Boomerang Nebula: Difference between revisions
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*WKK98 (Woudt+[[Renée C. Kraan-Korteweg|Kraan-Korteweg]]+) 1328 <ref name=SIMBADIRAS+12419-5414/> }} | *WKK98 (Woudt+[[Renée C. Kraan-Korteweg|Kraan-Korteweg]]+) 1328 <ref name=SIMBADIRAS+12419-5414/> }} | ||
The '''Boomerang Nebula''' ([[canonical]] name <ref name=WakelyHoran/>) is a | The '''Boomerang Nebula''' ([[canonical]] name <ref name=WakelyHoran/>) is a bipolar reflection<ref name=101093mnras1932321>{{Cite journal|last1=Taylor|first1= K. N. R.|last2=Scarrott|first2=S. M.|date=28 December 1979 |title=The Boomerang Nebula - A highly polarized bipolar |url=https://www.researchgate.net/publication/234324617 |journal=Monthly Notices of the Royal Astronomical Society|volume=193|issue=2 |page=322|doi=10.1093/mnras/193.2.321|doi-access= free|publication-date=October 1980|archive-url=https://archive.today/20250329125123/https://www.researchgate.net/publication/234324617_The_Boomerang_Nebula_-_A_highly_polarized_bipolar|archive-date=29 March 2025}}</ref><ref name=Bolles''Scattered''>{{cite web|author=Dana Bolles|url=https://science.nasa.gov/asset/hubble/scattered-light-from-the-boomerang-nebula/|website=science.nasa.gov|title=Scattered Light from the Boomerang Nebula|date=28 March 2025 | ||
|publisher=NASA|access-date=|url-status=|archive-url=|archive-date=}}</ref> | |publisher=NASA|access-date=|url-status=|archive-url=|archive-date=}}</ref> young planetary [[nebula]]<ref>{{Cite web|url=http://apod.nasa.gov/apod/ap071228.html|title=APOD: 2007 December 28 - A Beautiful Boomerang Nebula}}</ref> located approximately 5,000 [[light-year]]s from [[Earth]] in the constellation [[Centaurus]].<ref name=Bolles''Scattered''/><ref>{{cite web|url=https://noirlab.edu/public/education/constellations/centaurus/|website=noirlab.edu|title=88 Constellations|date=|publisher=NSF NOIRLab (U.S. National Science Foundation National Optical-Infrared Astronomy Research Laboratory)|access-date=3 April 2025|url-status=|archive-url=|archive-date=}}</ref> | ||
Holmberg & Lauberts ([[Uppsala Observatory]]) and Schuster & West ([[European Southern Observatory]] (ESO)) <ref>{{Cite journal|last1=Holmberg|first1=E. B.|last2=Lauberts |first2=A.|last3=Schuster|first3= H.-E.|last4=West |first4=R. M.|url=https://adsabs.harvard.edu/full/1977A&AS...27..295H|date=1977 |title=The ESO/Uppsala survey of the ESO (B) Atlas of the Southern Sky. IV.|journal=Astronomy and Astrophysics Supplement|volume=27|page=295 |bibcode=1977A&AS...27..295H|access-date=29 March 2025}}</ref> in their survey of 1976 or earlier discovered the existence of an object at the location.<ref name=101093mnras1932321/> Before or during 1978 I.S. Glass <ref name=1979MNRAS> | Holmberg & Lauberts ([[Uppsala Observatory]]) and Schuster & West ([[European Southern Observatory]] (ESO)) <ref>{{Cite journal|last1=Holmberg|first1=E. B.|last2=Lauberts |first2=A.|last3=Schuster|first3= H.-E.|last4=West |first4=R. M.|url=https://adsabs.harvard.edu/full/1977A&AS...27..295H|date=1977 |title=The ESO/Uppsala survey of the ESO (B) Atlas of the Southern Sky. IV.|journal=Astronomy and Astrophysics Supplement|volume=27|page=295 |bibcode=1977A&AS...27..295H|access-date=29 March 2025}}</ref> in their survey of 1976 or earlier discovered the existence of an object at the location.<ref name=101093mnras1932321/> Before or during 1978 I.S. Glass <ref name=1979MNRAS> | ||
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|publisher = [[Chalmers University of Technology]] | |publisher = [[Chalmers University of Technology]] | ||
|access-date = | |access-date = | ||
}}</ref> with G. Wegner,<ref name=SALÉR-RAMBERG/><ref name=1979MNRAS/> both of [[South African Astronomical Observatory]], from data of the [[ESO]] Quick Blue Survey.<ref name=1979MNRAS/> Wegner and Glass in their paper of 1979 mentioned a "butterfly" or "bow-tie" like shape.<ref name=1979MNRAS/> K. N. R. Taylor ([[University of New South Wales]]) and S. M. Scarrott ([[Durham University]]) made observations July 17, 1979 and named it after the [[boomerang]].<ref name=101093mnras1932321/> Modelling of measurements of outflow of the nebula published 1997 by Sahai ([[Jet Propulsion Laboratory]]) and Nyman (ESO & [[Onsala Space Observatory]]) indicate [[kelvin]] (K) less than [[microwave background|cosmic microwave background radiation]] (cmbr), so the | }}</ref> with G. Wegner,<ref name=SALÉR-RAMBERG/><ref name=1979MNRAS/> both of [[South African Astronomical Observatory]], from data of the [[ESO]] Quick Blue Survey.<ref name=1979MNRAS/> Wegner and Glass in their paper of 1979 mentioned a "butterfly" or "bow-tie" like shape.