- NGC 7027
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NGC 7027 
Observation data
(Epoch J2000)Right ascension 21h 7m 1.7s[1] Declination +42° 14′ 11″[1] Distance 3,000 ly[2] Apparent magnitude (V) 10[3] Apparent dimensions (V) 14" Constellation Cygnus Physical characteristics Radius 14,000 AU[2] See also: Planetary nebula, Lists of nebulae NGC 7027 is a very young and dense planetary nebula[4] located around 3,000 light-years (920 pc) away in the constellation Cygnus. It was discovered in 1878 by Édouard Jean-Marie Stephan, using the 31 inch reflector at Marseille Observatory.[5] It is one of the smallest planetary nebulae, and by far the most extensively studied.[5]
NGC 7027 is one of the visually brightest planetary nebulae.[6] It is about 600 years old.[7]
It is unusually small, measuring only 0.2 by 0.1 light-years whereas the typical size for a planetary nebula is 1 light-year.[8] It has a very complex shape, consisting of an elliptical region of ionized gas[9] within a massive neutral cloud.[10] The inner structure is surrounded by a translucent shroud of gas and dust.[11] The nebula is shaped like a prolate ellipsoidal shell and contains a photodissociation region shaped like a "clover leaf".[9] NGC 7027 is expanding at 17 kilometers per second (11 mi/s).[10] The central regions of NGC 7027 have been found to emit X-rays, indicating very high temperatures.[9] Surrounding the ellipsoidal nebula are a series of faint, blue concentric shells.[12]
It is possible that the central white dwarf of NGC 7027 has an accretion disk that acts as a source of high temperatures.[13] The white dwarf is believed to have a mass approximately 0.7 times the mass of the Sun and is radiating at 7,700 times the Sun's luminosity.[6] NGC 7027 is currently in a short phase of planetary nebula evolution in which molecules in its envelope are being dissociated into their component atoms, and the atoms are being ionized.[14]
The expanding halo of NGC 7027 has a mass of about three times the mass of the Sun, and is about 100 times more massive than the ionized central region. This mass loss in NGC 7027 provided important evidence that stars a few times more massive than the Sun can avoid being destroyed in supernova explosions.[8]
NGC 7027 has a rich and highly ionized spectrum caused by its hot central star.[4] The nebula is rich in carbon, and is a very interesting object for the study of carbon chemistry in dense molecular material exposed to strong ultraviolet radiation.[15] The spectrum of NGC 7027 contains fewer spectral lines from neutral molecules than is usual for planetary nebulae. This is due to the destruction of neutral molecules by intense UV radiation.[16] The nebula contains ions of extremely high ionization potential.[17] NGC 7027 is a promising place to look for HeH+, a molecule which is believed to exist in interstellar space, but which has never been conclusively identified.[15] There is evidence for the presence of nanodiamond in NGC 7027.[18]
It was photographed by the Hubble Space Telescope in 1996. Prior to these observations, NGC 7027 was thought to be a proto-planetary nebula with the central star too cool to ionize any of the gas, but it is now known to be a planetary nebula in the earliest stage of its development.[8] The central star is believed to have been about 3–4 times the mass of the Sun.[4]
Despite being so well known and studied, NGC 7027 does not have a popular name.[6] In a 6" telescope at around 50x it appears as a relatively bright bluish star. It is best viewed with the highest magnification possible.
See also
References
- ^ a b "NASA/IPAC EXTRAGALACTIC DATABASE". Results for NGC 7027. http://nedwww.ipac.caltech.edu. Retrieved 2008-04-02.
- ^ a b "Staring into the Winds of Destruction: HST/NICMOS Images of the Planetary Nebula NGC 7027". http://spider.ipac.caltech.edu/staff/latter/N7027description.html. Retrieved 2008-10-11.
- ^ "NGC 7027". SEDS NGC Database. http://seds.org/~spider/ngc/ngc.cgi?7027. Retrieved 2008-10-11.
- ^ a b c Bernard Salas, J.; Pottasch, S. R.; Beintema, D. A.; Wesselius, P. R. (2001). "The ISO-SWS spectrum of planetary nebula NGC 7027". Astronomy and Astrophysics 367 (3): 949–958. Bibcode 2001A&A...367..949B. doi:10.1051/0004-6361:20000435.
