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Created page with "{{Night Sky | image = | designation =NGC 2346<br/>V651 Mon | rightascension =07<sup>h</sup> 09<sup>m</sup> 22.5217<sup>s</sup><ref name=simbad>{{cite web|url=ht..."
{{Night Sky
| image =
| designation =NGC 2346<br/>V651 Mon
| rightascension =07<sup>h</sup> 09<sup>m</sup> 22.5217<sup>s</sup><ref name=simbad>{{cite web|url=https://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC+2346&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id|title=NGC 2346|accessdate=2019-08-25|work=Simbad Astronomical Database|publisher=simbad.u-strasbg.fr}}</ref><ref name=vizie>Gaia Colaboration. VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018). (2018). ''VizieR Online Data Catalog''. {{Bibcode|2018yCat.1345....0G}}</ref>
| declination =-00° 48′ 23.611″<ref name=simbad/><ref name=vizie/>
| distance =2,300 ly<ref name=spacetelescope>{{cite web|url=https://www.spacetelescope.org/images/opo9935d/|title=NGC 2346|accessdate=2019-08-25|publisher=spacetelescope.org|date=1999-10-07}}</ref>
| constellation =Monoceros
| type =Planetary nebula
| dimensions =0.910'×0.910'<ref name=simbad/><ref>
{{cite journal
|last1=Stanghellini |first1=L.
|last2=Shaw |first2=R. A.
|last3=Villaver |first3=E.
|title=The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale
|journal=The Astrophysical Journal
|volume=689
|issue=1|page=194-202|date=2008
|doi=10.1086/592395
|bibcode=2008ApJ...689..194S
|ref=harv
}} {{arXiv|0807.1129}}
</ref>
| magnitude =Apparent Mag: +11.58<ref name=simbad/><ref>
{{cite journal
|last1=Høg |first1=E.
|last2=Fabricius |first2=C.
|last3=Makarov |first3=V. V.
|last4=Urban |first4=S.
|last5=Corbin |first5=T.
|last6=Wycoff |first6=G.
|last7=Bastian |first7=U.
|last8=Schwekendiek |first8=P.
|last9=Wicenec |first9=A.
|display-authors=3
|title=The Tycho-2 catalogue of the 2.5 million brightest stars
|journal=Astronomy and Astrophysics
|volume=355
|page=L27-L30|date=2000
|bibcode=2000A&A...355L..27H
|ref=harv
}}
</ref><br/>Absolute Mag: +2.34<ref>From direct calculation using distance of 2,300 ly and [[star magnitude|apparent magnitude]] of +11.58.</ref>
| redshift =
| radvelocity =47.00 km/s<ref name=simbad/><ref>
{{cite journal
|last1=Barbier-Brossat |first1=M.
|last2=Petit |first2=M.
|last3=Figon |first3=P.
|display-authors=3
|title=Third bibliographic catalogue of stellar radial velocities
|journal=Astronomy and Astrophysics Supplementary Series
|volume=108
|issue=|page=603-609|date=1994
|doi=
|bibcode=1994A&AS..108..603B
|ref=harv
}}
</ref>
| propmotion =RA: -2.146 mas/year<ref name=simbad/><ref name=vizie/><br/>Dec: -1.219 mas/year<ref name=simbad/><ref name=vizie/>
| parallax =0.6861±0.0431 mas<ref name=simbad/><ref name=vizie/>
}}
'''NGC 2346''' (V651 Mon) is a [[planetary nebula]] in the [[constellation]] of [[Monoceros]].<ref name=apod>{{cite web|url=https://apod.nasa.gov/apod/ap011028.html|title=NGC 2346: A Butterfly-Shaped Planetary Nebula|accessdate=2019-08-25|publisher=apod.nasa.gov|date=2001-10-28}}</ref> The nebula is unusual for having a very small [[binary star|binary system]] at its centre that has an orbital period of only 16 days.<ref name=spacetelescope/> NGC 2346 was discovered in 1795 by [[William Herschel]].<ref name=skyandtelescope>{{cite web|url=https://www.skyandtelescope.com/observing/ngc-2346-bi-polar-nebula-with-a-peek-a-boo-star030220160203/|title=NGC 2346: A Cosmic Butterfly Plays Peekaboo|accessdate=2019-08-25|date=2016-03-02|piblisher=skyandtelescope.com|author=Bob King}}</ref> The nebula is sometimes called the "Butterfly nebula," though this more commonly refers to [[Butterfly nebula|NGC 6302]].