<ref name=1979MNRAS/> K. N. R. Taylor ([[University of New South Wales]]) and S. M. Scarrott ([[Durham University]]) made observations July 17, 1979 and named it after the [[boomerang]].<ref name=101093mnras1932321/> Modelling of measurements of outflow of the nebula published 1997 by Sahai ([[Jet Propulsion Laboratory]]) and Nyman (ESO & [[Onsala Space Observatory]]) indicate [[kelvin]] (K) less than [[microwave background|cosmic microwave background radiation]] (cmbr), so it's the [[Orders of magnitude (temperature)|coldest natural place currently known]]<ref name="Sahai & Nyman, 1997">{{cite journal |last1=Sahai |first1=Raghvendra |last2=Nyman |first2=Lars-Åke |year=1997 |title=The Boomerang Nebula: The Coolest Region of the Universe?|journal=The Astrophysical Journal |volume=487 |issue=2 |pages=L155–L159 |doi=10.1086/310897 |bibcode=1997ApJ...487L.155S |hdl=2014/22450|doi-access=free|quote='''L156''': We have measured a 9 mK upper limit (3 σ) on continuum emission at 89.2 and 145.6 GHz toward the Boomerang Nebula, which is much smaller than the negative temperatures seen in the CO and <sup>13</sup>CO ''J'' 1–0 spectra, so these must result from absorption of the microwave background, requiring the excitation temperature (''T''<sub>ex</sub>) to be less than 2.8 [[Kelvin|K]] (''T''<sub>bb</sub>). '''3. A TWO–SHELL MODEL''' In shell 2 (''R''<sub>1</sub>,''<sub>o</sub>'' < ''r'' < ''R''<sub>2</sub>), ''T''<sub>kin</sub> < 2.8 K." "1994-1995 :2. OBSERVATIONS AND RESULTS}}</ref> in the [[Observed universe|observed Universe]]. | ||
The central star is | The central star is an old star. The [[Star#Temperature|max-diametrical temperature]] of the central star is estimated to be 6000 K (by Wegner and Glass <ref name=1991A&A242247B>{{Cite journal|last1=Bujarrabal |first1=V.|last2=Bachiller |first2=R.|location=ESO |date=1 February 1991|url=https://articles.adsabs.harvard.edu//full/1991A%26A...242..247B/0000251.000.html|title= CO observations of southern protoplanetary nebulae with optical counterparts|journal=Astronomy and Astrophysics|volume=242|issue= 1|pages=251|issn=0004-6361 |bibcode=1991A&A...242..247B|access-date=30 March 2025}}</ref> 1978 or earlier) <ref name=1979MNRAS/> or 7000 K (Bujarrabal & Bachiller before July 1990).<ref name=1991A&A242247B/> | ||
The Boomerang Nebula is believed to be a [[star system]] evolving toward the [[planetary nebula]] phase. It continues to form and develop due to the outflow of gas from its core where a star in its late stage life sheds mass and emits starlight, illuminating dust in the nebula. [[Millimeter]] scale dust grains obscure portions of the nebula's center, so most escaping visible [[light]] is in two opposing lobes forming a distinctive hourglass shape as viewed by [[space telescope]] data on Earth. The outflowing gas at about 164 [[km/s]] expands rapidly into space; this gas expansion results in the nebula's unusual K. | The Boomerang Nebula is believed to be a [[star system]] evolving toward the [[planetary nebula]] phase. It continues to form and develop due to the outflow of gas from its core where a star in its late stage life sheds mass and emits starlight, illuminating dust in the nebula. [[Millimeter]] scale dust grains obscure portions of the nebula's center, so most escaping visible [[light]] is in two opposing lobes forming a distinctive hourglass shape as viewed by [[space telescope]] data on Earth. The outflowing gas at about 164 [[km/s]] expands rapidly into space; this gas expansion results in the nebula's unusual K. | ||
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* [http://www.esa.int/esaSC/Pr_1_2003_h_en.html The Boomerang Nebula - The Coolest Place in the Universe?], [[European Space Agency|ESA]], 20 February 2003 | * [http://www.esa.int/esaSC/Pr_1_2003_h_en.html The Boomerang Nebula - The Coolest Place in the Universe?], [[European Space Agency|ESA]], 20 February 2003 | ||
* [http://www.universetoday.com/am/publish/scattered_light_from_boomerang.html Hubble's View of the Boomerang Nebula], 13 September 2005; see also [http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/25/image/a Scattered Light from the Boomerang Nebula] | * [http://www.universetoday.com/am/publish/scattered_light_from_boomerang.html Hubble's View of the Boomerang Nebula], 13 September 2005; see also [http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/25/image/a Scattered Light from the Boomerang Nebula] | ||
* [ | * [https://www.spacetelescope.org/news/html/heic0301.html ESA/Hubble-Boomerang Nebula] | ||
