Acrux

This article is about the star. For the Christian college, see Alphacrucis. For research ship, see Alpha Crucis (research vessel).
Acrux

The position of Acrux
Observation data
Epoch J2000      Equinox J2000
Constellation Crux
Pronunciation /ˈeɪkrʌks/
α Crucis AB
Right ascension 12h 26m 35.89522s[1]
Declination −63° 05′ 56.7343″[1]
Apparent magnitude (V) 0.76[2] (combined)
1.33 (A) + 1.75 (B)[3]
α Crucis C
Right ascension 12h 26m 30.8829s[4]
Declination −63° 07′ 20.047″[4]
Apparent magnitude (V) 4.86 (Ca + Cb)[3]
13.36 (D)[3]
Characteristics
Spectral type B0.5 IV (Aa)[5]
B1 V (B)[5]
B5 V (Ca)[6]
M0 V (D)[3]
U−B color index −0.59 (C)[7]
B−V color index −0.26 (AB)[2]
−0.12 (C)[7]
Variable type β Cep[8][a]
Astrometry
α Crucis AB
Radial velocity (Rv)+19.2±0.8[9] km/s
Proper motion (μ) RA: −35.83[1] mas/yr
Dec.: −14.86[1] mas/yr
Parallax (π)10.13±0.50 mas[1]
Distance348±5 ly
(106.7±1.5 pc)[9]
Absolute magnitude (MV)−3.77[10]
α Crucis C
Radial velocity (Rv)+27[11] km/s
Proper motion (μ) RA: −39.548[4] mas/yr
Dec.: −13.760[4] mas/yr
Parallax (π)9.3964±0.1289 mas[4]
Distance348±5 ly
(106.7±1.5[9] pc)
Absolute magnitude (MV)−0.98[10]
Orbit[9]
Primaryα Crucis Aa
Nameα Crucis Ab
Period (P)75.7469±0.0017 d
Semi-major axis (a)(9.48±0.30)×10−3"
(1.01±0.04 au)
Eccentricity (e)0.369±0.015
Inclination (i)66.2±1.4°
Longitude of the node (Ω)225.0±2.0°
Periastron epoch (T)2,458,183.1±0.4 JD
Argument of periastron (ω)
(secondary)		229.5±2.2°
Semi-amplitude (K1)
(primary)		40.6±0.9 km/s
Orbit[9][b]
Primaryα Crucis Ba
Nameα Crucis Bb
Period (P)405.4+0.4
−0.3 d
Semi-major axis (a)(28.2±0.8)×10−3"
(3.0 au)
Eccentricity (e)0.36+0.45
−0.07
Inclination (i)94.4+2.6
−0.3°
Longitude of the node (Ω)86.0+3.4
−6.1°
Periastron epoch (T)2,458,099+258
−145 JD
Argument of periastron (ω)
(secondary)		105.2+32.1
−55.3°
Orbit[12]
Primaryα Crucis Ca
Nameα Crucis Cb
Period (P)1.225155±0.000005 d
Semi-major axis (a)≥1.044 R☉
Eccentricity (e)0.024±0.014
Periastron epoch (T)2438903.314±0.003 JD
Argument of periastron (ω)
(secondary)		314±34°
Semi-amplitude (K1)
(primary)		43.1±0.6 km/s
Details
α Crucis Aa
Mass17.2±1.2[9] M☉
Radius6.8[9] R☉
Luminosity31,110+3,190
−2,910[8] L☉
Temperature28,950[9] K
Rotational velocity (v sin i)84[9] km/s
Age7.1[9] Myr
α Crucis Ab
Mass6.8±0.3[9] M☉
Radius3.2[9] R☉
Luminosity1,400[c] L☉
Temperature19,750 K
Age7.1[9] Myr
α Crucis Ba
Mass12.4[9] M☉
Radius5.4[9] R☉
Luminosity14,000[c] L☉
Surface gravity (log g)4.00[13] cgs
Temperature26,950[9] K
Rotational velocity (v sin i)200[14] km/s
Age7.1[9] Myr
α Crucis Bb
Mass9.8[9] M☉
Radius4.4[9] R☉
Luminosity6,100[c] L☉
Temperature24,350[9] K
α Crucis Ca
Mass4.5[9] M☉
Radius2.5[9] R☉
Luminosity380[15] L☉
Surface gravity (log g)4.05[15] cgs
Temperature15,900[9] K
Rotational velocity (v sin i)131[16] km/s
α Crucis Cb
Mass≥0.64[9] M☉
α Crucis D
Mass0.5[9] M☉
Age12[17] Myr
Other designations
α Crucis, CPD−62°2745, HIP 60718, CCDM J12266-6306, WDS J12266-6306
α Cru A: Acrux, α1 Crucis, 26 G. Crucis, FK5 462, GC 16952, HD 108248, HR 4730
α Cru B: α2 Crucis, 27 G. Crucis, GC 16953, HD 108249, HR 4731, 2MASS J12263615-6305571
α Cru C: 27 G. Crucis, CPD−62°2742, GC 16951, HD 108250, HR 4729
Database references
SIMBADα Cru
α Crucis A
α Crucis B
α Crucis C

