Hyades (star cluster)

Hyades Cluster
Observation data (J2000.0 epoch)
Constellation Taurus
Right ascension 4h 27m
Declination +15° 52′
Distance 153 ly (47 pc[1][2][3][4])
Apparent magnitude (V) 0.5
Apparent dimensions (V) 330′
Physical characteristics
Mass 400 M☉
Radius 10 light years (core radius)
Estimated age 625 million years
Other designations Melotte 25, Collinder 50, Caldwell 41

The Hyades (/ˈhaɪ.ədiːz/; Greek Ὑάδες, also known as Melotte 25 or Collinder 50) is the nearest open cluster to the Solar System and one of the best-studied of all star clusters. The Hipparcos satellite, the Hubble Space Telescope, and infrared color-magnitude diagram fitting have been used to establish a distance of ~153 ly (47 pc) to the cluster center.[1][2][3][4] The distances established by these three independent methods agree, thereby making the Hyades an important rung on the cosmic distance ladder. The cluster consists of a roughly spherical group of hundreds of stars sharing the same age, place of origin, chemical content, and motion through space.[1][5] From the perspective of observers on Earth, the Hyades Cluster appears in the constellation Taurus, where its brightest stars form a "V" shape along with the still brighter red giant Aldebaran. However, Aldebaran is unrelated to the Hyades, as it is located much closer to Earth (hence its apparent brightness) and merely happens to lie along the same line of sight.

The five brightest member stars of the Hyades have all evolved away from the Main Sequence and now lie at the bottom of the giant branch.[6] Four of these stars, with Bayer designations Gamma, Delta 1, Epsilon, and Theta Tauri, form an asterism that is traditionally identified as the head of Taurus the Bull.[6] The other is Zeta 1 Tauri, which lies 2° further south. Epsilon Tauri, known as Ain (the "Bull's Eye"), has a gas giant exoplanet candidate,[7] the first planet to be found in any open cluster.

The age of the Hyades is estimated to be about 625 million years.[1] The cluster core, where stars are most densely packed, has a radius of 2.7 parsecs (corresponding to a diameter of 17.6 light years), and the cluster's tidal radius is 10 parsecs (corresponding to a diameter of 65 light years).[1] However, about one-third of confirmed member stars have been observed well outside this boundary, in the cluster's extended halo; these stars are probably in the process of escaping from its gravitational influence.[1]

Proper motion

The stars of the Hyades are more enriched in heavier elements than our Sun and other ordinary stars in the Solar neighborhood, with the overall cluster metallicity measured at +0.14.[1]

Animation of proper motion in -/+ 300 000 years (cross-eyed viewing)
Animation of proper motion in million years for 3D glasses (red-green or red-blue)

The Hyades Cluster is related to other stellar groups in the Sun's vicinity. Its age, metallicity, and proper motion coincide with those of the larger and more distant Praesepe Cluster,[8] and the trajectories of both clusters can be traced back to the same region of space, indicating a common origin.[9] Another associate is the Hyades Stream, a large collection of scattered stars that also share a similar trajectory with the Hyades Cluster. Recent results have found that at least 15% of stars in the Hyades stream share the same chemical fingerprint as the Hyades cluster stars.[10] However, about 85% of stars in the Hyades Stream have been shown to be completely unrelated to the original cluster on the grounds of dissimilar age and metallicity; their common motion is attributed to tidal effects of the massive rotating bar at the center of the Milky Way Galaxy.[11] Among the remaining members of the Hyades Stream, the exoplanet host star Iota Horologii has recently been proposed as an escaped member of the primordial Hyades Cluster.[12]

The Hyades are unrelated to two other nearby stellar groups, the Pleiades and the Ursa Major Stream, which are easily visible to the naked eye under clear dark skies.

History

Bright stars in the core of the Hyades Cluster

In Greek mythology, the Hyades were the five daughters of Atlas and half-sisters to the Pleiades. After the death of their brother, Hyas, the weeping sisters were transformed into a cluster of stars that was afterwards associated with rain.

