Thick disk

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Edge on view of the Milky Way with several structures indicated (not to scale). The thick disk is shown in light yellow. Milky-way-edge-on.pdf
Edge on view of the Milky Way with several structures indicated (not to scale). The thick disk is shown in light yellow.

The thick disk is one of the structural components of about 2/3 of all disk galaxies, including the Milky Way. It was discovered first in external edge-on galaxies. [1] Soon after, it was proposed as a distinct galactic structure in the Milky Way, different from the thin disk and the halo in the 1983 article by Gilmore & Reid. [2] It is supposed to dominate the stellar number density between 1 and 5 kiloparsecs (3.3 and 16.3  kly) above the galactic plane [2] and, in the solar neighborhood, is composed almost exclusively of older stars. For the Milky Way, the thick disk has a scale height of around 0.6–1.1 kiloparsecs (2.0–3.6  kly) in the axis perpendicular to the disk, which is 3-4 times larger than the thin disk, and a scale length of around 1.9–2.3 kiloparsecs (6.2–7.5  kly) in the horizontal axis, in the direction of the radius. [3] Its stellar chemistry and stellar kinematics (composition and motion of it stars) are also said to set it apart from the thin disk. [4] Compared to the thin disk, thick disk stars typically have significantly lower levels of metals—that is, the abundance of elements other than hydrogen and helium. [5]

Contents

The thick disk is a source of early kinematic and chemical evidence for a galaxy's composition and thus is regarded as a very significant component for understanding galaxy formation.

With the availability of observations at larger distances away from the Sun, more recently it has become apparent that the Milky Way thick disk does not have the same chemical and age composition as all galactic radii. It was found instead that it is metal poor inside the solar radius, but becomes more metal rich outside it. [6] Additionally, recent observations have revealed that the average stellar age of thick disk stars quickly decreases as one moves from the inner to the outer disk. [7]

Origin

It was shown that there is a diversity of thick disc formation scenarios. [8] In general, various scenarios for the formation of this structure have been proposed, including:

Dispute

Although the thick disk is mentioned as a bona fide galactic structure in numerous scientific studies and it's even thought to be a common component of disk galaxies in general, [21] its nature is still under dispute.

The view of the thick disk as a single separate component has been questioned by a series of papers that describe the galactic disk with a continuous spectrum of components with different thicknesses. [22] [23]