Acrux is a multiple star system the brightest star in the southern constellation of Crux. It has the Bayer designation α Crucis, which is Latinised to Alpha Crucis and abbreviated Alpha Cru or α Cru. With a combined visual magnitude of +0.76, it is the 13th-brightest star in the night sky. It is the most southerly star of the asterism known as the Southern Cross and is the southernmost first-magnitude star, 2.3 degrees more southerly than Alpha Centauri.[18] This system is located at a distance of 348 light-years (106.7 parsecs) from the Sun.[9]

To the naked eye Acrux appears as a single star, but it is actually a multiple star system containing seven components.[9] Through optical telescopes, Acrux appears as a triple star, whose two brightest components are visually separated by about 4 arcseconds and are known as α Cru A and α Cru B, α1 Crucis and α2 Crucis, or α Crucis A and α Crucis B. Both components are B-type stars, and are many times more massive and luminous than the Sun. This system was the second ever to be recognized as a binary, in 1685 by a Jesuit priest.[19] α1 and α2 Crucis are close binaries themselves, with components designated α Crucis Aa (officially named Acrux, historically the name of the entire system)[20][21] α Crucis Ab, α Crucis Ba, and α Crucis Bb.

α Cru C, also known as HR 4729, is a more distant companion, forming a triple star through small telescopes. C is a spectroscopic binary and has a faint companion, which brings the total number of stars in the system to seven.

Nomenclature

α Crucis (Latinised to Alpha Crucis) is the system's Bayer designation; α1 and α2 Crucis, those of its two main components stars. The designations of these two constituents as α Cru A and α Cru B and those of A's components—α Cru Aa and α Cru Ab—derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[22]

The historical name Acrux for α1 Crucis is an "Americanism" coined in the 19th century, but entering common use only by the mid 20th century.[23] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[24] to catalog and standardize proper names for stars. The WGSN states that in the case of multiple stars the name should be understood to be attributed to the brightest component by visual brightness.[25] The WGSN approved the name Acrux for the star α Cru Aa on 20 July 2016 and it is now so entered in the IAU Catalog of Star Names.[21]

Since Acrux is at −63° declination, making it the southernmost first-magnitude star, it is only visible south of latitude 27° North. It barely rises from cities such as Miami, United States, or Karachi, Pakistan (both around 25°N) and not at all from New Orleans, United States, or Cairo, Egypt (both about 30°N). Because of Earth's axial precession, the star was visible to ancient Hindu astronomers in India who named it Tri-shanku. It was also visible to the ancient Romans and Greeks, who regarded it as part of the constellation of Centaurus.[26]

In Chinese, 十字架 (Shí Zì Jià, "Cross"), refers to an asterism consisting of Acrux, Mimosa, Gamma Crucis and Delta Crucis.[27] Consequently, Acrux itself is known as 十字架二 (Shí Zì Jià èr, "the Second Star of Cross").[28]

This star is known as Estrela de Magalhães ("Star of Magellan") in Portuguese.[29]

Stellar properties

Aa
Period = 75.75 d
Ab
Period ≈ 1,300 yr
Ba
Period = 405 d
Bb
Period ≈ 130,000 yr
Ca
Period = 1.22 d
Cb
Period ≈ 1,500 yr
D

Hierarchy of orbits in the system[9]