* [http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Boomerang+Nebula SIMBAD], Coordinates and Scientific data. January 4, 2007. | * [http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Boomerang+Nebula SIMBAD], Coordinates and Scientific data. January 4, 2007. | ||
Latest revision as of 14:15, 28 September 2025
Template:Short description Template:Infobox nebula
The Boomerang Nebula (canonical name [1]) is a bipolar reflection[2][3] young planetary nebula[4] located approximately 5,000 light-years from Earth in the constellation Centaurus.[3][5]
Holmberg & Lauberts (Uppsala Observatory) and Schuster & West (European Southern Observatory (ESO)) [6] in their survey of 1976 or earlier discovered the existence of an object at the location.[2] Before or during 1978 I.S. Glass [7] discovered the object as a nebula [8] with G. Wegner,[8][7] both of South African Astronomical Observatory, from data of the ESO Quick Blue Survey.[7] Wegner and Glass in their paper of 1979 mentioned a "butterfly" or "bow-tie" like shape.[7] K. N. R. Taylor (University of New South Wales) and S. M. Scarrott (Durham University) made observations July 17, 1979 and named it after the boomerang.[2] Modelling of measurements of outflow of the nebula published 1997 by Sahai (Jet Propulsion Laboratory) and Nyman (ESO & Onsala Space Observatory) indicate kelvin (K) less than cosmic microwave background radiation (cmbr), so it's the coldest natural place currently known[9] in the observed Universe.
The central star is an old star. The max-diametrical temperature of the central star is estimated to be 6000 K (by Wegner and Glass [10] 1978 or earlier) [7] or 7000 K (Bujarrabal & Bachiller before July 1990).[10]
The Boomerang Nebula is believed to be a star system evolving toward the planetary nebula phase. It continues to form and develop due to the outflow of gas from its core where a star in its late stage life sheds mass and emits starlight, illuminating dust in the nebula. Millimeter scale dust grains obscure portions of the nebula's center, so most escaping visible light is in two opposing lobes forming a distinctive hourglass shape as viewed by space telescope data on Earth. The outflowing gas at about 164 km/s expands rapidly into space; this gas expansion results in the nebula's unusual K.
Using observations from 1994 and 1995 with the 15-metre Swedish-ESO Submillimetre Telescope in Chile, the astronomers Sahai & Nyman concluded carbon monoxide (CO) molecules produced after stellar co-absorption in a binary system of the nebula which outflow as a gas wind were less kinetically excited than the local outer space (cmbr).Template:Efn Radiation transfer of cmbr into the CO parts Template:Efn of the nebula wind indicated those parts onlyTemplate:Efn must have a kelvin temperature state which is uniquely the least of any observed location in nature.[9][11]
The kinetic energy (KE) of the CO outflow is theorized Template:Efn as the product of common-envelope evolution,[12] which was a change in the outer environment (an envelope) of the dual orbital system of the binary system.[13] The KE within the outflow is theorized as an environment forced out from the area of the orbital system of the larger star by the absorption of the lesser sized star into the core of the larger by terminal gravitational attraction.[12] Cooling to sub cmbr temperature is by adiabatic expansion.[14]
A succession of periodic observations from November 2011 (Atacama Large Millimeter Array) ending June 2012 (Australia Telescope Compact Array) with archived observations from Hubble (HST) (1998 & 2005) [14] revealed other features.[15] The nebula's visible double lobe was observed to be surrounded by a larger spherical region of cold gas seen only in sub-millimeter radio wavelengths. The nebula's outer fringes appear to be gradually warming.
As of mid-2017, it is believed that the star at the center of the nebula is a dying red giant.[16][17]
Gallery
ALMA (2017)
HST
-
Imaged using polarizing filters (analogous to polarized sunglasses) and color-coded by the angle associated with the polarized light.
-
Red filter applied to monochromatic data
Notes
References
External links
- NRAO Boomerang Nebula
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- The Boomerang Nebula - The Coolest Place in the Universe?, ESA, 20 February 2003
- Hubble's View of the Boomerang Nebula, 13 September 2005; see also Scattered Light from the Boomerang Nebula
- ESA/Hubble-Boomerang Nebula
- SIMBAD, Coordinates and Scientific data. January 4, 2007.
Template:Stars of Centaurus Template:Portal bar
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