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|name = Barnard 68
|name = Barnard 68
|image = Barnard 68.jpg
|image = Barnard 68.jpg
|caption = Image of Barnard 68 in visible and near-infrared light. This image is sometimes mistakenly attributed to the [[Boötes Void]].
|caption =
|type = Bok globule
|type = Bok globule
|type2 = [[dark nebula]]
|type2 = [[dark nebula]]
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|names = Barnard 68, LDN 57
|names = Barnard 68, LDN 57
|dist_pc=125<ref name="de Geus"/>}}
|dist_pc=125<ref name="de Geus"/>}}
'''Barnard 68''' is a [[molecular cloud]], dark [[absorption nebula]] or [[Bok globule]], towards the southern constellation [[Ophiuchus]] and well within the [[Milky Way]] galaxy at a distance of about 125 parsecs (407 lightyears).<ref name="de Geus">{{Cite journal |last1=de Geus |first1=E.J. |last2=de Zeeuw |first2=P.T. |last3=Lub |first3=J. |date=June 1989 |title=Physical parameters of stars in the Scorpio-Centaurus OB association |url=https://scholarlypublications.universiteitleiden.nl/access/item%3A2728265/view |journal=Astronomy and Astrophysics |volume=216}}</ref> It is both close and dense enough that stars behind it cannot be seen from Earth. American astronomer [[Edward Emerson Barnard]] added this nebula to his catalog of [[dark nebulae]] in 1919. His catalog was published in 1927, at which stage it included some [[List of dark nebulae|350 objects]]. Because of its opacity, its interior is extremely cold, its temperature being about 16 K (&minus;257&nbsp;°C/-431&nbsp;°F). Its mass is about twice that of the Sun and it measures about half a light-year across.<ref name="APOD">{{cite web|url=http://apod.nasa.gov/apod/ap990511.html|title=Astronomy Picture of the Day - 11 May 1999 - Barnard 68|date=1999-05-11|publisher=[[NASA]]|accessdate=2009-03-01| archiveurl= https://web.archive.org/web/20090411164807/http://apod.nasa.gov/apod/ap990511.html| archivedate= 11 April 2009 | url-status= live}}</ref>
'''Barnard 68''' is a [[molecular cloud]], dark [[absorption nebula]] or [[Bok globule]], towards the southern constellation [[Ophiuchus]] and well within the [[Milky Way]] galaxy at a distance of about 125 parsecs (407 lightyears).<ref name="de Geus">{{Cite journal |last1=de Geus |first1=E.J. |last2=de Zeeuw |first2=P.T. |last3=Lub |first3=J. |date=June 1989 |title=Physical parameters of stars in the Scorpio-Centaurus OB association |url=https://scholarlypublications.universiteitleiden.nl/access/item%3A2728265/view |journal=Astronomy and Astrophysics |volume=216|page=44 |bibcode=1989A&A...216...44D }}</ref> It is both close and dense enough that stars behind it cannot be seen from Earth. American astronomer [[Edward Emerson Barnard]] added this nebula to his catalog of [[dark nebulae]] in 1919. His catalog was published in 1927, at which stage it included some [[List of dark nebulae|350 objects]]. Because of its opacity, its interior is extremely cold, its temperature being about 16 K (&minus;257&nbsp;°C/-431&nbsp;°F). Its mass is about twice that of the Sun and it measures about half a light-year across.<ref name="APOD">{{cite web|url=http://apod.nasa.gov/apod/ap990511.html|title=Astronomy Picture of the Day - 11 May 1999 - Barnard 68|date=1999-05-11|publisher=[[NASA]]|accessdate=2009-03-01| archiveurl= https://web.archive.org/web/20090411164807/http://apod.nasa.gov/apod/ap990511.html| archivedate= 11 April 2009 | url-status= live}}</ref>