As a naked-eye object, the Hyades cluster has been known since prehistoric times. It is mentioned by numerous Classical authors from Homer to Ovid.[13] In Book 18 of the Iliad the stars of the Hyades appear along with the Pleiades, Ursa Major, and Orion on the shield that the god Hephaistos made for Achilles.[14]

In England the cluster was known as the "April Rainers" from an association with April showers, as recorded in the folk song "Green Grow the Rushes, O".

The cluster was probably first catalogued by Giovanni Batista Hodierna in 1654, and it subsequently appeared in many star atlases of the 17th and 18th centuries.[13] However, Charles Messier did not include the Hyades in his 1781 catalog of deep sky objects.[13] It therefore lacks a Messier number, unlike many other, more distant open clusters – e.g., M44 (Praesepe), M45 (Pleiades), and M67.

In 1869, the astronomer R.A. Proctor observed that numerous stars at large distances from the Hyades share a similar motion through space.[15] In 1908, Lewis Boss reported almost 25 years of observations to support this premise, arguing for the existence of a co-moving group of stars that he called the Taurus Stream (now generally known as the Hyades Stream or Hyades Supercluster). Boss published a chart that traced the scattered stars' movements back to a common point of convergence.[16]

By the 1920s, the notion that the Hyades shared a common origin with the Praesepe Cluster was widespread,[17] with Rudolf Klein-Wassink noting in 1927 that the two clusters are "probably cosmically related."[18] For much of the twentieth century, scientific study of the Hyades focused on determining its distance; modeling its evolution; confirming or rejecting candidate members; and characterizing individual stars.

Morphology and evolution

All stars form in clusters, but most clusters break up less than 50 million years after star formation concludes.[19] The astronomical term for this process is "evaporation." Only extremely massive clusters, orbiting far from the Galactic center, can avoid evaporation over extended timescales.[20] As one such survivor, the Hyades Cluster probably contained a much larger star population in its infancy. Estimates of its original mass range from 800 to 1600 times the mass of our Sun (M☉), implying still larger numbers of individual stars.[21][22]

Star populations

Theory predicts that a young cluster of this size should give birth to stars and substellar objects of all spectral types, from huge, hot O stars down to dim brown dwarfs.[22] However, studies of the Hyades show that it is deficient in stars at both extremes of mass.[5][23] At an age of 625 million years, the cluster's main sequence turn-off is about 2.3 M☉, meaning that all heavier stars have evolved into subgiants, giants, or white dwarfs, while less massive stars continue fusing hydrogen on the main sequence.[21] Extensive surveys have revealed a total of 8 white dwarfs in the cluster core,[24] corresponding to the final evolutionary stage of its original population of B-type stars (each about 3 M☉).[21] The preceding evolutionary stage is currently represented by the cluster's four red clump giants. Their present spectral type is K0 III, but all are actually "retired A stars" of around 2.5 M☉.[7][25][26] An additional "white giant" of type A7 III is the primary of θ² Tauri, a binary system that includes a less massive companion of spectral type A; this pair is visually associated with θ¹ Tauri, one of the four red giants, which also has an A-type binary companion.[25][27]

The remaining population of confirmed cluster members includes numerous bright stars of spectral types A (at least 21), F (about 60), and G (about 50).[1][23] All these star types are concentrated much more densely within the tidal radius of the Hyades than within an equivalent 10-parsec radius of the Earth. By comparison, our local 10-parsec sphere contains only 4 A stars, 6 F stars, and 21 G stars.[28]

The Hyades' cohort of lower-mass stars – spectral types K and M – remains poorly understood, despite proximity and long observation. At least 48 K dwarfs are confirmed members, along with about a dozen M dwarfs of spectral types M0-M2.[1][23][29] Additional M dwarfs have been proposed, but few are later than M3, and only about 12 brown dwarfs are currently reported.[5][30][31] This deficiency at the bottom of the mass range contrasts strongly with the distribution of stars within 10 parsecs of the Solar System, where at least 239 M dwarfs are known, comprising about 76% of all neighborhood stars.[28]

