. "We now know there are many more planets in the universe than stars, and there are a lot of stars (to research). There is so much to be done in (researching) this (protoplanetary) phase."

Explore further: Research group to study interstellar molecules

More information: "Complex organic molecules in protoplanetary disks." Catherine Walsh, Tom. J. Millar, Hideko Nomura, Eric Herbst, Susanna Widicus Weaver, Yuri Aikawa, Jacob C. Laas and Anton I. Vasyunin. A&A 563 A33 (2014). DOI: dx.doi.org/10.1051/0004-6361/201322446

add to favorites email to friend print save as pdf

Related Stories

Building blocks of life found around young star

Aug 29, 2012

(Phys.org)—A team of astronomers using the Atacama Large Millimeter/submillimeter Array (ALMA) has spotted sugar molecules in the gas surrounding a young Sun-like star. This is the first time sugar been ...

Research group to study interstellar molecules

Apr 11, 2014

From April 2014, a new group will study interstellar molecules and use them to explore the entire star and planet formation process at the Max Planck Institute for Extraterrestrial Physics. Newly appointed ...

Astronomers suggest more accurate star formation rates

Apr 10, 2014

(Phys.org) —Astronomers have found a new way of predicting the rate at which a molecular cloud—a stellar nursery—will form new stars. Using a novel technique to reconstruct a cloud's 3-D structure, ...

'Death stars' in Orion blast planets before they even form

Mar 10, 2014

(Phys.org) —The Orion Nebula is home to hundreds of young stars and even younger protostars known as proplyds. Many of these nascent systems will go on to develop planets, while others will have their planet-forming ...

Astronomers looking for clues to water's origins

Mar 27, 2014

A gas and dust cloud collapses to form a star. Amid a whirling disc of debris, little bits of rock coated with liquid water and ice begin to stick together. It is this stage of a star's formation that astronomers ...

Recommended for you

A colorful gathering of middle-aged stars

15 hours ago

NGC 3532 is a bright open cluster located some 1300 light-years away in the constellation of Carina(The Keel of the ship Argo). It is informally known as the Wishing Well Cluster, as it resembles scattered ...

User comments : 5

Adjust slider to filter visible comments by rank

Display comments: newest first

Z99
not rated yet Apr 23, 2014
1. Formaldehyde: HC(=O)H; Methane CH4; Carbon monoxide C=O; Methanol H3COH. All the above have one carbon IOW, any of the above can be precursors of the rest.
2. it is not complexity that determines brightness of any single molecule, rather each bond is mostly 'alone' in emitting/absorbing a particular intensity of light. C=O is particularily intense, C-H not so much. It is true that the more complex the molecule is, the LESS of will be emitting light and the harder they will be to see.
3. the 1952 experiment used conditions (what was thought at the time to be the composition of the atmosphere of early Earth) which are no longer accepted as being realistic.
4. it is is misleading to claim glycine is a "building block" of life. That is like claiming a electronic ignition is a building block for a car. Sure, cars now days have them but they didn't for most of their 'evolution'. Same with proteins: we don't know what composed the primadorial 'stuff of life'.
mark_mnarkwynne
1 / 5 (2) Apr 24, 2014
Life imho was created by solar output delivering the ingredients to the earth and electrical activity, possibly in stages, amino acids and then further stages of evolution driven by electrical activity. Energy is what bonds everything together so it wouldn't be a complete shock to discover massive primordial electrical discharge phenomenon repeatedly interacted with the evolution of life on Earth.

Electrical discharges into a molecule rich environment may have created life in several places on earth in parallel and those all followed similar evolution paths, I am not of that all life came from one pool as it were but rather, given the same ingredients and catalyst were present globally then it is not a giant leap to assume life sprung up from multiple places simultaneously.
Part of this evolution could possibly be storms of unstable charged particles bombarding the planet and combining en route. Just has hydrogen hits the atmosphere and a % of it combines with oxygen to make water.
Torbjorn_Larsson_OM
not rated yet Apr 24, 2014
Note that characterizing disk chemistries are thought to more illuminate planet- and atmosphere-formation rather than life as such.

@Z99: The Miller experiment was an illustration, not a discussion of actual pathways. These pathways are not seen as quite as unrealistical today as when the neutral, less productive CO2-dominated atmospheres were found to be more compatible with geology in the early 00's. For one thing, local environments (around vents and volcanoes) were still reductive and productive, for another the state of the primordial atmosphere and the geological record is now thought to allow more hydrogen and methane.

But mostly, soup theories such as Millers have been taking more of the backstage as compared to vent theories.
Torbjorn_Larsson_OM
not rated yet Apr 24, 2014
@mark: Phylogeny predicts that early energy sources were electrochemical if not "electrical". E.g. we share the pH differential and the import part of chemiosmosis with geochemistry of Hadean alkaline vents, and possibly the electron chains across membranes too. Those two pathways for free energy use were in turn driven by nitrite/nitrate superoxidants in the UCA metabolic chain, which were mostly sourced by lightning from volcanoes and thunderstorms to high enough steady state concentrations in the Hadean CO2/N2 atmosphere, so "electrical". [Russell et al, sundry papers.]
FineStructureConstant
not rated yet Apr 26, 2014
a square kilometer (0.4 miles) in size
(roughly) 0.4 SQUARE miles in size...

Please sign in to add a comment. Registration is free, and takes less than a minute. Read more

Click here to reset your password.
Sign in to get notified via email when new comments are made.