==Characteristics==
==Characteristics==
Despite being opaque at visible-light wavelengths, use of the [[Very Large Telescope]] at [[Cerro Paranal]] has revealed the presence of about 3,700 blocked background Milky Way stars, some 1,000 of which are visible at infrared wavelengths.<ref>{{cite web |url=http://www.eso.org/public/images/eso9934b/ |title= The Dark Cloud B68 at Different Wavelengths |publisher= [[European Southern Observatory]]|accessdate= January 30, 2012}}</ref> Careful measurements of the degree of obscuration resulted in a finely sampled and accurate mapping of the dust distribution inside the cloud.<ref>
Despite being opaque at visible-light wavelengths, use of the [[Very Large Telescope]] at [[Cerro Paranal]] has revealed the presence of about 3,700 obscured background Milky Way stars, some 1,000 of which are only visible at infrared wavelengths.<ref>{{cite web |url=http://www.eso.org/public/images/eso9934b/ |title= The Dark Cloud B68 at Different Wavelengths |publisher= [[European Southern Observatory]]|accessdate= January 30, 2012}}</ref> Careful measurements of the degree of obscuration resulted in a finely sampled and accurate mapping of the dust distribution inside the cloud.<ref>
{{cite journal
{{cite journal
|title=Seeing the light through the dark
|title=Seeing the light through the dark
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|bibcode = 2012A&A...547A..11N |display-authors=etal
|bibcode = 2012A&A...547A..11N |display-authors=etal
|volume=547
|volume=547
|pages=A11|s2cid=40817221 }}</ref> Having a dark cloud in the [[solar neighborhood]] greatly facilitates observation and measurement. If not disrupted by external forces, the stability of dust clouds is a fine balance between outward pressure caused by the [[Hydrostatic equilibrium|heat or pressure]] of the cloud's contents, and inward gravitational forces generated by the same particles (see [[Jeans instability]] and [[Bonnor–Ebert mass]]). This causes the cloud to wobble or oscillate in a manner not unlike that of a large soap bubble or a water-filled balloon which is jiggled. In order for the cloud to become a star, gravity must gain the upper hand long enough to cause the cloud to collapse and reach a temperature and density where [[Nuclear fusion|fusion]] can be sustained. When this happens, the much smaller size of the star's envelope signals a new balance between greatly increased gravity and radiation pressure.<ref>
|pages=A11|s2cid=40817221 }}</ref> Having a dark cloud in the [[solar neighborhood]] greatly facilitates observation and measurement. If not disrupted by external forces, the stability of dust clouds is a fine balance between outward pressure caused by the [[Hydrostatic equilibrium|heat or pressure]] of the cloud's contents, and inward gravitational forces generated by the same particles (see [[Jeans instability]] and [[Bonnor–Ebert mass]]). This causes the cloud to wobble or oscillate in a manner like that of a large soap bubble or a water-filled balloon which is jiggled. In order for the cloud to become a star, gravity must gain the upper hand long enough to cause the cloud to collapse and reach a temperature and density where [[Nuclear fusion|fusion]] can be sustained. When this happens, the much smaller size of the star's envelope signals a new balance between greatly increased gravity and radiation pressure.<ref>
{{cite journal
{{cite journal
|last1= Redman|first1=Matt P.
|last1= Redman|first1=Matt P.
Line 69: Line 69:
|arxiv = astro-ph/0604056
|arxiv = astro-ph/0604056
|doi=10.1111/j.1745-3933.2006.00172.x
|doi=10.1111/j.1745-3933.2006.00172.x
|doi-access=free
|s2cid=7654075
|s2cid=7654075
}}</ref>
}}</ref>
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The cloud's mass is about twice that of the Sun, and it measures about half a light-year across.<ref name="APOD"/> Barnard 68's well-defined edges and other features show that it is on the verge of gravitational collapse followed by becoming a star within the next 200,000 years or so.<ref name="BurkertAlves2009">{{cite journal|last1=Burkert|first1=Andreas|last2=Alves|first2=João|title=The Inevitable Future of the Starless Core Barnard 68 |journal=The Astrophysical Journal|volume=695|issue=2|year=2009|pages=1308–1314|issn=0004-637X|doi=10.1088/0004-637X/695/2/1308|arxiv = 0809.1457 |bibcode = 2009ApJ...695.1308B |s2cid=18851013 }}</ref>
The cloud's mass is about twice that of the Sun, and it measures about half a light-year across.<ref name="APOD"/> Barnard 68's well-defined edges and other features show that it is on the verge of gravitational collapse followed by becoming a star within the next 200,000 years or so.<ref name="BurkertAlves2009">{{cite journal|last1=Burkert|first1=Andreas|last2=Alves|first2=João|title=The Inevitable Future of the Starless Core Barnard 68 |journal=The Astrophysical Journal|volume=695|issue=2|year=2009|pages=1308–1314|issn=0004-637X|doi=10.1088/0004-637X/695/2/1308|arxiv = 0809.1457 |bibcode = 2009ApJ...695.1308B |s2cid=18851013 }}</ref>


