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Cepheus B: Trigger-Happy Star Formation
Cepheus B
Cepheus B
Visual Description:

  • Cepheus B is a cloud of molecular hydrogen, a place where stars are known to form

  • Researchers used Chandra and Spitzer to study this cloud, which is relatively close at 2,400 light years away

  • The combined data reveal that massive stars may trigger star formation more often than previously thought

This composite image, combining data from the Chandra X-ray Observatory and the Spitzer Space Telescope shows the molecular cloud Cepheus B, located in our Galaxy about 2,400 light years from the Earth. A molecular cloud is a region containing cool interstellar gas and dust left over from the formation of the galaxy and mostly contains molecular hydrogen. The Spitzer data, in red, green and blue shows the molecular cloud (in the bottom part of the image) plus young stars in and around Cepheus B, and the Chandra data in violet shows the young stars in the field.

The Chandra observations allowed the astronomers to pick out young stars within and near Cepheus B, identified by their strong X-ray emission. The Spitzer data showed whether the young stars have a so-called "protoplanetary" disk around them. Such disks only exist in very young systems where planets are still forming, so their presence is an indication of the age of a star system.

These data provide an excellent opportunity to test a model for how stars form. The new study suggests that star formation in Cepheus B is mainly triggered by radiation from one bright, massive star (HD 217086) outside the molecular cloud. According to the particular model of triggered star formation that was tested -- called the radiation-driven implosion (RDI) model -- radiation from this massive star drives a compression wave into the cloud triggering star formation in the interior, while evaporating the cloud's outer layers.

The labeled version of the image (rollover the image above) shows important regions in and around Cepheus B. The "inner layer" shows the Cepheus B region itself, where the stars are mostly about one million years old and about 70-80% of them have protoplanetary disks. The "intermediate layer" shows the area immediately next to Cepheus B, where the stars are two to three million years old and about 60% of them have disks, while in the "outer layer" the stars are about three to five million years old and about 30% of them have disks. This increase in age as the stars are further away from Cepheus B is exactly what is predicted from the RDI model of triggered star formation.

Different types of triggered star formation have been observed in other environments. For example, the formation of our solar system was thought to have been triggered by a supernova explosion, In the star-forming region W5, a "collect-and-collapse" mechanism is thought to apply, where shock fronts generated by massive stars sweep up material as they progress outwards. Eventually the accumulated gas becomes dense enough to collapse and form hundreds of stars. The RDI mechanism is also thought to be responsible for the formation of dozens of stars in W5. The main cause of star formation that does not involve triggering is where a cloud of gas cools, gravity gets the upper hand, and the cloud falls in on itself.

Visual Description:

The composite image of the molecular cloud Cepheus B features a dark, starry sky with a dramatic pinkish-reddish gas cloud reaching up from the bottom of the image to the center, like a jagged mountain reaching for the sky. The gas cloud is almost shaped like a pyramid, with its tip pointing towards the top. The texture of the gas cloud resembles a fluffy, cotton-candy-like substance, and there are speckles of bright purple and green in the “sky” area up top. This composite image combines data from the Chandra X-ray Observatory (purple dots) and the Spitzer Space Telescope (red gas and green dots) shows a region containing cool interstellar gas and dust. The gas and dust are left over from the formation of the galaxy and mostly contain molecular hydrogen. The Spitzer data outline the molecular cloud (in the bottom part of the image) plus young stars in and around Cepheus B, and the Chandra data in purple shows the young stars in the field.

 

Fast Facts for Cepheus B:
Credit  X-ray (NASA/CXC/PSU/K. Getman et al.); IR (NASA/JPL-Caltech/CfA/J. Wang et al.)
Release Date  August 12, 2009
Scale  Image is 15 arcmin across
Category  Normal Stars & Star Clusters, White Dwarfs & Planetary Nebulas
Coordinates (J2000)  RA 22h 56m 46.99s | Dec +62° 40' 0.0012"
Constellation  Cepheus
Observation Date  03/11/2003
Observation Time  8 hours
Obs. ID  3502
Instrument  ACIS
References Getman, K.V., et al. (2009), ApJ, 699, 1454
Color Code  X-ray (Violet); IR (Red, Green, Blue)
IR
X-ray
Distance Estimate  About 2400 light years
distance arrow
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