Elephant's Trunk Nebula

The Elephant's Trunk Nebula is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in the constellation Cepheus about 2,400 light years away from Earth.[1] The piece of the nebula shown here is the dark, dense globule IC 1396A; it is commonly called the Elephant's Trunk nebula because of its appearance at visible light wavelengths, where there is a dark patch with a bright, sinuous rim. The bright rim is the surface of the dense cloud that is being illuminated and ionized by a very bright, massive star (HD 206267) that is just to the east of IC 1396A. (In the Spitzer Space Telescope view shown, the massive star is just to the left of the edge of the image.) The entire IC 1396 region is ionized by the massive star, except for dense globules that can protect themselves from the star's harsh ultraviolet rays.

Elephant's Trunk Nebula
Emission nebula
Spitzer Space Telescope photo of the nebula
Captured in classic Hubble Palette (Ha/OIII/SII) by astronomer Chuck Ayoub using a 127mm refractor telescope
Elephant Trunk Nebula captured in Hydrogen alpha using a 102mm telescope
Elephant Trunk Nebula captured in Hydrogen Alpha and in Oxygen
Elephant trunk Ha+OIII+SII Hubble palette modified
Observation data
Distance2,400 ly
ConstellationCepheus
For similarly the named type of formation in other nebulae, see Elephant trunk (astronomy).

The Elephant's Trunk Nebula is now thought to be a site of star formation, containing several very young (less than 100,000 yr) stars that were discovered in infrared images in 2003. Two older (but still young, a couple of million years, by the standards of stars, which live for billions of years) stars are present in a small, circular cavity in the head of the globule. Winds from these young stars may have emptied the cavity.

The combined action of the light from the massive star ionizing and compressing the rim of the cloud, and the wind from the young stars shifting gas from the center outward lead to very high compression in the Elephant's Trunk Nebula. This pressure has triggered the current generation of protostars.[2][3]

References
  1. Matthews, H. I. (1979). "High resolution radio observations of bright rims in IC 1396". Astronomy and Astrophysics. 75: 345–350. Bibcode:1979A&A....75..345M.
  2. Barentsen, G. (2011). "T Tauri candidates and accretion rates using IPHAS: method and application to IC1396". Monthly Notices of the Royal Astronomical Society. 415: 103–132. arXiv:1103.1646. Bibcode:2011MNRAS.415..103B. doi:10.1111/j.1365-2966.2011.18674.x.
  3. Getman, K. V.; et al. (2012). "The Elephant Trunk Nebula and the Trumpler 37 cluster: contribution of triggered star formation to the total population of an H II region". Monthly Notices of the Royal Astronomical Society. 426 (4): 2917–2943. arXiv:1208.1471. Bibcode:2012MNRAS.426.2917G. doi:10.1111/j.1365-2966.2012.21879.x.


This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.