α Crucis AB

The two innermost visual components of Acrux are α Crucis A (α1 Crucis) and α Crucis B (α2 Crucis),[9] separated by 3.9". α1 is magnitude 1.33 whereas α2 is magnitude 1.75.[3] Spectral types of B0.5 IV and B1 V have been assigned for the components, showing that they are hot B-type stars.[5] They orbit over such a long period that motion is only barely seen.[3] From their projected separation of 430 astronomical units, the period is estimated to be around 1,300 years.[9] α1 and α2 are binaries themselves, with α1 being a single-lined spectroscopic binary[3] and α2 an interferometric binary.[9]

The components of α1 have masses of 17 and 6.8 times that of the Sun (M☉), estimated radii of 6.8 and 3.2 R☉, and effective temperatures of approximately 29,000 and 20,000 K. They take 75.747 days to complete an orbit around each other at a semi-major axis of almost exactly one astronomical unit (au), with a considerable orbital eccentricity of 0.37.[9] The mass of α1 Crucis A suggest that it is going to expand into a red supergiant (similar to Betelgeuse and Antares) before exploding as supernovae.[30] Component Ab may perform electron capture in the degenerate O+Ne+Mg core and trigger a supernova explosion,[31][32] otherwise it will become a massive white dwarf.[30]

The components of α2 have masses estimated at 12.4 and 9.8 M☉, radii at 5.4 and 4.4 R☉, and effective temperatures at 26,950 and 24,350 K, respectively. Their orbit is not so well-constrained, with a likely orbital period of 405.4 days, semi-major axis of 3.0 au and eccentricity of 0.40, although an orbital period of 202.9 days coupled with a higher eccentricity of 0.64 and a semi-major axis of 1.90 au is still possible. The orbits of the α1 and α2 systems are significantly misaligned with each other, indicating that the system was initially an unstable multiple system which underwent dynamical unfolding.[9]

Photometry with the TESS satellite has shown that one of the stars in the α Crucis system is a β Cephei variable, although α1 and α2 Crucis are too close for TESS to resolve and determine which one is the pulsator.[8]

Rizzuto and colleagues determined in 2011 that the α Crucis system was 66% likely to be a member of the Lower Centaurus–Crux sub-group of the Scorpius–Centaurus association. It was not previously seen to be a member of the group.[33] A bow shock is present around α Crucis, and is visible in the infrared spectrum, but is not aligned with α Crucis; the bow shock likely formed from large-scale motions in the interstellar matter.[34]

α Crucis C

α Crucis C, also known as HD 108250 and HR 4729, has an apparent magnitude of 4.79[3] and lies 90 arcseconds away from triple star system α Crucis AB. It shares common proper motion with α Cru AB, and it is therefore generally assumed to be physically associated.[35][36] The projected separation between both systems is 9,600 astronomical units (au), which together with the components' masses, implies an orbital period of 130,000 years.[9] It was first observed in 1829, as a companion to α Crucis, by James Dunlop from Paramatta in New South Wales.[37]

α Crucis C is itself a single-lined spectroscopic binary system, initially uncovered in 1916, although the orbital elements were not known muntil 1979.[12] The two components orbit around each other with an orbital period of roughly 1.225 days.[12] The primary is a B-type star with a spectral class of B5 V.[6] It is estimated to be 4.5 times more massive than the Sun and 2.5 times larger. Nothing is known about the secondary but a lower limit on its mass of 0.64 M☉.[9]

α Crucis D

A close companion to α Crucis C, α Crucis D is magnitude 13.36[3] red dwarf star with a spectral type of M0V[3] and half the mass of the Sun.[9] It has been first identified in 1999 using adaptive optics at infrared wavelengths,[17] and is located at only 2.836" from α Crucis C.[3] Given the projected separation of 225 au, the orbital period between it and α Crucis C is thought to be 1,500 years.[9] It has been named α Crucis P (in order of discovery), or α Crucis D (as the fourth visible member of the system).[3]

  • Image of α Crucis (HD 108248/9), α Crucis C (HD 108250), and the bow shock nebula from the Spitzer Space Telescope
  • α Crucis AB and α Crucis C (the 2nd-brightest star)
  • Artist's impression of the stellar components compared to the Sun

In culture

Acrux is represented in the flags of Australia, New Zealand, Samoa, and Papua New Guinea as one of five stars that compose the Southern Cross. It is also featured in the flag of Brazil, along with 26 other stars, each of which represents a state; Acrux represents the state of São Paulo.[38] As of 2015, it is also represented on the cover of the Brazilian passport.

