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Cotton candy nebula (view source)
Revision as of 11:37, September 30, 2018
, 11:37, September 30, 2018Created page with "{{Night Sky | image = | designation =IRAS 17150−3224 | rightascension =17<sup>h</sup> 18<sup>m</sup> 19.85<sup>s</sup><ref name=simbad>[http://simbad.u-strasb..."
{{Night Sky
| image =
| designation =IRAS 17150−3224
| rightascension =17<sup>h</sup> 18<sup>m</sup> 19.85<sup>s</sup><ref name=simbad>[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=cotton+candy+nebula&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Cotton candy nebula] from the [http://simbad.u-strasbg.fr/simbad SIMBAD Astronomical Database]</ref>
| declination =-32° 27′ 21.6″<ref name=simbad/>
| distance =9,650 ly<ref name=dist>Vickers, S., Frew, D., Parker, Q. and Bojičić, I. (2014). New light on Galactic post-asymptotic giant branch stars – I. First distance catalogue. ''Monthly Notices of the Royal Astronomical Society'', 447(2), pp.1673-1691. [https://arxiv.org/abs/1403.7230 arXiv:1403.7230 <nowiki>[astro-ph.SR]</nowiki>]</ref>
| constellation =Ara
| type =Protoplanetary nebula
| dimensions =
| magnitude =
| redshift =
| radvelocity =
| propmotion =
| parallax =
}}
The '''Cotton candy nebula''' (IRAS 17150−3224) is a [[protoplanetary nebula]] in the [[constellation]] of [[Ara]], The Altar. The nebula has a bipolar structure (meaning it consists of two large lobes), with a central [[star]].<ref name=arxiv>Lagadec, E. et Al. (2011). A mid-infrared imaging catalogue of post-asymptotic giant branch stars. ''Monthly Notices of the Royal Astronomical Society'', 417(1), pp.32-92. [https://arxiv.org/abs/1102.4561 arXiv:1102.4561 <nowiki>[astro-ph.SR]</nowiki>]</ref> This central star is not visible in optical image of the nebula due to a dark lane that obscures it. However is can be observed in the [[infrared]] portion of the [[electromagnetic spectrum]], where the obscuring effects of dust are greatly reduced. The two lobes are spearated by this dark lane.<ref name=arxiv/> It is thought there is a [[torus|toriodal]] (doughnut-shaped) structure at the very core of the nebula that is expanding.<ref>Weintraub, D., Huard, T., Kastner, J. and Gatley, I. (1998). The Onset of Molecular Hydrogen Emission from Proto–planetary Nebulae. ''The Astrophysical Journal'', 509(2), pp.728-732. [http://adsabs.harvard.edu/abs/1998ApJ...509..728W Bibcode:1998ApJ...509..728W]</ref>
The nebula lies approximately 9,650 [[light year]]s from [[Earth]] and have a temperature between 168-409 kelvin.<ref name=dist/> The total [[luminosity]] of the nebula has been estimated to be 12,000 times that of the [[Sun]].<ref name=dist/> Intense [[ultraviolet]] radiation emanating from the central star [[ionization|ionizes]] the enveloping [[gas]], causing it to glow.
==References==
{{reflist}}
{{Nebulae}}
[[Category:Astronomy]]
[[Category:Nebulae]]
| image =
| designation =IRAS 17150−3224
| rightascension =17<sup>h</sup> 18<sup>m</sup> 19.85<sup>s</sup><ref name=simbad>[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=cotton+candy+nebula&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Cotton candy nebula] from the [http://simbad.u-strasbg.fr/simbad SIMBAD Astronomical Database]</ref>
| declination =-32° 27′ 21.6″<ref name=simbad/>
| distance =9,650 ly<ref name=dist>Vickers, S., Frew, D., Parker, Q. and Bojičić, I. (2014). New light on Galactic post-asymptotic giant branch stars – I. First distance catalogue. ''Monthly Notices of the Royal Astronomical Society'', 447(2), pp.1673-1691. [https://arxiv.org/abs/1403.7230 arXiv:1403.7230 <nowiki>[astro-ph.SR]</nowiki>]</ref>
| constellation =Ara
| type =Protoplanetary nebula
| dimensions =
| magnitude =
| redshift =
| radvelocity =
| propmotion =
| parallax =
}}
The '''Cotton candy nebula''' (IRAS 17150−3224) is a [[protoplanetary nebula]] in the [[constellation]] of [[Ara]], The Altar. The nebula has a bipolar structure (meaning it consists of two large lobes), with a central [[star]].<ref name=arxiv>Lagadec, E. et Al. (2011). A mid-infrared imaging catalogue of post-asymptotic giant branch stars. ''Monthly Notices of the Royal Astronomical Society'', 417(1), pp.32-92. [https://arxiv.org/abs/1102.4561 arXiv:1102.4561 <nowiki>[astro-ph.SR]</nowiki>]</ref> This central star is not visible in optical image of the nebula due to a dark lane that obscures it. However is can be observed in the [[infrared]] portion of the [[electromagnetic spectrum]], where the obscuring effects of dust are greatly reduced. The two lobes are spearated by this dark lane.<ref name=arxiv/> It is thought there is a [[torus|toriodal]] (doughnut-shaped) structure at the very core of the nebula that is expanding.<ref>Weintraub, D., Huard, T., Kastner, J. and Gatley, I. (1998). The Onset of Molecular Hydrogen Emission from Proto–planetary Nebulae. ''The Astrophysical Journal'', 509(2), pp.728-732. [http://adsabs.harvard.edu/abs/1998ApJ...509..728W Bibcode:1998ApJ...509..728W]</ref>
The nebula lies approximately 9,650 [[light year]]s from [[Earth]] and have a temperature between 168-409 kelvin.<ref name=dist/> The total [[luminosity]] of the nebula has been estimated to be 12,000 times that of the [[Sun]].<ref name=dist/> Intense [[ultraviolet]] radiation emanating from the central star [[ionization|ionizes]] the enveloping [[gas]], causing it to glow.
==References==
{{reflist}}
{{Nebulae}}
[[Category:Astronomy]]
[[Category:Nebulae]]