See also

Galaxy parts

References

  1. ↑ Burstein, D. (1979-12-01). "Structure and origin of S0 galaxies. III - The luminosity distribution perpendicular to the plane of the disks in S0's". The Astrophysical Journal. 234: 829–836. Bibcode:1979ApJ...234..829B. doi:10.1086/157563. ISSN   0004-637X.
  2. 1 2 Gilmore, G.; Reid, N. (1983). "New light on faint stars. III - Galactic structure towards the South Pole and the Galactic thick disc". Monthly Notices of the Royal Astronomical Society . 202 (4): 1025. Bibcode:1983MNRAS.202.1025G. doi: 10.1093/mnras/202.4.1025 .
  3. ↑ Tkachenko, R.; et al. (2025). "Determining the Scale Length and Height of the Milky Way's Thick Disc Using RR Lyrae". Universe . 11 (4): 132. arXiv: 2505.00780 . doi: 10.3390/universe11040132 .
  4. ↑ Kordopatis, G.; et al. (2011). "A spectroscopic survey of thick disc stars outside the solar neighbourhood". Astronomy & Astrophysics . 535: A107. arXiv: 1110.5221 . Bibcode:2011A&A...535A.107K. doi:10.1051/0004-6361/201117373. S2CID   118616147.
  5. ↑ Freeman, K. C. (2010). "The HERMES Project: Reconstructing Galaxy Formation". In Block, D. L.; Freeman, K. C.; Puerari, I. (eds.). Galaxies and their Masks. Springer. p. 319. Bibcode:2010gama.conf..319F. doi:10.1007/978-1-4419-7317-7_27. ISBN   978-1-4419-7316-0.
  6. ↑ Bensby, T.; Alves-Brito, A.; Oey, M. S.; Yong, D.; Meléndez, J. (2011-07-01). "A First Constraint on the Thick Disk Scale Length: Differential Radial Abundances in K Giants at Galactocentric Radii 4, 8, and 12 kpc". The Astrophysical Journal Letters. 735 (2): L46. arXiv: 1106.1914 . Bibcode:2011ApJ...735L..46B. doi:10.1088/2041-8205/735/2/L46. ISSN   0004-637X. S2CID   119266731.
  7. ↑ Martig, Marie; Minchev, Ivan; Ness, Melissa; Fouesneau, Morgan; Rix, Hans-Walter (2016-11-01). "A Radial Age Gradient in the Geometrically Thick Disk of the Milky Way". The Astrophysical Journal. 831 (2): 139. arXiv: 1609.01168 . Bibcode:2016ApJ...831..139M. doi: 10.3847/0004-637X/831/2/139 . ISSN   0004-637X. S2CID   54652169.
  8. ↑ Kasparova, A. (2016). "The Diversity of Thick Galactic Discs". Monthly Notices of the Royal Astronomical Society: Letters . 460 (1): 89–93. arXiv: 1604.07624 . Bibcode:2016MNRAS.460L..89K. doi: 10.1093/mnrasl/slw083 .
  9. ↑ Villalobos, Álvaro; Helmi, Amina (2008-12-01). "Simulations of minor mergers - I. General properties of thick discs". Monthly Notices of the Royal Astronomical Society. 391 (4): 1806–1827. arXiv: 0803.2323 . Bibcode:2008MNRAS.391.1806V. doi: 10.1111/j.1365-2966.2008.13979.x . ISSN   0035-8711. S2CID   14881474.
  10. ↑ Steinmetz, M. (2012). "The Galactic thin and thick disk". Astronomische Nachrichten . 333 (5–6): 523–529. arXiv: 1205.6098 . Bibcode:2012AN....333..523S. doi:10.1002/asna.201211698. S2CID   119112515.
  11. ↑ Bensby, T.; Feltzing, F. (2009). "The Galactic thin and thick discs in the context of galaxy formation". Proceedings of the IAU Symposium . 265: 300–303. arXiv: 0908.3807 . Bibcode:2010IAUS..265..300B. doi:10.1017/S1743921310000773. S2CID   18562648.
  12. ↑ Schoenrich, R.; Binney, J. (2009). "Chemical Evolution with Radial Migration" (PDF). Monthly Notices of the Royal Astronomical Society . 396 (1): 203–222. arXiv: 0809.3006 . Bibcode:2009MNRAS.396..203S. doi: 10.1111/j.1365-2966.2009.14750.x . S2CID   14749516.
  13. ↑ Loebman, S.; et al. (2011). "The Genesis of the Milky Way's Thick Disk via Stellar Migration". The Astrophysical Journal . 737 (1): 8. arXiv: 1009.5997 . Bibcode:2011ApJ...737....8L. doi:10.1088/0004-637X/737/1/8. S2CID   21097464.
  14. ↑ Brook, C. B; Kawata, D.; Gibson, B. K.; Freeman, K. C. (2004). "The Emergence of the Thick Disk in a CDM Universe". The Astrophysical Journal . 612 (2): 894–899. arXiv: astro-ph/0405306 . Bibcode:2004ApJ...612..894B. doi:10.1086/422709. S2CID   54633942.
  15. ↑ Bournaud, Frédéric; Elmegreen, Bruce G.; Martig, Marie (2009-12-01). "The Thick Disks of Spiral Galaxies as Relics from Gas-rich, Turbulent, Clumpy Disks at High Redshift". The Astrophysical Journal Letters. 707 (1): L1 –L5. arXiv: 0910.3677 . Bibcode:2009ApJ...707L...1B. doi:10.1088/0004-637X/707/1/L1. ISSN   0004-637X. S2CID   118528894.
  16. ↑ Minchev, I.; Martig, M.; Streich, D.; Scannapieco, C.; de Jong, R. S.; Steinmetz, M. (2015-04-24). "On the Formation of Galactic Thick Disks". The Astrophysical Journal. 804 (1): L9. arXiv: 1502.06606 . Bibcode:2015ApJ...804L...9M. doi:10.1088/2041-8205/804/1/L9. ISSN   2041-8213. S2CID   59389858.
  17. ↑ Fohlmeister, J. (24 April 2015). "The riddle of galactic thin–thick disk solved". Phys.org . Retrieved 24 May 2015.
  18. ↑ Bournaud, Frédéric; Elmegreen, Bruce G.; Martig, Marie (2009-12-01). "The Thick Disks of Spiral Galaxies as Relics from Gas-rich, Turbulent, Clumpy Disks at High Redshift". The Astrophysical Journal Letters. 707 (1): L1 –L5. arXiv: 0910.3677 . Bibcode:2009ApJ...707L...1B. doi:10.1088/0004-637X/707/1/L1. ISSN   0004-637X. S2CID   118528894.
  19. ↑ Clarke, A.; Debattista, V. P.; Nidever, D. (2019-04-01). "The imprint of clump formation at high redshift - I. A disc alpha-abundance dichotomy". Monthly Notices of the Royal Astronomical Society. 484 (3): 3476–3490. arXiv: 1901.00931 . Bibcode:2019MNRAS.484.3476C. doi: 10.1093/mnras/stz104 . ISSN   0004-637X.
  20. ↑ Beraldo e Silva, L.; Debattista, V. P.; Khachaturyants, T. (2020-03-01). "Geometric properties of galactic discs with clumpy episodes". Monthly Notices of the Royal Astronomical Society. 492 (4): 4716–4726. arXiv: 1911.03717 . Bibcode:2020MNRAS.492.4716B. doi: 10.1093/mnras/staa065 . ISSN   0004-637X.
  21. ↑ Yoachim, P.; Dalcanton, J. (2012). "Structural Parameters of Thin and Thick Disks in Edge-On Disk Galaxies". The Astronomical Journal . 131 (1): 226–249. arXiv: astro-ph/0508460 . Bibcode:2006AJ....131..226Y. doi:10.1086/497970. S2CID   2219155.
  22. ↑ Bovy, Jo; Rix, Hans-Walter; Liu, Chao; Hogg, David W.; Beers, Timothy C.; Lee, Young Sun (2012-07-01). "The Spatial Structure of Mono-abundance Sub-populations of the Milky Way Disk". The Astrophysical Journal. 753 (2): 148. arXiv: 1111.1724 . Bibcode:2012ApJ...753..148B. doi:10.1088/0004-637X/753/2/148. ISSN   0004-637X. S2CID   118530729.
  23. ↑ Bovy, J.; Rix, H.- W.; Hogg, D. W. (2012). "The Milky Way Has No Distinct Thick Disk". The Astrophysical Journal . 751 (2): 131. arXiv: 1111.6585 . Bibcode:2012ApJ...751..131B. doi:10.1088/0004-637X/751/2/131. S2CID   119299930.
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