The Brazilian oceanographic research vessel Alpha Crucis is named after the star.

Notes

  1. ^ It is not known if the variability is coming from the α Crucis A or the α Crucis B system; more data is needed to uncover which one is the pulsator.
  2. ^ While the orbit listed below is the best possibility, a second set of orbits implying a smaller orbital period among other different elements cannot be ruled out yet by the observations.
  3. ^ a b c Derived from known radius and surface temperature of star.

References

  1. ^ a b c d e 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 Corben, P. M. (1966). "Photoelectric magnitudes and colours for bright southern stars". Monthly Notes of the Astron. Soc. Southern Africa. 25: 44. Bibcode:1966MNSSA..25...44C.
  3. ^ a b c d e f g h i j k l Tokovinin, Andrei (2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5.
  4. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  5. ^ a b c Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor: Dept. Of Astronomy. Bibcode:1978mcts.book.....H.
  6. ^ a b Corbally, C. J. (1984). "Close visual binaries. I - MK classifications". Astrophysical Journal Supplement Series. 55: 657. Bibcode:1984ApJS...55..657C. doi:10.1086/190973.
  7. ^ a b Stagg, Christopher (1987). "A photometric survey of the bright southern Be stars". Monthly Notices of the Royal Astronomical Society. 227: 213–240. Bibcode:1987MNRAS.227..213S. doi:10.1093/mnras/227.1.213.
  8. ^ a b c Sharma, Awshesh N.; Bedding, Timothy R.; Saio, Hideyuki; White, Timothy R. (2022). "Pulsating B stars in the Scorpius–Centaurus Association with TESS". Monthly Notices of the Royal Astronomical Society. 515 (1): 828–840. arXiv:2203.02582. Bibcode:2022MNRAS.515..828S. doi:10.1093/mnras/stac1816.
  9. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak Waisberg, Idel; Katz, Boaz (2026-03-11). "Upgrading Alpha Crucis to a seven star system. Discovery of Bb and orbital misalignment". arXiv:2603.11194 [astro-ph.SR].
  10. ^ a b Kaltcheva, N. T.; Golev, V. K.; Moran, K. (2014). "Massive stellar content of the Galactic supershell GSH 305+01-24". Astronomy & Astrophysics. 562: A69. arXiv:1312.5592. Bibcode:2014A&A...562A..69K. doi:10.1051/0004-6361/201321454. S2CID 54222753.
  11. ^ Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
  12. ^ a b c Hernandez, C. A.; De Hernandez, E. B. (1979). "The orbital elements of 25 G Crucis (HD 108250)". Revista Mexicana de Astronomía y Astrofísica. 4: 297. Bibcode:1979RMxAA...4..297H.
  13. ^ Jin, Harim; Langer, Norbert; Lennon, Daniel J.; Proffitt, Charles R. (2024). "Boron depletion in Galactic early B-type stars reveals two different main sequence star populations". Astronomy and Astrophysics. 690: A135. arXiv:2405.18266. Bibcode:2024A&A...690A.135J. doi:10.1051/0004-6361/202450896.
  14. ^ Dravins, Dainis; Jensen, Hannes; Lebohec, Stephan; Nuñez, Paul D. (2010). "Stellar intensity interferometry: Astrophysical targets for sub-milliarcsecond imaging". Optical and Infrared Interferometry II. Proceedings of the SPIE. Vol. 7734. pp. 77340A. arXiv:1009.5815. Bibcode:2010SPIE.7734E..0AD. doi:10.1117/12.856394. S2CID 55641060.
  15. ^ a b Aerts, C.; Molenberghs, G.; De Ridder, J. (2023). "Astrophysical properties of 15062 Gaia DR3 gravity-mode pulsators. Pulsation amplitudes, rotation, and spectral line broadening". Astronomy and Astrophysics. 672. arXiv:2302.07870. Bibcode:2023A&A...672A.183A. doi:10.1051/0004-6361/202245713.
  16. ^ Brown, A. G. A.; Verschueren, W. (1997). "High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2". Astronomy and Astrophysics. 319: 811. arXiv:astro-ph/9608089. Bibcode:1997A&A...319..811B.
