A mercury-manganese star is a type of chemically peculiar star with a prominent spectral line at 398.4 nm, due to absorption from ionized mercury. These stars are of spectral type B8, B9, or A0, corresponding to surface temperatures between about 10,000 and 15,000 K, with two distinctive characteristics:
- An atmospheric excess of elements like phosphorus, manganese, gallium, strontium, yttrium, zirconium, platinum and mercury.
- A lack of a strong dipole magnetic field.
Their rotation is relatively slow, and as a consequence their atmosphere is relatively calm. It is thought, but has not been proven, that some types of atoms sink under the force of gravity, while others are lifted towards the exterior of the star by radiation pressure, making a heterogeneous atmosphere.
The following table includes the brightest stars in this group.
|Name||Bayer or Flamsteed designation||Spectral type||Apparent visual magnitude|
|Gienah Corvi||γ Corvi A||B8III||2.59|
|Muliphein||γ Canis Majoris||B8II||4.10|
|ι Coronae Borealis||A0p||4.98|
|κ Cancri A||B8IIImnp||5.24|
|Dabih Minor||β Capricorni B||B9.5III/IV||6.10|
|HD 30963||B9 III||7.23|
- Mercury-manganese star. The Internet Encyclopedia of Science, David Darling. Accessed on line August 14, 2008.
- Michaud, Georges (May 1970). "Diffusion Processes in Peculiar A Stars". Astrophysical Journal 160: 641–658. doi:10.1086/150459. Bibcode: 1970ApJ...160..641M. http://cdsads.u-strasbg.fr/abs/1970ApJ...160..641M.
- Names, spectral types and apparent magnitudes taken from SIMBAD, except as noted.
- Muliphein , Stars, Jim Kaler. Accessed on line August 14, 2008.
- Adelman, S. J. (December 1988), "Elemental Abundance Analyses with Coadded DAO Spectrograms - Part Five - the Mercury-Manganese Stars Phi-Herculis 28-HERCULIS and HR:7664", Monthly Notices of the Royal Astronomical Society 235 (3): 763, doi:10.1093/mnras/235.3.763, Bibcode: 1988MNRAS.235..763A.
- Dabih , Stars, Jim Kaler. Accessed on line August 14, 2008.
Original source: https://en.wikipedia.org/wiki/ Mercury-manganese star. Read more