- ^ a b O'Meara, Stephen James (2007). Hidden Treasures. pp. 514. ISBN 0521837049. http://books.google.com/?id=a6VY0Q1zsJoC&pg=PA514&dq=ngc+7027&cd=6#v=onepage&q=ngc%207027.
- ^ a b c Kaler, James B. (2002). The 100 Greatest Stars. New York: Springer-Verlag. pp. 133. ISBN 0-387-93436-8. http://books.google.com/?id=MXxBoLwu2QMC&pg=PT220&dq=ngc+7027&cd=4#v=onepage&q=ngc%207027.
- ^ Waters, L. B. F. M.; C Waelkens, Karel A. van der Hucht (1998-08-31). ISO's View on Stellar Evolution. pp. 490. ISBN 9780792351528. http://books.google.com/?id=QG3dN6hpJwAC&pg=PA490&dq=ngc+7027+spectrum&cd=38#v=onepage&q=ngc%207027%20spectrum.
- ^ a b c O'Meara, Stephen James (2007). Hidden Treasures. pp. 516. ISBN 0521837049. http://books.google.com/?id=a6VY0Q1zsJoC&pg=PA514&dq=ngc+7027&cd=6#v=onepage&q=ngc%207027.
- ^ a b c Kastner, Joel H.; Vrtilek, Saeqa D.; Soker, Noam (04/2001). "Discovery of Extended X-Ray Emission from the Planetary Nebula NGC 7027 by the Chandra X-Ray Observatory". The Astrophysical Journal 550 (2): L189–L192. arXiv:astro-ph/0102468. Bibcode 2001ApJ...550L.189K. doi:10.1086/319651.
- ^ a b Masson, C. R. (1989/1). "The structure of NGC 7027 and a determination of its distance by measurement of proper motions". The Astrophysical Journal 336: 294–303. Bibcode 1989ApJ...336..294M. doi:10.1086/167011.
- ^ "NGC 7027". NOAO. http://www.noao.edu/outreach/aop/observers/n7027.html. Retrieved 2010-03-11.
- ^ "Hubble Telescope Photo Reveals Stellar Death Process". 1996-01-16. http://hubblesite.org/newscenter/archive/releases/1996/1996/05/. Retrieved 2010-03-11.
- ^ Gurzadi︠a︡n, Grigor Aramovich (1997). The physics and dynamics of planetary nebulae. Springer-Verlag. pp. 464. ISBN 3-540-60965-2. http://books.google.com/?id=xxVkZBVIZeAC&pg=PP245&dq=ngc+7027+spectrum&cd=17#v=onepage&q=ngc%207027%20spectrum.
- ^ "Hubble Captures the Shrouds of Dying Stars". 1998-03-18. http://hubblesite.org/newscenter/archive/releases/1998/11/background/. Retrieved 2010-03-11.
- ^ a b Liu, X.-W.; Barlow, M. J.; Dalgarno, A.; Tennyson, J.; Lim, T.; Swinyard, B. M.; Cernicharo, J.; Cox, P.; Baluteau, J.-P.; Pequignot, D.; Nguyen-Q-Rieu; Emery, R. J.; Clegg, P. E (10/1997). "An ISO Long Wavelength Spectrometer detection of CH in NGC 7027 and an HeH^+ upper limit". Monthly Notices of the Royal Astronomical Society 290 (4): L71–L75. Bibcode 1997MNRAS.290L..71L.
- ^ Kwok, Sun; Sandford, Scott (2008). Organic Matter in Space. United Kingdom: Cambridge University Press. pp. 170. ISBN 9780 521 889 827. http://books.google.com/?id=EWURgHzF3DQC&pg=PA170&dq=ngc+7027+molecules&cd=24#v=onepage&q=ngc%207027%20molecules.
- ^ Gurzadi︠a︡n, Grigor Aramovich (1997). The physics and dynamics of planetary nebulae. Springer-Verlag. pp. 45. ISBN 3-540-60965-2. http://books.google.com/?id=xxVkZBVIZeAC&pg=PP245&dq=ngc+7027+spectrum&cd=17#v=onepage&q=ngc%207027%20spectrum.
- ^ Reddy, Francis (2006-01-17). "Seeing red with nanodiamonds". Astronomy.com. http://www.astronomy.com/asy/default.aspx?c=a&id=3851. Retrieved 2010-03-11.
External links
Categories:- Protoplanetary nebulae
- Planetary nebulae
- NGC objects
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