  17. ^ a b Tokovinin, A. A.; Chalabaev, A.; Shatsky, N. I.; Beuzit, J. L. (1999). "A near IR adaptive optics search for faint companions to early-type multiple stars". Astronomy and Astrophysics. 346: 481. Bibcode:1999A&A...346..481T.
  18. ^ Bordeleau, André G. (12 August 2013). "Federative Republic of Brazil: Constellations in the Breeze". Flags of the Night Sky. New York: Springer. pp. 1–72. doi:10.1007/978-1-4614-0929-8_1. ISBN 978-1-4614-0928-1.
  19. ^ "A Story about Crux | Centre for Astronomical Heritage (CfAH)".
  20. ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
  21. ^ a b "IAU Catalog of Star Names". Retrieved 21 November 2016.
  22. ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  23. ^ Memoirs of the Rev. Walter M. Lowrie: missionary to China (1849), p. 93. Described as an "Americanism" in The Geographical Journal, vol. 92, Royal Geographical Society, 1938.
  24. ^ "IAU Working Group on Star Names (WGSN)". Archived from the original on 10 June 2016. Retrieved 22 May 2016.
  25. ^ "Bulletin of the IAU Working Group on Star Names, No. 2" (PDF). Retrieved 12 October 2016.
  26. ^ Richard Hinckley Allen, Star Names: Their Lore and Meaning, Dover Books, 1963.
  27. ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  28. ^ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived 2010-09-03 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  29. ^ Silva, Guilherme Marques dos Santos; Ribas, Felipe Braga; Freitas, Mário Sérgio Teixeira de (2008). "Transformação de coordenadas aplicada à construção da maquete tridimensional de uma constelação". Revista Brasileira de Ensino de Física. 30: 1306.1 – 1306.7. doi:10.1590/S1806-11172008000100007.
  30. ^ a b Kaler, James B. (2002). "Acrux". The Hundred Greatest Stars. pp. 4–5. doi:10.1007/0-387-21625-1_2. ISBN 978-0-387-95436-3.
  31. ^ Nomoto, K. (1984). "Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + NE + MG cores". Astrophysical Journal. 277: 791. Bibcode:1984ApJ...277..791N. doi:10.1086/161749.
  32. ^ S. E. Woosley, Alexander Heger (May 25, 2015). "The Remarkable Deaths of 9 - 11 Solar Mass Stars". Astrophysics. 810 (1): 34. arXiv:1505.06712. Bibcode:2015ApJ...810...34W. doi:10.1088/0004-637X/810/1/34. S2CID 119163256.
  33. ^ Rizzuto, Aaron; Ireland, Michael; Robertson, J. G. (October 2011). "Multidimensional Bayesian membership analysis of the Sco OB2 moving group". Monthly Notices of the Royal Astronomical Society. 416 (4): 3108–3117. arXiv:1106.2857. Bibcode:2011MNRAS.416.3108R. doi:10.1111/j.1365-2966.2011.19256.x. S2CID 54510608.
  34. ^ Torosyan, M.; Azatyan, N.; Nikoghosyan, E.; Samsonyan, A.; Andreasyan, D. (2024). "The runaway nature and origin of α Crucis system". Communications of the Byurakan Astrophysical Observatory. 71: 42–47. arXiv:2407.09934. Bibcode:2024CoBAO..71...42T. doi:10.52526/25792776-24.71.1-42.
  35. ^ Shatsky, N.; Tokovinin, A. (2002). "The mass ratio distribution of B-type visual binaries in the Sco OB2 association". Astronomy and Astrophysics. 382: 92–103. arXiv:astro-ph/0109456. Bibcode:2002A&A...382...92S. doi:10.1051/0004-6361:20011542. S2CID 16697655.
  36. ^ Eggleton, Peter; Tokovinin, A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  37. ^ Dunlop, James (1829). "Approximate Places of Double Stars in the Southern Hemisphere, observed at Paramatta in New South Wales". Memoirs of the Royal Astronomical Society. 3: 257. Bibcode:1829MmRAS...3..257D.
  38. ^ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website.
Cite error: A list-defined reference named "GSM" is not used in the content (see the help page).


This article is issued from Wikipedia. The text is available under Creative Commons Attribution-Share Alike 4.0 unless otherwise noted. Additional terms may apply for the media files.