Barium stars are spectral class G to K stars whose spectra indicate an overabundance of s-process elements by the presence of singly ionized barium, Ba II, at λ 455.4 nm. Barium stars also show enhanced spectral features of carbon, the bands of the molecules CH, CN and C2. The class was originally recognized and defined by William P. Bidelman and Philip Keenan.[1] Initially, after their discovery, they were thought to be red giants, but the same chemical signature has been observed in main-sequence stars[2][3] as well.
Observational studies of their radial velocity suggested that all barium stars are binary stars.[4][5][6][7][8] Observations in the ultraviolet using International Ultraviolet Explorer detected white dwarfs in some barium star systems.[9][10]
Barium stars are believed to be the result of mass transfer in a binary star system. The mass transfer occurred when the now-observed giant star was on the main sequence. Its companion, the donor star, was a carbon star on the asymptotic giant branch (AGB), and had produced carbon and s-process elements in its interior. These nuclear fusion products were mixed by convection to its surface. Some of that matter "polluted" the surface layers of the main-sequence star as the donor star lost mass at the end of its AGB evolution, and it subsequently evolved to become a white dwarf. These systems are being observed at an indeterminate amount of time after the mass transfer event, when the donor star has long been a white dwarf.[11][12] Depending on the initial properties of the binary system, the polluted star can be found at different evolutionary stages.[13]
During its evolution, the barium star will at times be larger and cooler than the limits of the spectral types G or K. When this happens, ordinarily such a star is spectral type M, but its s-process excesses may cause it to show its altered composition as another spectral peculiarity. While the star's surface temperature is in the M-type regime, the star may show molecular features of the s-process element zirconium, zirconium oxide (ZrO) bands. When this happens, the star will appear as an "extrinsic" S star.
Historically, barium stars posed a puzzle, because in standard stellar evolution theory G and K giants are not far enough along in their evolution to have synthesized carbon and s-process elements and mix them to their surfaces. The discovery of the stars' binary nature resolved the puzzle, putting the source of their spectral peculiarities into a companion star which should have produced such material. The mass transfer episode is believed to be quite brief on an astronomical timescale.
Prototypical barium stars include Zeta Capricorni, HR 774, and HR 4474.
The CH stars are Population II stars with similar evolutionary state, spectral peculiarities, and orbital statistics, and are believed to be the older, metal-poor analogs of the barium stars.[14]
References
edit- ^ Bidelman, W. P.; Keenan, P. C. (1951), "The BA II Stars", Astrophysical Journal, 114: 473, Bibcode:1951ApJ...114..473B, doi:10.1086/145488
- ^ Porto de Mello, G. F.; da Silva, L. (1997-02-20). "HR 6094: A Young Solar-Type, Solar-Metallicity Barium Dwarf Star". The Astrophysical Journal. 476 (2): L89–L92. Bibcode:1997ApJ...476L..89P. doi:10.1086/310504. ISSN 0004-637X.
- ^ North, Pierre; Jorissen, Alain; Mayor, Michel (2000). "Binarity among Barium Dwarfs and CH Subgiants: Will They Become Barium Giants?". Symposium - International Astronomical Union. 177: 269–275. doi:10.1017/s0074180900002497. ISSN 0074-1809.
- ^ McClure, R. D.; Fletcher, J. M.; Nemec, J. M. (1980), "The binary nature of the barium stars", Astrophysical Journal Letters, 238: L35, Bibcode:1980ApJ...238L..35M, doi:10.1086/183252
- ^ McClure, R. D.; Woodsworth, A. W. (1990), "The binary nature of the barium and CH stars. III – Orbital parameters", Astrophysical Journal, 352: 709, Bibcode:1990ApJ...352..709M, doi:10.1086/168573
- ^ Jorissen, A.; Mayor, M. (1988), "Radial velocity monitoring of a sample of barium and S stars using CORAVEL – Towards an evolutionary link between barium and S stars?", Astronomy and Astrophysics, 198: 187, Bibcode:1988A&A...198..187J
- ^ Jorissen, A.; Boffin, H.M.J.; Karinkuzhi, D.; Van Eck, S.; Escorza, A.; Shetye, S.; Van Winckel, H. (2019-05-30). "Barium and related stars and their white-dwarf companions. I. Giant stars". Astronomy & Astrophysics. 626: A127. arXiv:1904.03975. Bibcode:2019A&A...626A.127J. doi:10.1051/0004-6361/201834630. ISSN 0004-6361. S2CID 102351666.
- ^ Escorza, A.; Karinkuzhi, D.; Jorissen, A.; Siess, L.; Van Winckel, H.; Pourbaix, D.; Johnston, C.; Miszalski, B.; Oomen, G-M. (2019-04-22). "Barium and related stars, and their white-dwarf companions. II. Main-sequence and subgiant stars". Astronomy & Astrophysics. 626: A128. arXiv:1904.04095. Bibcode:2019A&A...626A.128E. doi:10.1051/0004-6361/201935390. ISSN 0004-6361. S2CID 102352414.
- ^ Dominy, J. F.; Lambert, D. L. (July 1983). "Do all barium stars have a white dwarf companion?". The Astrophysical Journal. 270: 180. Bibcode:1983ApJ...270..180D. doi:10.1086/161109. ISSN 0004-637X.
- ^ Gray, R. O.; McGahee, C. E.; Griffin, R. E. M.; Corbally, C. J. (2011-04-04). "First Direct Evidence That Barium Dwarfs Have White Dwarf Companions". The Astronomical Journal. 141 (5): 160. Bibcode:2011AJ....141..160G. doi:10.1088/0004-6256/141/5/160. ISSN 0004-6256.
- ^ McClure, R. D. (1985), "The carbon and related stars", Journal of the Royal Astronomical Society of Canada, 79: 277, Bibcode:1985JRASC..79..277M
- ^ Boffin, H. M. J.; Jorissen, A. (1988), "Can a barium star be produced by wind accretion in a detached binary?", Astronomy and Astrophysics, 205: 155, Bibcode:1988A&A...205..155B
- ^ Escorza, A.; Boffin, H. M. J.; Jorissen, A.; Van Eck, S.; Siess, L.; Van Winckel, H.; Karinkuzhi, D.; Shetye, S.; Pourbaix, D. (December 2017). "Hertzsprung-Russell diagram and mass distribution of barium stars". Astronomy & Astrophysics. 608: A100. arXiv:1710.02029. Bibcode:2017A&A...608A.100E. doi:10.1051/0004-6361/201731832. ISSN 0004-6361. S2CID 119428276.
- ^ McClure, R. D. (1984), "The barium stars", Publications of the Astronomical Society of the Pacific, 96: 117, Bibcode:1984PASP...96..117M, doi:10.1086/131310