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{{Short description|Star in the constellation Crux}}
{{Starbox begin
{{Starbox begin
| name=DU Crucis
| name=DU Crucis
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}}
}}
{{Starbox detail
{{Starbox detail
| source=<ref name="Healy2023">{{Cite journal |last=Healy |first=Sarah |last2=Horiuchi |first2=Shunsaku |last3=Molla |first3=Marta Colomer |last4=Milisavljevic |first4=Dan |last5=Tseng |first5=Jeff |last6=Bergin |first6=Faith |last7=Weil |first7=Kathryn |last8=Tanaka |first8=Masaomi |date=2024-03-23 |title=Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova |bibcode=2024MNRAS.529.3630H |doi-access=free|journal=Monthly Notices of the Royal Astronomical Society |volume=529 |issue=4 |pages=3630–3650 |doi=10.1093/mnras/stae738 |issn=0035-8711|arxiv=2307.08785 }}</ref>
| source=<ref name=harris/>
| mass=
| mass=
| radius=664
| radius=598{{efn | name=radius | [[Stefan–Boltzmann law|Calculated]] from effective temperature and luminosity figures, with reference to the nominal solar temperature of 5,772&nbsp;K}}
| luminosity=46,600
| luminosity=69,600
| temperature=3,467
| temperature=3,467<ref name=harris/>
| metal_fe=
| metal_fe=
| gravity=
| gravity=
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}}
}}
{{Starbox end}}
{{Starbox end}}
'''DU Crucis''' is a [[ruby]]-[[red supergiant|colored supergiant]]<ref>{{Cite book|url=https://www.worldcat.org/oclc/795853507|title=Universe.|last=|first=|date=2012|publisher=Dorling Kindersley|year=|isbn=9781409376507|edition= New|location=London|pages=412|oclc=795853507}}</ref> and [[slow irregular variable]] star in the [[open cluster]] [[NGC 4755]], which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.
'''DU Crucis''' is a [[red supergiant]] and [[slow irregular variable]] star in the [[open cluster]] [[NGC 4755]], which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.


==Location==
==Location==
[[File:A Snapshot of the Jewel Box cluster with the ESO VLT.jpg|thumb|left|upright=1.0|A Snapshot of the Jewel Box cluster (Credit: ESO VLT).]]
[[File:A Snapshot of the Jewel Box cluster with the ESO VLT.jpg|thumb|left|upright=1.0|A Snapshot of the Jewel Box cluster (Credit: ESO VLT).]]
DU Crucis is one of the brighter members of the Jewel Box Cluster and the brightest [[red supergiant]], strongly contrasting with the other bright members which are [[blue supergiant]]s.<ref name=kharchenko2004/> It is part of the central bar of the prominent letter "A"-shaped [[Asterism (astronomy)|asterism]] at the centre of the cluster. The cluster is part of the larger Centaurus OB1 association and lies about 8,500 light years away.
DU Crucis is one of the brighter members of the Jewel Box Cluster and the brightest [[red supergiant]], strongly contrasting with the other bright members which are [[blue supergiant]]s.<ref name=kharchenko2004/> It is part of the central bar of the prominent letter A-shaped [[Asterism (astronomy)|asterism]] at the centre of the cluster. The cluster is part of the larger Centaurus OB1 association and lies about 8,500 light years away.


The cluster is just to the south-east of [[Beta Crucis|β Crucis]], the lefthand star of the [[Southern Cross]].
The cluster is just to the south-east of [[Beta Crucis|β Crucis]], the lefthand star of the [[Southern Cross]].


==Properties==
==Properties==
DU Crucis is an M2 intermediate luminosity [[supergiant]] (luminosity class Iab). Despite its low temperature, it is 46,600 times the luminosity of the sun, due to its very large size. The κ Crucis cluster has a calculated age of 11.2 million years.<ref name="aidelman"/>
DU Crucis is an M2 intermediate luminosity [[supergiant]] (luminosity class Iab). Despite its low temperature, it is 46,600 times the luminosity of the sun, due to its very large size. The κ Crucis cluster has a calculated age of 11.2 million years.<ref name="aidelman"/>


