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RCW 36: Astronomers See Stellar Self-Control in Action

  • A new study shows how some stars can demonstrate “self-control” when forming in groups.

  • By expelling most of the gas from the system, the biggest and brightest stars limit new star formation.

  • This result gives astronomers a better idea of what controls the numbers of stars forming in clusters.

  • Researchers used NASA’s Chandra X-ray Observatory, SOFIA, ESA’s Herschel and the APEX telescope for this result.

Many factors can limit the size of a group, including external ones that members have no control over. Astronomers have found that groups of stars in certain environments, however, can regulate themselves.

A new study has revealed stars in a cluster having “self-control,” meaning that they allow only a limited number of stars to grow before the biggest and brightest members expel most of the gas from the system. This process should drastically slow down the birth of new stars, which would better align with astronomers’ predictions for how quickly stars form in clusters.

This study combines data from several telescopes including NASA's Chandra X-ray Observatory, NASA's now-retired Stratospheric Observatory for Infrared Astronomy (SOFIA), the APEX (the Atacama Pathfinder EXperiment) telescope, and ESA’s (European Space Agency’s) retired Herschel telescope.

The target of the observations was RCW 36, a large cloud of gas called an HII (pronounced "H-two") region mainly composed of hydrogen atoms that have been ionized — that is, stripped of their electrons. This star-forming complex is located in the Milky Way about 2,900 light-years from Earth. Infrared data from Herschel is shown in red, orange, and green, and X-ray data is blue, with point sources in white. North is 32 degrees left of vertical.

RCW 36 contains a cluster of young stars and two cavities — or voids — carved out of the ionized hydrogen gas, extending in opposite directions. There is also a ring of gas that wraps around the cluster in between the cavities, forming a waist around the hourglass-shaped cavities. These features are labeled in the image.

Labeled, X-ray and Infrared Image of RCW 36
Labeled, X-ray and Infrared Image of RCW 36 (Credit: X-ray: NASA/CXC/Ames Research Center/L. Bonne et al.; Infrared: ESA/NASA.JPL-Caltech/Herschel Space Observatory/JPL/IPAC)

Hot gas with a temperature of about two million kelvins (3.6 million degrees Fahrenheit), radiating in X-rays detected by Chandra, is concentrated near the center of RCW 36, close to the two hottest and most massive stars in the cluster. These stars are a major source of the hot gas. A large amount of the rest of the hot gas is outside the cavities, after having leaked through the borders of the cavities. The SOFIA and APEX data shows that the ring contains cool, dense gas (with typical temperatures of 15 to 25 kelvins, or about -430 to -410 degrees Fahrenheit) and is expanding at 2,000 to 4,000 miles per hour.

The SOFIA data show that on the perimeter of both cavities are shells of cool gas expanding at about 10,000 miles per hour, likely being driven outward by pressure from the hot gas observed with Chandra. The hot gas, plus radiation from stars in the cluster, has also cleared even larger cavities around RCW 36, forming a Russian doll structure. These features are labeled in a Herschel image covering a larger area, which also shows the Chandra field-of-view and the other structures described here. The intensity levels in this image have been adjusted to show the larger cavities as clearly as possible, causing much of the inner regions near the RCW 36 cavities to be saturated. North is vertical in this image.

Labeled wide-field image from Herschel Space Observatory in infrared
Wide Field, Labeled, Infrared Image of RCW 36 (Credit: NASA/JPL-Caltech, Herschel Space Observatory)

The researchers also see evidence from the SOFIA data for some cool gas around the ring being ejected from RCW 36 at even higher speeds of about 30,000 miles per hour, with the equivalent of 170 Earth masses per year being pushed out.

The expansion speeds of the different structures described here, and the mass ejection rate, show that most of the cool gas within about three light-years of the center of the HII region can be ejected in 1 million to 2 million years. This will clear out the raw material needed to form stars, suppressing their continued birth in the region. Astronomers call this process where stars can regulate themselves “stellar feedback.” Results such as this help us understand the role stellar feedback plays in the star formation process.

A paper describing these results appeared in the Aug. 20 issue of The Astrophysical Journal and is available online. The authors are Lars Bonne (NASA Ames Research Center), Nicola Schneider (University of Cologne, Germany), Pablo Garcia (Chinese Academy of Sciences), Akanksha Bij (Queen’s University, Canada), Patrick Broos (Penn State), Laura Fissel (Queen’s University) , Rolf Guesten (Max Planck Institute for Radio Astronomy, Germany), James Jackson (NASA Ames), Robert Simon (University of Cologne), Leisa Townsley (Penn State), Annie Zavagno (Aix Marseille University, France), Rebeca Aladro (Max Planck Institute for Radio Astronomy), Christof Buchbender (University of Cologne), Cristian Guevara (University of Cologne), Ronan Higgins (University of Cologne), Arshia Maria Jacob (Max Planck Institute for Radio Astronomy), Slawa Kabanovic (University of Cologne), Ramsey Karim (University of Maryland), Archana Soam (NASA Ames), Jurgen Stutzki (University of Cologne), Maitraiyee Tiwari (University of Maryland), Freidrich Wyrowski (Max Planck Institute for Radio Astronomy), and Alexander Tielens (University of Maryland).

NASA's Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory's Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.

SOFIA was a Boeing 747SP aircraft modified to carry a reflecting telescope. The observatory was a joint project of NASA and the German Space Agency at DLR.

 

Fast Facts for RCW 36:
Credit  X-ray: NASA/CXC/Ames Research Center/L. Bonne et al.; Infrared: ESA/NASA.JPL-Caltech/Herschel Space Observatory/JPL/IPAC
Release Date  November 29, 2022
Scale  Image is about 17 arcmin (14 light-years) across. North is 32° to the left of vertical.
Category  Normal Stars & Star Clusters
Coordinates (J2000)  RA 08h 59m 00.9s | Dec -43° 44´ 10"
Constellation  Vela
Observation Date  September 23, 2006
Observation Time  19 hours 33 minutes
Obs. ID  6433
Instrument  ACIS
References Bonne, L., et al., 2022, ApJ, 935, 171; arXiv:2207.06479
Color Code  X-ray: blue with white stars; Infrared: red (250 nm), orange (160 nm), green (70 nm)
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X-ray
Distance Estimate  About 2,900 light-years
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