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{{Short description|Planetary nebula in the constellation Cepheus}}
{{Infobox nebula
{{Infobox nebula
| image = [[File:NGC 7354.jpg|250px]]
| image = [[File:NGC 7354.jpg|250px]]
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This nebula is the result of an aging star casting off its outer atmosphere.<ref name=Phillips2009/> Overall the nebula is elliptical in form, with a complex interior structure having inner and outer shells, several bright equatorial knots, and two [[Astrophysical jet|jet-like features]] near the nebula poles.<ref name=Contreras2010/> The rim of the inner shell is ellipsoidal with an aspect ratio of 1.6 and a major axis spanning {{val|30|ul=arcsecond}}. The outer shell is more circular, and is approximately {{val|33|u=arcsecond}} in diameter.<ref name=Phillips2009/> The faint outer shell is expanding with a higher velocity than the inner shell, and the knots are moving at the same velocity as the outer shell. The outer shell has an estimated age of 2,500&nbsp;years, while the inner shell is 1,600&nbsp;years old.<ref name=Contreras2010/>
This nebula is the result of an aging star casting off its outer atmosphere.<ref name=Phillips2009/> Overall the nebula is elliptical in form, with a complex interior structure having inner and outer shells, several bright equatorial knots, and two [[Astrophysical jet|jet-like features]] near the nebula poles.<ref name=Contreras2010/> The rim of the inner shell is ellipsoidal with an aspect ratio of 1.6 and a major axis spanning {{val|30|ul=arcsecond}}. The outer shell is more circular, and is approximately {{val|33|u=arcsecond}} in diameter.<ref name=Phillips2009/> The faint outer shell is expanding with a higher velocity than the inner shell, and the knots are moving at the same velocity as the outer shell. The outer shell has an estimated age of 2,500&nbsp;years, while the inner shell is 1,600&nbsp;years old.<ref name=Contreras2010/>


The morphological features of the nebula may be explained by an interacting [[binary star]] system with one of the pair passing through the [[asymptotic giant branch]] phase. The jets may be generated by an [[accretion disk]] surrounding the resulting [[white dwarf]] star.<ref name=Contreras2010/>
The morphological features of the nebula may be explained by an interacting [[binary star]] system with one of the pair passing through the [[asymptotic giant branch]] phase. The jets may be generated by an [[accretion disk]] surrounding the resulting [[white dwarf]] star.<ref name=Contreras2010/> Additionally, an analysis of ''[[Gaia (spacecraft)|Gaia]]'' data suggests that the central star is binary.<ref name=Chornay>{{cite journal|doi=10.1051/0004-6361/202140288|title=Towards a more complete sample of binary central stars of planetary nebulae with Gaia|year=2021|last1=Chornay|first1=N.|last2=Walton|first2=N. A.|last3=Jones|first3=D.|last4=Boffin|first4=H. M. J.|last5=Rejkuba|first5=M.|last6=Wesson|first6=R.|journal=Astronomy & Astrophysics|volume=648|pages=A95|arxiv=2101.01800|bibcode=2021A&A...648A..95C|s2cid=230770301}}</ref>


== References ==
== References ==
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<ref name=simbad>{{cite simbad
<ref name=simbad>{{cite simbad
| title=NGC 7354 | accessdate=2020-10-09 }}</ref>
| title=NGC 7354 | access-date=2020-10-09 }}</ref>


<ref name=cseligman>{{cite web
<ref name=cseligman>{{cite web
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| volume=399 | issue=3 | pages=1126–1144 | date=November 2009
| volume=399 | issue=3 | pages=1126–1144 | date=November 2009
| arxiv=0909.1829 | bibcode=2009MNRAS.399.1126P
| arxiv=0909.1829 | bibcode=2009MNRAS.399.1126P
| doi=10.1111/j.1365-2966.2009.15379.x }}</ref>
| doi=10.1111/j.1365-2966.2009.15379.x | doi-access=free | s2cid=118344696 }}</ref>


<ref name=Contreras2010>{{cite journal
<ref name=Contreras2010>{{cite journal
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| volume=139 | issue=4 | pages=1426–1437 | date=April 2010
| volume=139 | issue=4 | pages=1426–1437 | date=April 2010
| arxiv=1002.0881 | bibcode=2010AJ....139.1426C
| arxiv=1002.0881 | bibcode=2010AJ....139.1426C
| doi=10.1088/0004-6256/139/4/1426 }}</ref>
| doi=10.1088/0004-6256/139/4/1426 | s2cid=118501386 }}</ref>