{{Clear|left}}
==Variability==
==Variability==
[[File:DUCruLightCurve.png|thumb|left|A [[light curve]] for DU Crucis, plotted from ''[[Hipparcos]]'' data<ref name=HipDataAccess/>]]
Photometry from the [[Hipparcos]] satellite mission showed that DU Crucis varies in brightness with an amplitude of 0.44 magnitudes.<ref name=adelman/> No periodicity could be detected in the variations and it was classified as a slow irregular variable of type Lc, indicating a supergiant.<ref name=gcvs/>
Photometry from the [[Hipparcos]] satellite mission showed that DU Crucis varies in brightness with an amplitude of 0.44 magnitudes.<ref name=adelman/> No periodicity could be detected in the variations and it was classified as a slow irregular variable of type Lc, indicating a supergiant.<ref name=gcvs/>

⚫
==Notes==
{{Notelist}}


==References==
==References==
{{reflist|refs=
{{reflist|refs=


<ref name=HipDataAccess>{{cite web |title=Hipparcos Tools Interactive Data Access |url=https://www.cosmos.esa.int/web/hipparcos/interactive-data-access |website=Hipparcos |publisher=ESA |access-date=8 December 2021}}</ref>
⚫
<ref name=adelman>{{cite journal|bibcode=2001BaltA..10..589A|title=Stars with the Largest Hipparcos Photometric Amplitudes|journal=Baltic Astronomy|volume=10|pages=589|author1=Adelman|first1=Saul J.|year=2001|doi=10.1515/astro-2001-0403}}</ref>

⚫
<ref name=adelman>{{cite journal|bibcode=2001BaltA..10..589A|title=Stars with the Largest Hipparcos Photometric Amplitudes|journal=Baltic Astronomy|volume=10|issue=4|pages=589|last1=Adelman|first1=Saul J.|year=2001|doi=10.1515/astro-2001-0403|doi-access=free}}</ref>


<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>
<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>


<ref name="vanLeeuwen2007">{{citation
<ref name="vanLeeuwen2007">{{citation
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| doi=10.1051/0004-6361:20078357
| doi=10.1051/0004-6361:20078357
| arxiv=0708.1752
| arxiv=0708.1752
| s2cid=18759600
| postscript=.
| postscript=.
}}</ref>
}}</ref>
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| issue= 9
| issue= 9
| pages= 740–748
| pages= 740–748
| author1= Kharchenko
| last1= Kharchenko
| first1= N. V.
| first1= N. V.
| last2= Piskunov
| last2= Piskunov
Line 112: Line 121:
}}</ref>
}}</ref>


<ref name="aidelman">{{cite journal|bibcode=2012A&A...544A..64A|title=Open clusters. I. Fundamental parameters of B stars in NGC 3766 and NGC 4755|journal=Astronomy & Astrophysics|volume=544|pages=A64|author1=Aidelman|first1=Y.|last2=Cidale|first2=L. S.|last3=Zorec|first3=J.|last4=Arias|first4=M. L.|year=2012|doi=10.1051/0004-6361/201219069}}</ref>
<ref name="aidelman">{{cite journal|bibcode=2012A&A...544A..64A|title=Open clusters. I. Fundamental parameters of B stars in NGC 3766 and NGC 4755|journal=Astronomy & Astrophysics|volume=544|pages=A64|last1=Aidelman|first1=Y.|last2=Cidale|first2=L. S.|last3=Zorec|first3=J.|last4=Arias|first4=M. L.|year=2012|doi=10.1051/0004-6361/201219069|doi-access=free|hdl=11336/145136|hdl-access=free}}</ref>


<ref name=corti2013>{{cite journal|bibcode=2013A&A...553A.108C|title=Members of Centaurus OB1 and NGC 4755: New spectroscopic and astrometric studies|journal=Astronomy & Astrophysics|volume=553|pages=A108|author1=Corti|first1=M. A.|last2=Orellana|first2=R. B.|year=2013|doi=10.1051/0004-6361/201220743}}</ref>
<ref name=corti2013>{{cite journal|bibcode=2013A&A...553A.108C|title=Members of Centaurus OB1 and NGC 4755: New spectroscopic and astrometric studies|journal=Astronomy & Astrophysics|volume=553|pages=A108|last1=Corti|first1=M. A.|last2=Orellana|first2=R. B.|year=2013|doi=10.1051/0004-6361/201220743|doi-access=free|hdl=11336/8495|hdl-access=free}}</ref>


