Astronomy:NGC 7027

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Short description: Planetary nebula in the constellation Cygnus
NGC 7027
Emission nebula
Planetary nebula
File:NGC7027 - HST - Heic2011c.tif
Hubble image of NGC 7027
Observation data: J2000 epoch
Right ascension 21h 07m 1.7s[1]
Declination+42° 14′ 11″[1]
Distance3,000[2] ly
Apparent magnitude (V)10[3]
Apparent dimensions (V)16" × 12"
ConstellationCygnus
Physical characteristics
Dimensions0.2 × 0.1 ly[4]
Notable featuresYoung (600 years) and unusually massive (3–4 M☉)
DesignationsJewel Bug Nebula,[citation needed] Gummy Bear Nebula[5]
See also: Lists of nebulae

NGC 7027, also known as the Jewel Bug Nebula, is a very young and dense planetary nebula[6] located around 3,000 light-years (920 parsecs) from Earth in the constellation Cygnus. Discovered in 1878 by Édouard Stephan using the 800 mm (31 in) reflector at Marseille Observatory,[4] it is one of the smallest planetary nebulae and by far the most extensively studied.[4]

Observation

NGC 7027 is one of the visually brightest planetary nebulae.[7] In a 6" telescope at around 50× it appears as a relatively bright bluish star. It is best viewed with the highest magnification possible.[5]

In 1977 at Yerkes Observatory, a small Schmidt telescope was used to derive an accurate optical position for the planetary nebula NGC 7027 to allow comparison between photographs and radio maps of the object.[8]

It has been photographed multiple times by the Hubble Space Telescope since its launch in 1990.[9][10] 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.[4]

Overview

NGC 7027 is unusually small, measuring only 0.2 by 0.1 light-years, whereas the typical size for a planetary nebula is 1 light-year.[4] It is fairly young, at about 600 years old.[11] It has a very complex shape, consisting of an elliptical region of ionized gas[12] and an equatorial belt[13] within a massive neutral cloud.[14] The inner structure is surrounded by a translucent shroud of gas and dust.[15] The nebula is shaped like a prolate ellipsoidal shell and contains a photodissociation region shaped like a "clover leaf".[12] The inner shell is also punctured by several shocks and X-ray jets, leading to the "spike"-like structures.[13] NGC 7027 is expanding at 17 kilometers per second (11 mi/s).[14] The central regions of NGC 7027 have been found to emit X-rays, indicating very high temperatures.[12] Surrounding the ellipsoidal nebula are a series of faint, blue concentric shells.[16]

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.[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.[17] 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.[18] The nebula contains ions of extremely high ionization potential.[19] The helium hydride ion, thought to be the earliest molecule to have been formed in the Universe (about 100,000 years after the Big Bang), was detected in 2019 for the first time in space in NGC 7027.[20][21] There is also evidence for the presence of nanodiamond in NGC 7027.[22]

Central star

NGC 7027 has a rich and highly ionized spectrum caused by its hot central star.[6] The progenitor star of NGC 7027 is believed to have been about 3 to 4 times the mass of the Sun before the nebula was formed.[6] It is possible that the central white dwarf of NGC 7027 has an accretion disk that acts as a source of high temperatures.[23] 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.[7] 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.[24]

The central star is suspected to be a binary system with the secondary being undetected. Although the details of NGC 7027's formation are unclear, it is hypothesized that interactions with the secondary star produced the complex structure of the planetary nebula, including the jets and resulting spikes.[13]