The nebula is thought to lie about 2,300 [[light year]]s away.<ref name=spacetelescope/> It has an apparent diameter of 0.910 [[arcminute]]s which corresponds to a physical size of roughly one third of a light year across. The nebula is a bipolar planetary nebula meaning it has two large protrusions or lobes pointing in opposite directions. large clumps of material as well as a [[torus|toriodal]] structure have been observed in the nebula.<ref name=Manchado>
{{cite journal
|last1=Manchado |first1=L.
|last2=Stanghellini |first2=E.
|last3=Villaver |first3=E.
|last4=Garcia-Segura |first4=G.
|last5=Shaw |first5=R. A.
|last6=Garcia-Hernandez |first6=D. A.
|display-authors=3
|title=High resolution imaging of NGC 2346 with GSAOI/GeMS: disentangling the planetary nebula molecular structure to understand its origin and evolution
|journal=The Astrophysical Journal
|volume=808
|issue=2|page=|date=2015
|doi=10.1088/0004-637X/808/2/115
|bibcode=2015ApJ...808..115M
|ref=harv
}} {{arXiv|1506.03712}}
</ref>
==Binary star system==
The [[star]]s at the nebula's core orbit each other every 15.99 days with a separation estimated between 0.159-0.167 [[AU]] or 34.2-35.7 solar radii.<ref name=Kato>
{{cite journal
|last1=Kato |first1=T.
|last2=Nogami |first2=D.
|last3=Baba |first3=H.
|title=The 1996-1997 Fading of V651 Mon, the Binary Central Star of the Planetary Nebula NGC 2346
|journal=Publications of the Astronomical Society of Japan
|volume=53
|issue=5|page=901–904|date=2001
|doi=10.1093/pasj/53.5.901
|bibcode=
|ref=harv
}} {{arXiv|astro-ph/0112304}}
</ref> The binary system has a combined apparent magnitude of +11.<ref name=skyandtelescope/> The first star in the system is a A5V subdwarf star with a mass 1.8 times that of the [[Sun]] and a [[luminosity]] 18 times larger.<ref name=Manchado/> It has a surface temperature of 8,000 kelvin, making it slightly hotter than the Sun's surface. The other star is thought to be a [[white dwarf]] star with a surface temperature in excess of 100,000 kelvin.
The two stars form a [[variable star]], thought to be caused by dust surrounding the stars' occasionally dimming their light.<ref name=skyandtelescope/> Early photographic plates of the stars suggest their light was steady from 1899 until 1981 when it suddenly dropped, reducing the apparent magnitude of the two stars to +15. It then regularly varied between +15 and +11 with its usual period of 16 days. It is thought to be because the brighter of the two stars would periodically be hidden by a cloud in front of the nebula, estimated at perhaps 12 to 30 million miles across.<ref name=skyandtelescope/> This lasted until 1985 when the star's brightness recovered. In 1996 the star experienced another such dimming though to be caused for similar reasons that lasted for around 400 days. Yet another such dimming occurred in 2004.
==References==
{{reflist}}
{{Nebulae}}
[[Category:Astronomy]]
[[Category:Nebulae]]
| image =
| designation =NGC 2346<br/>V651 Mon
| rightascension =07<sup>h</sup> 09<sup>m</sup> 22.5217<sup>s</sup><ref name=simbad>{{cite web|url=https://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC+2346&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id|title=NGC 2346|accessdate=2019-08-25|work=Simbad Astronomical Database|publisher=simbad.u-strasbg.fr}}</ref><ref name=vizie>Gaia Colaboration. VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018). (2018). ''VizieR Online Data Catalog''. {{Bibcode|2018yCat.1345....0G}}</ref>
| declination =-00° 48′ 23.611″<ref name=simbad/><ref name=vizie/>
| distance =2,300 ly<ref name=spacetelescope>{{cite web|url=https://www.spacetelescope.org/images/opo9935d/|title=NGC 2346|accessdate=2019-08-25|publisher=spacetelescope.org|date=1999-10-07}}</ref>
| constellation =Monoceros
| type =Planetary nebula
| dimensions =0.910'×0.910'<ref name=simbad/><ref>
{{cite journal
|last1=Stanghellini |first1=L.
|last2=Shaw |first2=R. A.
|last3=Villaver |first3=E.
|title=The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale
|journal=The Astrophysical Journal
|volume=689
|issue=1|page=194-202|date=2008
|doi=10.1086/592395
|bibcode=2008ApJ...689..194S
|ref=harv
}} {{arXiv|0807.1129}}
</ref>
| magnitude =Apparent Mag: +11.58<ref name=simbad/><ref>
{{cite journal
|last1=Høg |first1=E.
|last2=Fabricius |first2=C.
|last3=Makarov |first3=V. V.
|last4=Urban |first4=S.
|last5=Corbin |first5=T.
|last6=Wycoff |first6=G.
|last7=Bastian |first7=U.
|last8=Schwekendiek |first8=P.
|last9=Wicenec |first9=A.
|display-authors=3
|title=The Tycho-2 catalogue of the 2.5 million brightest stars
|journal=Astronomy and Astrophysics
|volume=355
|page=L27-L30|date=2000
|bibcode=2000A&A...355L..27H
|ref=harv
}}
</ref><br/>Absolute Mag: +2.34<ref>From direct calculation using distance of 2,300 ly and [[star magnitude|apparent magnitude]] of +11.58.</ref>
| redshift =
| radvelocity =47.00 km/s<ref name=simbad/><ref>
{{cite journal
|last1=Barbier-Brossat |first1=M.