<ref name=perkins>{{cite journal|bibcode= 1989ApJS...71..245K |title= The Perkins catalog of revised MK types for the cooler stars |journal= Astrophysical Journal Supplement Series |issn=0067-0049 |volume= 71 |pages= 245 |author1= Keenan |first1= Philip C. |last2= McNeil |first2= Raymond C. |year= 1989 |doi= 10.1086/191373 }}</ref>
<ref name=perkins>{{cite journal|bibcode= 1989ApJS...71..245K |title= The Perkins catalog of revised MK types for the cooler stars |journal= Astrophysical Journal Supplement Series |issn=0067-0049 |volume= 71 |pages= 245 |last1= Keenan |first1= Philip C. |last2= McNeil |first2= Raymond C. |year= 1989 |doi= 10.1086/191373 |s2cid= 123149047 }}</ref>


<ref name=mermilliod>{{cite journal|bibcode=2008A&A...485..303M|title=Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters|journal=Astronomy and Astrophysics|volume=485|pages=303–314|author1=Mermilliod|first1=J. C.|last2=Mayor|first2=M.|last3=Udry|first3=S.|year=2008|doi=10.1051/0004-6361:200809664|citeseerx=10.1.1.30.7545}}</ref>
<ref name=mermilliod>{{cite journal|bibcode=2008A&A...485..303M|title=Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters|journal=Astronomy and Astrophysics|volume=485|issue=1|pages=303–314|last1=Mermilliod|first1=J. C.|last2=Mayor|first2=M.|last3=Udry|first3=S.|year=2008|doi=10.1051/0004-6361:200809664|citeseerx=10.1.1.30.7545}}</ref>


<ref name=dr2>{{cite DR2|6056407605465876352}}</ref>
<ref name=dr2>{{cite DR2|6056407605465876352}}</ref>


<ref name=harris>{{cite journal|bibcode=1976ApJS...30..451H|title=Evolved stars in open clusters|journal=Astrophysical Journal|volume=30|pages=451|author1=Harris|first1=G. L. H.|year=1976|doi=10.1086/190368}}</ref>
<ref name=harris>{{cite journal|bibcode=1976ApJS...30..451H|title=Evolved stars in open clusters|journal=Astrophysical Journal|volume=30|pages=451|last1=Harris|first1=G. L. H.|year=1976|doi=10.1086/190368}}</ref>


}}
}}

⚫
==Notes==
{{notelist}}


==External links==
==External links==
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{{Stars of Crux}}
{{Stars of Crux}}


{{DEFAULTSORT:DU Crucis}}
[[Category:Crux (constellation)]]
[[Category:Crux]]
[[Category:M-type supergiants]]
[[Category:M-type supergiants]]
[[Category:Hipparcos objects|062918]]
[[Category:Hipparcos objects|062918]]
[[Category:Durchmusterung objects]]
[[Category:Durchmusterung objects|CD-59 4459]]
[[Category:2MASS objects]]
[[Category:2MASS objects|J12534132-6020578]]
[[Category:Slow irregular variables]]
[[Category:Slow irregular variables]]
[[Category:IRAS catalogue objects]]
[[Category:IRAS catalogue objects]]

Latest revision as of 20:18, 11 June 2024

DU Crucis

The centre of NGC 4755, with DU Cru at top right
Credit: NASA/ESA and Jesús Maíz Apellániz (Instituto de Astrofísica de Andalucía, Spain)
Observation data
Epoch J2000      Equinox J2000
Constellation Crux
Right ascension 12h 53m 41.33485s[1]
Declination −60° 20′ 57.9647″[1]
Apparent magnitude (V) 7.45[2]
Characteristics
Spectral type M2- Iab[3]
U−B color index +2.57[2]
B−V color index +2.22[2]
Variable type Lc[4]
Astrometry
Radial velocity (Rv)−21.24[5] km/s
Proper motion (μ) RA: −4.703[6] mas/yr
Dec.: −1.162[6] mas/yr
Parallax (π)0.5075 ± 0.0516 mas[6]
Distance2,600[7][8] pc
Absolute magnitude (MV)−5.52[9]
Details[10]
Radius664 R☉
Luminosity69,600 L☉
Temperature3,467[9] K
Other designations
DU Cru, CD−59°4459, HIP 62918, SAO 252073, 2MASS J12534132-6020578, IRAS 12506-6004
Database references
SIMBADdata

DU Crucis is a red supergiant and slow irregular variable star in the open cluster NGC 4755, which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.