See also

References

  1. ↑ 1.0 1.1 "NASA/IPAC Extragalactic Database". Results for NGC 7027. http://ned.ipac.caltech.edu/byname?objname=NGC%207027&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Latter, William B. (12 March 1998). "Staring into the Winds of Destruction: HST/NICMOS Images of the Planetary Nebula NGC 7027". SIRTF Science Center. http://spider.ipac.caltech.edu/staff/latter/N7027description.html. 
  3. ↑ "NGC 7027". SEDS NGC Database. http://spider.seds.org/ngc/ngc.cgi?CatalogNumber=NGC+7027. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 O'Meara, Stephen James (2007). "104: NGC 7027". Hidden Treasures. Cambridge University Press. pp. 514–516. ISBN 978-0-521-83704-0. https://books.google.com/books?id=a6VY0Q1zsJoC&pg=PA514. 
  5. ↑ 5.0 5.1 "NGC 7027 – Gummy Bear Planetary Nebula". 26 September 2016. https://stargazerslounge.com/topic/278437-ngc-7027-gummy-bear-planetary-nebula/. 
  6. ↑ 6.0 6.1 6.2 Salas, J. Bernard et al. (March 2001). "The ISO-SWS spectrum of planetary nebula NGC 7027". Astronomy & Astrophysics 367 (3): 949–958. doi:10.1051/0004-6361:20000435. Bibcode: 2001A&A...367..949B. https://www.rug.nl/research/portal/files/56918172/The_ISO_SWS_spectrum_of_planetary_nebula.pdf. 
  7. ↑ 7.0 7.1 Kaler, James B. (2002). The 100 Greatest Stars. New York: Springer-Verlag. pp. 133. ISBN 978-0-387-95436-3. https://books.google.com/books?id=MXxBoLwu2QMC&pg=PT220. 
  8. ↑ Cudworth, K. M.; Oravecz, M. (June–July 1978). "Astrometry with a small Schmidt telescope: The position of NGC 7027". Astronomical Society of the Pacific 90: 333–334. doi:10.1086/130337. Bibcode: 1978PASP...90..333C. 
  9. ↑ "Planetary Nebula NGC 7027: A Sun-Like Star Burning Out". 19 March 1998. https://hubblesite.org/contents/media/images/1998/11/626-Image.html. 
  10. ↑ "NGC 7027". Hubble Legacy Archive. https://hla.stsci.edu/hlaview.html#Inventory%7CfilterText%3D%24filterTypes%3D%7Cquery_string=NGC%207027&listdelimiter=whitespace&listformat=degrees&RA=316.756380&Dec=42.236530&Radius=0.200000&inst=WFPC2&inst=NICMOS&imagetype=best&preview=1&output_size=256&cutout_size=12.8. 
  11. ↑ Cox, P. (January 1997). "Planetary Nebulae". Astrophysics and Space Science 255 (1–2): 489–497. doi:10.1023/A:1001511603093. Bibcode: 1998Ap&SS.255..489C. https://books.google.com/books?id=QG3dN6hpJwAC&pg=PA490. 
  12. ↑ 12.0 12.1 12.2 Kastner, Joel H. et al. (April 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. doi:10.1086/319651. Bibcode: 2001ApJ...550L.189K. 
  13. ↑ 13.0 13.1 13.2 Moraga Baez, Paula; Kastner, Joel H.; Balick, Bruce; Montez, Rodolfo; Bublitz, Jesse (2023). "Panchromatic HST/WFC3 Imaging Studies of Young, Rapidly Evolving Planetary Nebulae. II. NGC 7027". The Astrophysical Journal 942 (1): 15. doi:10.3847/1538-4357/aca401. Bibcode: 2023ApJ...942...15M. 
  14. ↑ 14.0 14.1 Masson, C. R. (January 1989). "The structure of NGC 7027 and a determination of its distance by measurement of proper motions". The Astrophysical Journal 336: 294–303. doi:10.1086/167011. Bibcode: 1989ApJ...336..294M. 
  15. ↑ "NGC 7027". NOAO. http://www.noao.edu/outreach/aop/observers/n7027.html. 
  16. ↑ "Hubble Telescope Photo Reveals Stellar Death Process". 16 January 1996. https://hubblesite.org/contents/news-releases/1996/news-1996-05.html. 
  17. ↑ Liu, X.-W. et al. (October 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. doi:10.1093/mnras/290.4.l71. Bibcode: 1997MNRAS.290L..71L. http://discovery.ucl.ac.uk/1381067/1/1381067.pdf. 
  18. ↑ Kwok, Sun; Sandford, Scott (2008). Organic Matter in Space. Cambridge University Press. p. 170. ISBN 978-0-521-88982-7. https://books.google.com/books?id=EWURgHzF3DQC&pg=PA170. 
  19. ↑ Gurzadian, Grigor Aramovich (1997). The physics and dynamics of planetary nebulae. Springer-Verlag. p. 45. ISBN 978-3-540-60965-0. https://books.google.com/books?id=xxVkZBVIZeAC&pg=PP245. 
  20. ↑ Güsten, Rolf et al. (April 2019). "Astrophysical detection of the helium hydride ion HeH+". Nature 568 (7752): 357–359. doi:10.1038/s41586-019-1090-x. PMID 30996316. Bibcode: 2019Natur.568..357G. 
  21. ↑ Fisher, Christine (17 April 2019). "NASA finally found evidence of the universe's earliest molecule – The elusive helium hydride was found 3,000 light-years away". Engadget. https://www.engadget.com/2019/04/17/nasa-sofia-detects-helium-hydride/. 
  22. ↑ Reddy, Francis (17 January 2006). "Seeing red with nanodiamonds". http://www.astronomy.com/asy/default.aspx?c=a&id=3851. 
  23. ↑ Gurzadian, Grigor Aramovich (1997). The physics and dynamics of planetary nebulae. Springer-Verlag. p. 464. ISBN 978-3-540-60965-0. https://books.google.com/books?id=xxVkZBVIZeAC&pg=PP245. 
  24. ↑ "Hubble Captures the Shrouds of Dying Stars". 19 March 1998. https://hubblesite.org/contents/news-releases/1998/news-1998-11.html. 

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