<ref name=Stanghellini2008>{{cite journal
<ref name=Stanghellini2008>{{cite journal
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| volume=689 | issue=1 | pages=194–202 | year=2008
| volume=689 | issue=1 | pages=194–202 | year=2008
| arxiv=0807.1129 | bibcode = 2008ApJ...689..194S
| arxiv=0807.1129 | bibcode = 2008ApJ...689..194S
| doi=10.1086/592395 }}</ref>
| doi=10.1086/592395 | s2cid=119257242 }}</ref>


}}
}}
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{{Cepheus (constellation)}}
{{Cepheus (constellation)}}


{{DEFAULTSORT:NGC 7354}}
[[Category:Planetary nebulae]]
[[Category:Planetary nebulae]]
[[Category:NGC objects|7354]]
[[Category:NGC objects|7354]]

Latest revision as of 08:14, 23 August 2024

NGC 7354
Emission nebula
Planetary nebula
Hubble Space Telescope image of NGC 7354
Observation data: J2000 epoch
Right ascension22h 40m 19.87387s[1]
Declination+61° 17′ 08.7444″[1]
Distance5,538[2] ly   (1,698 pc)
Apparent dimensions (V)20.0″[2]
ConstellationCepheus
DesignationsPN G107.8+02.3, IRAS 22384+6101, NGC 7354[3]
See also: Lists of nebulae

NGC 7354 is a planetary nebula located in the northern circumpolar constellation of Cepheus, at a distance of approximately 5.5 kly from the Sun.[2] It was discovered by German-born astronomer William Herschel on November 3, 1787. John L. E. Dreyer described it as, "a planetary nebula, bright, small, round, pretty gradually a very little brighter middle".[4]

This nebula is the result of an aging star casting off its outer atmosphere.[5] Overall the nebula is elliptical in form, with a complex interior structure having inner and outer shells, several bright equatorial knots, and two jet-like features near the nebula poles.[6] The rim of the inner shell is ellipsoidal with an aspect ratio of 1.6 and a major axis spanning 30″. The outer shell is more circular, and is approximately 33″ in diameter.[5] The faint outer shell is expanding with a higher velocity than the inner shell, and the knots are moving at the same velocity as the outer shell. The outer shell has an estimated age of 2,500 years, while the inner shell is 1,600 years old.[6]

The morphological features of the nebula may be explained by an interacting binary star system with one of the pair passing through the asymptotic giant branch phase. The jets may be generated by an accretion disk surrounding the resulting white dwarf star.[6] Additionally, an analysis of Gaia data suggests that the central star is binary.[7]

References

[edit]
  1. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c Stanghellini, Letizia; et al. (2008). "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale". The Astrophysical Journal. 689 (1): 194–202. arXiv:0807.1129. Bibcode:2008ApJ...689..194S. doi:10.1086/592395. S2CID 119257242.
  3. ^ "NGC 7354". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-10-09.
  4. ^ Seligman, Courtney. "NGC Objects: NGC 7350 - 7399". Retrieved 2020-10-09.
  5. ^ a b Phillips, J. P.; et al. (November 2009). "Rings and haloes in the mid-infrared: the planetary nebulae NGC 7354 and NGC 3242". Monthly Notices of the Royal Astronomical Society. 399 (3): 1126–1144. arXiv:0909.1829. Bibcode:2009MNRAS.399.1126P. doi:10.1111/j.1365-2966.2009.15379.x. S2CID 118344696.
  6. ^ a b c Contreras, M. E.; et al. (April 2010). "Observational Study of the Multistructured Planetary Nebula NGC 7354". The Astronomical Journal. 139 (4): 1426–1437. arXiv:1002.0881. Bibcode:2010AJ....139.1426C. doi:10.1088/0004-6256/139/4/1426. S2CID 118501386.
  7. ^ Chornay, N.; Walton, N. A.; Jones, D.; Boffin, H. M. J.; Rejkuba, M.; Wesson, R. (2021). "Towards a more complete sample of binary central stars of planetary nebulae with Gaia". Astronomy & Astrophysics. 648: A95. arXiv:2101.01800. Bibcode:2021A&A...648A..95C. doi:10.1051/0004-6361/202140288. S2CID 230770301.
[edit]
  • Media related to NGC 7354 at Wikimedia Commons
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