Mass segregation

The observed distribution of stellar types in the Hyades Cluster demonstrates a history of mass segregation. With the exception of its white dwarfs, the cluster's central 2 parsecs (6.5 light years) contain only star systems of at least 1 M☉.[1] This tight concentration of heavy stars gives the Hyades its overall structure, with a core defined by bright, closely packed systems and a halo consisting of more widely separated stars in which later spectral types are common. The core radius is 2.7 parsecs (8.8 light years, a little more than the distance between the Sun and Sirius), while the half-mass radius, within which half the cluster's mass is contained, is 5.7 parsecs (18.6 light years). The tidal radius of 10 parsecs (32.6 light years) represents the Hyades' average outer limit, beyond which a star is unlikely to remain gravitationally bound to the cluster core.[1][21]

Stellar evaporation occurs in the cluster halo as smaller stars are scattered outward by more massive insiders. From the halo they may then be lost to tides exerted by the Galactic core or to shocks generated by collisions with drifting hydrogen clouds.[20] In this way the Hyades probably lost much of its original population of M dwarfs, along with substantial numbers of brighter stars.

Stellar multiplicity

Another result of mass segregation is the concentration of binary systems in the cluster core.[1][23] More than half of the known F and G stars are binaries, and these are preferentially located within this central region. As in the immediate Solar neighborhood, binarity increases with increasing stellar mass. The fraction of binary systems in the Hyades increases from 26% among K-type stars to 87% among A-type stars.[23] Hyades binaries tend to have small separations, with most binary pairs in shared orbits whose semimajor axes are smaller than 50 astronomical units.[32] Although the exact ratio of single to multiple systems in the cluster remains uncertain, this ratio has considerable implications for our understanding of its population. For example, Perryman and colleagues list about 200 high-probability Hyades members.[1] If the binary fraction is 50%, the total cluster population would be at least 300 individual stars.

Future evolution

Surveys indicate that 90% of open clusters dissolve less than 1 billion years after formation, while only a tiny fraction survive for the present age of the Solar System (about 4.6 billion years).[20] Over the next few hundred million years, the Hyades will continue to lose both mass and membership as its brightest stars evolve off the main sequence and its dimmest stars evaporate out of the cluster halo. It may eventually be reduced to a remnant containing about a dozen star systems, most of them binary or multiple, which will remain vulnerable to ongoing dissipative forces.[20]

Brightest stars

This is a list of Hyades cluster member stars that are fourth magnitude or brighter.[33]

Hyades brightest stars
Designation HD Apparent
magnitude		 Stellar
classification
Theta² Tauri 28319 3.398 A7III
Epsilon Tauri 28305 3.529 K0III
Gamma Tauri 27371 3.642 G8III
Delta¹ Tauri 27697 3.753 G8III
Theta¹ Tauri 28307 3.836 G7III
Kappa Tauri 27934 4.201 A7IV-V
90 Tauri 29388 4.262 A6V
Upsilon Tauri 28024 4.282 A8Vn
Delta² Tauri 27962 4.298 A2IV
71 Tauri 28052 4.480 F0V...