|last2=Petit |first2=M.
|last3=Figon |first3=P.
|display-authors=3
|title=Third bibliographic catalogue of stellar radial velocities
|journal=Astronomy and Astrophysics Supplementary Series
|volume=108
|issue=|page=603-609|date=1994
|doi=
|bibcode=1994A&AS..108..603B
|ref=harv
}}
</ref>
| propmotion =RA: -2.146 mas/year<ref name=simbad/><ref name=vizie/><br/>Dec: -1.219 mas/year<ref name=simbad/><ref name=vizie/>
| parallax =0.6861±0.0431 mas<ref name=simbad/><ref name=vizie/>
}}
'''NGC 2346''' (V651 Mon) is a [[planetary nebula]] in the [[constellation]] of [[Monoceros]].<ref name=apod>{{cite web|url=https://apod.nasa.gov/apod/ap011028.html|title=NGC 2346: A Butterfly-Shaped Planetary Nebula|accessdate=2019-08-25|publisher=apod.nasa.gov|date=2001-10-28}}</ref> The nebula is unusual for having a very small [[binary star|binary system]] at its centre that has an orbital period of only 16 days.<ref name=spacetelescope/> NGC 2346 was discovered in 1795 by [[William Herschel]].<ref name=skyandtelescope>{{cite web|url=https://www.skyandtelescope.com/observing/ngc-2346-bi-polar-nebula-with-a-peek-a-boo-star030220160203/|title=NGC 2346: A Cosmic Butterfly Plays Peekaboo|accessdate=2019-08-25|date=2016-03-02|piblisher=skyandtelescope.com|author=Bob King}}</ref> The nebula is sometimes called the "Butterfly nebula," though this more commonly refers to [[Butterfly nebula|NGC 6302]].
The nebula is thought to lie about 2,300 [[light year]]s away.<ref name=spacetelescope/> It has an apparent diameter of 0.910 [[arcminute]]s which corresponds to a physical size of roughly one third of a light year across. The nebula is a bipolar planetary nebula meaning it has two large protrusions or lobes pointing in opposite directions. large clumps of material as well as a [[torus|toriodal]] structure have been observed in the nebula.<ref name=Manchado>
{{cite journal
|last1=Manchado |first1=L.
|last2=Stanghellini |first2=E.
|last3=Villaver |first3=E.
|last4=Garcia-Segura |first4=G.
|last5=Shaw |first5=R. A.
|last6=Garcia-Hernandez |first6=D. A.
|display-authors=3
|title=High resolution imaging of NGC 2346 with GSAOI/GeMS: disentangling the planetary nebula molecular structure to understand its origin and evolution
|journal=The Astrophysical Journal
|volume=808
|issue=2|page=|date=2015
|doi=10.1088/0004-637X/808/2/115
|bibcode=2015ApJ...808..115M
|ref=harv
}} {{arXiv|1506.03712}}
</ref>
==Binary star system==
The [[star]]s at the nebula's core orbit each other every 15.99 days with a separation estimated between 0.159-0.167 [[AU]] or 34.2-35.7 solar radii.<ref name=Kato>
{{cite journal
|last1=Kato |first1=T.
|last2=Nogami |first2=D.
|last3=Baba |first3=H.
|title=The 1996-1997 Fading of V651 Mon, the Binary Central Star of the Planetary Nebula NGC 2346
|journal=Publications of the Astronomical Society of Japan
|volume=53
|issue=5|page=901–904|date=2001
|doi=10.1093/pasj/53.5.901
|bibcode=
|ref=harv
}} {{arXiv|astro-ph/0112304}}
</ref> The binary system has a combined apparent magnitude of +11.<ref name=skyandtelescope/> The first star in the system is a A5V subdwarf star with a mass 1.8 times that of the [[Sun]] and a [[luminosity]] 18 times larger.<ref name=Manchado/> It has a surface temperature of 8,000 kelvin, making it slightly hotter than the Sun's surface. The other star is thought to be a [[white dwarf]] star with a surface temperature in excess of 100,000 kelvin.
The two stars form a [[variable star]], thought to be caused by dust surrounding the stars' occasionally dimming their light.<ref name=skyandtelescope/> Early photographic plates of the stars suggest their light was steady from 1899 until 1981 when it suddenly dropped, reducing the apparent magnitude of the two stars to +15. It then regularly varied between +15 and +11 with its usual period of 16 days. It is thought to be because the brighter of the two stars would periodically be hidden by a cloud in front of the nebula, estimated at perhaps 12 to 30 million miles across.<ref name=skyandtelescope/> This lasted until 1985 when the star's brightness recovered. In 1996 the star experienced another such dimming though to be caused for similar reasons that lasted for around 400 days. Yet another such dimming occurred in 2004.
==References==
{{reflist}}
{{Nebulae}}
[[Category:Astronomy]]
[[Category:Nebulae]]