The cloud is often confused with [[Boötes Void]] although the two have nothing in common, and pictures of Barnard 68 are often erroneously used to illustrate articles about Boötes void.<ref>{{cite news|last=Felton|first=James|date=1 August 2022|title=A Giant Hole In The Universe: Just What Is The Boötes Void?|url=https://www.iflscience.com/a-giant-hole-in-the-universe-just-what-is-the-botes-void-64689|work=IFLScience|access-date=11 September 2023|quote=...Barnard 68, which – if the Internet is to be believed (which it's not) – is 'an empty void in space so big that if you traveled across it you wouldn’t bump into anything for 752,536,988 years'.}}</ref>
The cloud is often confused with the [[Boötes Void]], although the two have nothing in common. Pictures of Barnard 68 are often erroneously used to illustrate articles about the Boötes void.<ref>{{cite news|last=Felton|first=James|date=1 August 2022|title=A Giant Hole In The Universe: Just What Is The Boötes Void?|url=https://www.iflscience.com/a-giant-hole-in-the-universe-just-what-is-the-botes-void-64689|work=IFLScience|access-date=11 September 2023|quote=...Barnard 68, which – if the Internet is to be believed (which it's not) – is 'an empty void in space so big that if you traveled across it you wouldn’t bump into anything for 752,536,988 years'.}}</ref>


==See also==
==See also==
*[[Formation and evolution of the Solar System]]
*[[Formation and evolution of the Solar System]]
*[[Dark_Horse_(astronomy)|Dark Horse Nebula]]


==References==
==References==

Latest revision as of 18:51, 19 November 2024

Barnard 68
Molecular cloud
Bok globule
dark nebula
Image of Barnard 68 in visible and near-infrared light. This image is sometimes mistakenly attributed to the Boötes Void.
Observation data: J2000.0[1] epoch
Right ascension17h 22m 38.2s[1]
Declination−23° 49′ 34″[1]
Distance125[2] pc
ConstellationOphiuchus[3]
Physical characteristics
Radius0.25[3] ly
DesignationsBarnard 68, LDN 57
See also: Lists of nebulae

Barnard 68 is a molecular cloud, dark absorption nebula or Bok globule, towards the southern constellation Ophiuchus and well within the Milky Way galaxy at a distance of about 125 parsecs (407 lightyears).[2] It is both close and dense enough that stars behind it cannot be seen from Earth. American astronomer Edward Emerson Barnard added this nebula to his catalog of dark nebulae in 1919. His catalog was published in 1927, at which stage it included some 350 objects. Because of its opacity, its interior is extremely cold, its temperature being about 16 K (−257 °C/-431 °F). Its mass is about twice that of the Sun and it measures about half a light-year across.[3]

Characteristics

[edit]

