Infrared Dark Clouds Reveal Why Some Stars are Bigger than Others

Infrared Dark Clouds Reveal Why Some Stars are Bigger than Others

This image shows the ALMA data overlaid on an artist’s impression background. The ALMA data show two main cores as imaged by emission from the molecular ion N2D+ (two nitrogen and one deuterium atom). The core on the right is particularly bright and rounded, suggesting it is self-gravitating and poised to form a massive, single star – a very rare occurrence in star formation. The other core appears more distorted and fragmented, potentially leading to the formation of multiple lower-mass stars. This fragmentation is a normal process in star-forming clouds. Credit: Bill Saxton & Alexandra Angelich (NRAO/AUI/NSF); ALMA (ESO/NAOJ/NRAO)

Using the Atacama Large Millimeter/submillimeter Array telescope, astronomers surveyed the cores of some of the darkest, coldest, and densest clouds in our Galaxy to find out why some stars are bigger than others.

Massive stars – those at least 8 times the mass of our Sun – present an intriguing mystery: how do they grow so large when the vast majority of stars in the Milky Way are considerably smaller?

To find the answer, astronomers used the Atacama Large Millimeter/submillimeter Array (ALMA) telescope to survey the cores of some of the darkest, coldest, and densest clouds in our Galaxy to search for the telltale signs of star formation.

These objects, known as Infrared Dark Clouds, were observed approximately 10,000 light-years away in the direction of the constellations of Aquila and Scutum.

Since these cloud cores are so massive and dense, gravity should have already overwhelmed their supporting gas pressure, allowing them to collapse to form new, Sun-mass stars. If a star had not yet begun to shine, that would be a hint that something extra was supporting the cloud.

An animation showing two main cores as imaged by emission from the molecule N2D+ (two nitrogen and one deuterium atom). Both cores are on the verge of star formation, but one is being fragmented, indicating it will form a number of Sun-mass stars. The larger, more rounded core presents the rare qualities necessary to form a single, massive star. Credit: Brian Kent (NRAO/AUI/NSF); ALMA (ESO/NAOJ/NRAO)

“A starless core would indicate that some force was balancing out the pull of gravity, regulating star formation, and allowing vast amounts of material to accumulate in a scaled-up version of the way our own Sun formed,” remarked Jonathan Tan, an astrophysicist at the University of Florida, Gainesville, and lead author of a paper published today in the Astrophysical Journal. “This suggests that massive stars and Sun-like stars follow a universal mechanism for star formation. The only difference is the size of their parent clouds.”

Average stars like our Sun begin life as dense, but relatively low-mass concentrations of hydrogen, helium, and other trace elements inside large molecular clouds. After the initial kernel emerges from the surrounding gas, material collapses under gravity into the central region in a relatively ordered fashion via a swirling accretion disk, where eventually planets can form. After enough mass accumulates, nuclear fusion begins at the core and a star is born.

While this model of star formation can account for the vast majority of stars in our Milky Way, something extra is needed to explain the formation of more massive stars. “Some additional force is needed to balance out the normal process of collapse, otherwise our Galaxy would have a fairly uniform stellar population,” said Tan. “Alternatively, there has been speculation that two separate models of star formation are needed: one for Sun-like stars and one for these massive stars.”

The key to teasing out the answer is to find examples of massive starless cores – to witness the very beginnings of massive star birth.

The team of astronomers from the United States, the United Kingdom, and Italy used ALMA to look inside these cores for a unique chemical signature involving the isotope deuterium to essentially take the temperatures of these clouds to see if stars had formed. Deuterium is important because it tends to bond with certain molecules in cold conditions. Once stars turn on and heat the surrounding gas, the deuterium is quickly lost and replaced with the more common isotope of hydrogen.

The ALMA observations detected copious amounts of deuterium, suggesting that the cloud is cold and starless. This would indicate that some counter force is forestalling core collapse and buying enough time to form a massive star. The researchers speculate that strong magnetic fields may be propping up the cloud, preventing it from collapsing quickly.

“These new ALMA observations reveal objects that are quite similar to the nurseries of Sun-like stars, but simply scaled-up by tens or a hundred times. This may mean that nature is more important than nurture when it comes to determining a star’s size,” concludes Tan.

These observations were conducted during ALMA’s early science campaign. Future studies with ALMA’s full array of 66 antennas will uncover even more details about these star-forming regions.

ALMA, an international astronomy facility, is a partnership of Europe, North America, and East Asia in cooperation with the Republic of Chile. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning, and operation of ALMA.

The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.

Reference: “THE DYNAMICS OF MASSIVE STARLESS CORES WITH ALMA” by Jonathan C. Tan, Shuo Kong, Michael J. Butler, Paola Caselli and Francesco Fontani, 26 November 2013, The Astrophysical Journal.
DOI: 10.1088/0004-637X/779/2/96

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