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 Perryman, M.A.C.; et al. (1998). "The Hyades: distance, structure, dynamics, and age". Astronomy & Astrophysics 331: 81–120. arXiv:astro-ph/9707253. Bibcode:1998A&A...331...81P.
  2. 1 2 van Leeuwen, F. "Parallaxes and proper motions for 20 open clusters as based on the new Hipparcos catalogue", A\&A, 2009
  3. 1 2 Majaess, D.; Turner, D.; Lane, D.; Krajci, T. "Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars", JAAVSO, 2011
  4. 1 2 McArthur, Barbara E.; Benedict, G. Fritz; Harrison, Thomas E.; van Altena, William "Astrometry with the Hubble Space Telescope: Trigonometric Parallaxes of Selected Hyads", AJ, 2011
  5. 1 2 3 Bouvier J, Kendall T, Meeus G, Testi L, Moraux E, Stauffer JR, James D, Cuillandre J-C, Irwin J, McCaughrean MJ, Baraffe I, Bertin E. (2008) Brown dwarfs and very low mass stars in the Hyades cluster: a dynamically evolved mass function. Astronomy & Astrophysics, 481: 661-672. Abstract at http://adsabs.harvard.edu/abs/2008A%26A...481..661B.
  6. 1 2 Jim Kaler. "Hyadum I". Jim Kaler's Stars. Retrieved 29 October 2013.
  7. 1 2 Sato B, Izumiura H, Toyota E, et al. (2007) A planetary companion to the Hyades giant Epsilon Tauri. Astrophysical Journal, 661: 527-531. Abstract at http://adsabs.harvard.edu/abs/2007ApJ...661..527S.
  8. ↑ Dobbie, PD; Napiwotzki, R; Burleigh, MR; et al. (2006). "New Praesepe white dwarfs and the initial mass-final mass relation". Monthly Notices of the Royal Astronomical Society 369: 383–389. arXiv:astro-ph/0603314. Bibcode:2006MNRAS.369..383D. doi:10.1111/j.1365-2966.2006.10311.x.
  9. ↑ "Messier Object 44". SEDS. 2007-08-25. Retrieved 2012-12-24.
  10. ↑ De Silva, G; et al. (2011). "High-resolution elemental abundance analysis of the Hyades supercluster". MNRAS 415: 563–575. arXiv:1103.2588. Bibcode:2011MNRAS.415..563D. doi:10.1111/j.1365-2966.2011.18728.x.
  11. ↑ Famaey B, Pont F, Luri X, Udry S, Mayor M, Jorissen A. (2007) The Hyades stream: an evaporated cluster or an intrusion from the inner disk? Astronomy & Astrophysics, 461: 957-962. Abstract at http://adsabs.harvard.edu/abs/2007A%26A...461..957F.
  12. ↑ Vauclair, S.; Laymand, M.; Bouchy, F.; Vauclair, G.; Hui Bon Hoa, A.; Charpinet, S.; Bazot, M. (2008). "The exoplanet-host star iota Horologii: an evaporated member of the primordial Hyades cluster.". arXiv:0803.2029v1 [astro-ph]., announced in Emily Baldwin. "The Drifting Star". Retrieved 2008-04-18.
  13. 1 2 3 Information on the Hyades from SEDS
  14. ↑ Homer. The Iliad. Translated by Richmond Lattimore. University of Chicago Press, 1951.
  15. ↑ Zuckerman B, Song I. (2004) Young stars near the Sun. Annual Review of Astronomy & Astrophysics. Volume 42, 685-721. Abstract at http://adsabs.harvard.edu/abs/2004ARA%26A..42..685Z.
  16. ↑ Boss L. (1908) Convergent of a moving cluster in Taurus. Astronomical Journal, 26: 31-36. Full text link at http://adsabs.harvard.edu/abs/1908AJ.....26...31B.
  17. ↑ Hertzsprung E. (1922) On the motions of Praesepe and of the Hyades. Bulletin of the Astronomical Institutes of the Netherlands, Vol. 1, p.150. Full text link at http://adsabs.harvard.edu/abs/1922BAN.....1..150H.
  18. ↑ Klein-Wassink WJ. (1927) The proper motion and the distance of the Praesepe cluster. Publications of the Kapteyn Astronomical Laboratory Groningen, 41: 1-48. Full text link at http://adsabs.harvard.edu/abs/1927PGro...41....1K
  19. ↑ Lada, CJ; Lada, EA (2003). "Embedded clusters in molecular clouds". Annual Review of Astronomy & Astrophysics 41: 57–115. arXiv:astro-ph/0301540. Bibcode:2003ARA&A..41...57L. doi:10.1146/annurev.astro.41.011802.094844.