Despite being opaque at visible-light wavelengths, use of the Very Large Telescope at Cerro Paranal has revealed the presence of about 3,700 obscured background Milky Way stars, some 1,000 of which are only visible at infrared wavelengths.[4] Careful measurements of the degree of obscuration resulted in a finely sampled and accurate mapping of the dust distribution inside the cloud.[5][6] Observations obtained with Herschel Space Observatory were able to constrain the distribution of the dust component and its temperature even more.[7] Having a dark cloud in the solar neighborhood greatly facilitates observation and measurement. If not disrupted by external forces, the stability of dust clouds is a fine balance between outward pressure caused by the heat or pressure of the cloud's contents, and inward gravitational forces generated by the same particles (see Jeans instability and Bonnor–Ebert mass). This causes the cloud to wobble or oscillate in a manner like that of a large soap bubble or a water-filled balloon which is jiggled. In order for the cloud to become a star, gravity must gain the upper hand long enough to cause the cloud to collapse and reach a temperature and density where fusion can be sustained. When this happens, the much smaller size of the star's envelope signals a new balance between greatly increased gravity and radiation pressure.[8]

The cloud's mass is about twice that of the Sun, and it measures about half a light-year across.[3] Barnard 68's well-defined edges and other features show that it is on the verge of gravitational collapse followed by becoming a star within the next 200,000 years or so.[9]

The cloud is often confused with the Boötes Void, although the two have nothing in common. Pictures of Barnard 68 are often erroneously used to illustrate articles about the Boötes void.[10]

See also

[edit]

References

[edit]
  1. ^ a b c "LDN 57". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-03-01.
  2. ^ a b de Geus, E.J.; de Zeeuw, P.T.; Lub, J. (June 1989). "Physical parameters of stars in the Scorpio-Centaurus OB association". Astronomy and Astrophysics. 216: 44. Bibcode:1989A&A...216...44D.
  3. ^ a b c d "Astronomy Picture of the Day - 11 May 1999 - Barnard 68". NASA. 1999-05-11. Archived from the original on 11 April 2009. Retrieved 2009-03-01.
  4. ^ "The Dark Cloud B68 at Different Wavelengths". European Southern Observatory. Retrieved January 30, 2012.
  5. ^ Alves, João; Lada, Charles; Lada, Elizabeth (March 2001). "Seeing the light through the dark" (PDF). The Messenger. 103: 15–20. Bibcode:2001Msngr.103....1A.
  6. ^ Alves, João F.; Lada, Charles J.; Lada, Elizabeth A. (January 2001). "Internal structure of a cold dark molecular cloud inferred from the extinction of background starlight". Nature. 409 (6817): 159–161. Bibcode:2001Natur.409..159A. doi:10.1038/35051509. PMID 11196632. S2CID 4318459.
  7. ^ Nielbock, Markus; Launhardt, Ralf; Steinacker, Jürgen; et al. (August 2012). "The Earliest Phases of Star formation observed with Herschel (EPoS): The dust temperature and density distributions of B68". Astronomy and Astrophysics. 547: A11. arXiv:1208.4512. Bibcode:2012A&A...547A..11N. doi:10.1051/0004-6361/201219139. S2CID 40817221.
  8. ^ Redman, Matt P.; Keto, Eric; Rawlings, J. M. C. (July 2006). "Oscillations in the stable starless core Barnard". Monthly Notices of the Royal Astronomical Society. 370 (1): L1–L5. arXiv:astro-ph/0604056. Bibcode:2006MNRAS.370L...1R. doi:10.1111/j.1745-3933.2006.00172.x. S2CID 7654075.
  9. ^ Burkert, Andreas; Alves, João (2009). "The Inevitable Future of the Starless Core Barnard 68". The Astrophysical Journal. 695 (2): 1308–1314. arXiv:0809.1457. Bibcode:2009ApJ...695.1308B. doi:10.1088/0004-637X/695/2/1308. ISSN 0004-637X. S2CID 18851013.
  10. ^ Felton, James (1 August 2022). "A Giant Hole In The Universe: Just What Is The Boötes Void?". IFLScience. Retrieved 11 September 2023. ...Barnard 68, which – if the Internet is to be believed (which it's not) – is 'an empty void in space so big that if you traveled across it you wouldn't bump into anything for 752,536,988 years'.
[edit]
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