| Nebula | |
|---|---|
 Young stars in RCW 36 are revealed in the X-ray (blue), while infrared images (red and green) show both stars and gas. | |
| Observation data:J2000epoch | |
| Right ascension | 08h 59m 00.9s[1] |
| Declination | −43° 44′ 10″[1] |
| Distance | 2300[2] ly (700 pc) |
| Apparent dimensions (V) | 5arcmin |
| Constellation | Vela |
| Designations | RCW 36, Gum 20, BBW 217[3][1] |
| See also:Lists of nebulae | |
RCW 36 (also designatedGum 20)[4] is anemission nebula containing anopen cluster in the constellationVela. ThisH II region is part of a larger-scalestar-forming complex known as theVela Molecular Ridge (VMR), a collection ofmolecular clouds in theMilky Way that contain multiple sites of ongoing star-formation activity.[3] The VMR is made up of several distinct clouds, and RCW 36 is embedded in the VMR Cloud C.
RCW 36 is one of the sites of massive-star formation closest to the Solar System,[5] whose distance of approximately 700parsecs (2300light-years). The most massive stars in the star cluster are two stars withlate-O orearly-B spectral types, but the cluster also contains hundreds of lower-mass stars.[6] This region is also home to objects withHerbig–Haro jets, HH 1042 and HH 1043.[7] It is about 1.1million years old.[6]
Like most star-forming regions, theinterstellar medium around RCW 36 contains both the gas from which stars form and some newly formed young stars.[3] Here, young stellar clusters form ingiant molecular clouds.[8] Molecular clouds are the coldest, densest form of interstellar gas and are composed mostly ofmolecular hydrogen (H2), but also include morecomplex molecules,cosmic dust, and atomic helium. Stars form when the mass gas in part of a cloud becomes too great, causing it to collapse due to theJeans instability.[9] Most stars do not form alone, but in groups containing hundreds or thousands of other stars.[10] RCW 36 is an example of this type of "clustered" star formation.[2]
The Vela Molecular Ridge can be subdivided into several smaller clouds, each of which in turn can be subdivided into cloud "clumps". The molecular cloud clump from which the RCW 36 stars are forming is Clump 6 in the VMR C cloud.[11]
Early maps of the region were produced byradio telescopes that traced emission from several types of molecules found in the clouds, includingCO,OH, andH2CO.[12][13] More detailed CO maps were produced in the 1990s by a team of Japanese astronomers using theNANTEN millimeter-wavelength telescope. Using emission from C18O, they estimated the total mass of Cloud C to be 44,000M☉.[11] The cloud maps suggest that Cloud C is the youngest component of the VMR because of an ultra-compact H II region associated with RCW 36 and several sites of embedded protostars, while H II regions in other VMR clouds are more evolved.[3] Observations from theHerschel Space Telescope show that the material within the cloud is organized into filaments and RCW 36 sits near the south end of a 10-parsec long filament.[14][15][16][17]
Star formation in RCW 36 is currently ongoing. In the dense gas at the western edge of RCW 36, where the far-infrared emission is greatest, are found protostellar cores, the Herbig Haro objects, and an ultra-compact H II region. However, more deeply embedded star-formation is obscured by dust, so radiation can only escape from the cloud surface and not from the embedded objects themselves.[6]
The H II region is an area around the cluster in which hydrogen atoms in theinterstellar medium have been ionized by ultraviolet light from O- and B-type stars. The H II region in RCW 36 has an hourglass morphology,[14] similar to the shape of H II regions around other young stellar clusters likeW40 orSh2-106. In addition, an ultra-compact H II region surrounds IRAS source 08576−4333.[18]
Due to the youth of RCW 36, most of the stars in the cluster are at an early stage ofstellar evolution where they are known asyoung stellar objects orpre-main-sequence stars. These stars are still in the process of contraction before they reach themain sequence, and they may still have gasaccreting onto them from either acircumstellar disk orenvelope.
Cluster members in RCW 36 have been identified through both infrared and X-ray observations. Bright infrared sources, attributed to massive stars, were first identified by the TIFR 100-cm balloon-born telescope from theNational Balloon Facility in Hyderabad, India.[19] In the early 2000s, infrared images in theJ, H, and Ks bands have suggested at least 350 cluster members.[2] Observations byNASA'sSpitzer Space Telescope andChandra X-ray Observatory were used to identify cluster members as part of the MYStIX survey of nearby star-forming regions.[5] In the MYStIX catalog of 384 probable young stellar members of RCW 36, more than 300 of the stars are detected by X-ray sources.[20] Modeling of the brightnesses of stars at various infrared wavelengths has shown 132young stellar objects to have infrared excess consistent withcircumstellar disks or envelopes.[21]
The cluster has been noted by Baba et al. for having a high density of stars, withstar counts (the number of stars within an angular area of the sky) exceeding 3000 stars per square parsec at the center of the cluster.[2] A measurement of centralarea density using the MYStIX catalog suggested approximately 10,000 stars per square parsec at the cluster center, but this study also suggested that such densities are not unusual for massive star-forming regions.[22] The spatial distribution of stars has been described as a King profile[2] or alternatively as a "core-halo" structure.[23]
Stellardensity near the center of RCW 36 has been estimated to be approximately 300,000 stars per cubic parsec (or 10,000 stars per cubic light year).[24] In contrast, thedensity of stars in the Solar neighborhood is only 0.14 star per cubic parsec,[25][26] so the density of stars at the center of RCW 36 is about 2 million times greater. It has been calculated that for young stellar clusters with more than 104 stars pc.−3 close encounters between stars can lead to interactions between protoplanetary disks that affect developing planetary systems.[27]
Several special types of young stellar object have been identified in RCW 36, and are described in more detail below. The properties of these stars are related to their extreme youth.
Two stars in RCW 36 have Herbig-Haro jets (HH 1042 and HH 1043).[28] Jets of gas flowing out from young stars can be produced byaccretion onto a star.[29] In RCW 36 these jets were seen in a number of spectral lines, including lines from hydrogen, helium, oxygen, nitrogen, sulfur, nickel, calcium, and iron. Mass loss rates from the jets have been estimated to be on the order of 10−7M☉ solar masses per year. Inhomogeneities in the jets have been attributed to variable accretion rate on timescales of approximately 100 years.[28]
The young star 2MASS J08592851-4346029 has been classified as aHerbig Ae star. Stars in this class arepre-main-sequence, intermediate-mass stars (spectral type A) withemission lines in their spectra from hydrogen. Observations indicate that 2MASS J08592851-4346029 has a bloated radius as would be expected for a young star that is still contracting. Some of the lines in its spectrum have aP-Cygni Profile indicating the presence of a stellar wind.[6]
The young star CXOANC J085932.2−434602 was observed by the Chandra X-ray Observatory to have produced a largeflare with a peak temperature greater than 100 millionkelvins.[30] Such "super hot" flares from young stars have been seen in other star-forming regions like theOrion Nebula.[31]
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