  20. 1 2 3 4 Pavani, DB; Bica, E (2007). "Characterization of open cluster remnants". Astronomy & Astrophysics 468: 139–150. arXiv:0704.1159. Bibcode:2007A&A...468..139P. doi:10.1051/0004-6361:20066240.
  21. 1 2 3 4 Weideman V, Jordan S, Iben I, Casertano S. (1992) White dwarfs in the halo of the Hyades Cluster – The case of the missing white dwarfs. Astronomical Journal, 104: 1876-1891. 1992AJ....104.1876W.
  22. 1 2 Kroupa, P; Boily, CM (2002). "On the mass function of star clusters". Monthly Notices of the Royal Astronomical Society 336: 1188–1194. arXiv:astro-ph/0207514. Bibcode:2002MNRAS.336.1188K. doi:10.1046/j.1365-8711.2002.05848.x.
  23. 1 2 3 4 5 Böhm-Vitense, E (2007). "Hyades morphology and star formation". Astronomical Journal 133: 1903–1910. Bibcode:2007AJ....133.1903B. doi:10.1086/512124.
  24. ↑ Böhm-Vitense E. (1995) White dwarf companions to Hyades F stars. Astronomical Journal, 110: 228-231. Abstract at http://adsabs.harvard.edu/abs/1995AJ....110..228B.
  25. 1 2 Torres, G; Stefanik, RP; Latham, DW (1997). "The Hyades binaries Theta1 Tauri and Theta2 Tauri: The distance to the cluster and the mass-luminosity relation". Astrophysical Journal 485: 167–181. Bibcode:1997ApJ...485..167T. doi:10.1086/304422.
  26. ↑ Johnson JA, Fischer D, Marcy GW, Wright JT, Driscoll P, Butler RP, Hekker S, Reffert S, Vogt SS. (2007a) Retired A stars and their companions: Exoplanets orbiting three intermediate-mass subgiants. Astrophysical Journal, 665: 785-793. Abstract at http://adsabs.harvard.edu/abs/2007ApJ...665..785J.
  27. ↑ Armstrong, JT; Mozurkewich, D; Hajian, AR; et al. (2006). "The Hyades binary Theta2 Tauri: Confronting evolutionary models with optical interferometry". Astronomical Journal 131: 2643–2651. Bibcode:2006AJ....131.2643A. doi:10.1086/501429.
  28. 1 2 Research Consortium on Nearby Stars (RECONS). Ten-parsec census at http://joy.chara.gsu.edu/RECONS/census.posted.htm.
  29. ↑ Endl, M; Cochran, WD; Kurster, M; Paulson, DB; Wittenmyer, RA; MacQueen, PJ; Tull, RG (2006). "Exploring the frequency of close-in Jovian planets around M dwarfs". Astrophysical Journal 649: 436–443. arXiv:astro-ph/0606121. Bibcode:2006ApJ...649..436E. doi:10.1086/506465.
  30. ↑ Stauffer, JR; Balachandran, SC; Krishnamurthi, A; Pinsonneault, M; Terndrup, DM; Stern, RA (1997). "Rotational velocities and chromospheric activity of M dwarfs in the Hyades". Astrophysical Journal 475: 604–622. Bibcode:1997ApJ...479..776S. doi:10.1086/303930.
  31. ↑ Hogan E, Jameson R F, Casewell SL, Osbourne, SL, Hambly NC. (2008) L dwarfs in the Hyades. Monthly Notices of the Royal Astronomical Society, 388 (2) 495-499. Abstract at http://adsabs.harvard.edu/abs/2008MNRAS.388..495H.
  32. ↑ Patience J, Ghez AM, Reid IN, Weinberger AJ, Matthews K. (1998) The multiplicity of the Hyades and its implications for binary star formation and evolution. Astronomical Journal, 115: 1972-1988. Abstract at http://adsabs.harvard.edu/abs/1998AJ....115.1972P.
  33. ↑ Röser, S.; et al. (July 2011), "A deep all-sky census of the Hyades", Astronomy & Astrophysics 531: 15, arXiv:1105.6093, Bibcode:2011A&A...531A..92R, doi:10.1051/0004-6361/201116948, A92. In the Vizier catalogue, sort on Vmag using '<4.51'. See also the linked entries in the All-sky Compiled Catalogue of 2.5 million stars (Kharchenko+ 2009). line feed character in |postscript= at position 83 (help)

External links

Coordinates: 04h 28m 17s, +15° 45′ 40″

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