Location

[edit]
A Snapshot of the Jewel Box cluster (Credit: ESO VLT).

DU Crucis is one of the brighter members of the Jewel Box Cluster and the brightest red supergiant, strongly contrasting with the other bright members which are blue supergiants.[11] It is part of the central bar of the prominent letter A-shaped asterism at the centre of the cluster. The cluster is part of the larger Centaurus OB1 association and lies about 8,500 light years away.

The cluster is just to the south-east of β Crucis, the lefthand star of the Southern Cross.

Properties

[edit]

DU Crucis is an M2 intermediate luminosity supergiant (luminosity class Iab). Despite its low temperature, it is 46,600 times the luminosity of the sun, due to its very large size. The κ Crucis cluster has a calculated age of 11.2 million years.[7]

Variability

[edit]
A light curve for DU Crucis, plotted from Hipparcos data[12]

Photometry from the Hipparcos satellite mission showed that DU Crucis varies in brightness with an amplitude of 0.44 magnitudes.[13] No periodicity could be detected in the variations and it was classified as a slow irregular variable of type Lc, indicating a supergiant.[4]

Notes

[edit]

References

[edit]
  1. ^ a b van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c Dachs, J.; Kaiser, D. (November 1984), "UBV photometry of the southern galactic cluster NGC 4755 = Kappa Crucis", Astronomy and Astrophysics Supplement Series, 58: 411–429, Bibcode:1984A&AS...58..411D.
  3. ^ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. ISSN 0067-0049. S2CID 123149047.
  4. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ^ Mermilliod, J. C.; Mayor, M.; Udry, S. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy and Astrophysics. 485 (1): 303–314. Bibcode:2008A&A...485..303M. CiteSeerX 10.1.1.30.7545. doi:10.1051/0004-6361:200809664.
  6. ^ a b c 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.
  7. ^ a b Aidelman, Y.; Cidale, L. S.; Zorec, J.; Arias, M. L. (2012). "Open clusters. I. Fundamental parameters of B stars in NGC 3766 and NGC 4755". Astronomy & Astrophysics. 544: A64. Bibcode:2012A&A...544A..64A. doi:10.1051/0004-6361/201219069. hdl:11336/145136.
  8. ^ Corti, M. A.; Orellana, R. B. (2013). "Members of Centaurus OB1 and NGC 4755: New spectroscopic and astrometric studies". Astronomy & Astrophysics. 553: A108. Bibcode:2013A&A...553A.108C. doi:10.1051/0004-6361/201220743. hdl:11336/8495.
  9. ^ a b Harris, G. L. H. (1976). "Evolved stars in open clusters". Astrophysical Journal. 30: 451. Bibcode:1976ApJS...30..451H. doi:10.1086/190368.
  10. ^ Healy, Sarah; Horiuchi, Shunsaku; Molla, Marta Colomer; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (2024-03-23). "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova". Monthly Notices of the Royal Astronomical Society. 529 (4): 3630–3650. arXiv:2307.08785. Bibcode:2024MNRAS.529.3630H. doi:10.1093/mnras/stae738. ISSN 0035-8711.
  11. ^ Kharchenko, N. V.; Piskunov, A. E.; Röser, S.; Schilbach, E.; Scholz, R.-D. (2004). "Astrophysical supplements to the ASCC-2.5. II. Membership probabilities in 520 Galactic open cluster sky areas". Astronomische Nachrichten. 325 (9): 740–748. Bibcode:2004AN....325..740K. doi:10.1002/asna.200410256.
  12. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  13. ^ Adelman, Saul J. (2001). "Stars with the Largest Hipparcos Photometric Amplitudes". Baltic Astronomy. 10 (4): 589. Bibcode:2001BaltA..10..589A. doi:10.1515/astro-2001-0403.
[edit]
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