| 释义 |
Wolf–Rayet Astr.|ˈvɒlfrɛjɛ, wʊlf-|
The names of C. J. E. Wolf (1827–1918) and G. A. P. Rayet (1839–1906), French astronomers, used attrib. to denote any of a class of hot white-to-blue stars (first described by them in 1867) which are characterized by bright, broad spectral lines due to hydrogen, helium, carbon, or nitrogen and are believed to be short-lived and unstable.
1890A. M. Clerke Syst. of Stars v. 71 Accurate measurements of the three original Wolf-Rayet stars..were made. 1930R. H. Baker Astron. ix. 356 The Wolf-Rayet stars are distinguished from the other Class O stars by the great width of the bright lines in their spectra. 1978Pasachoff & Kutner University Astron. ii. 40 Astronomers think that the emission in Wolf-Rayet stars comes from shells of material that the star has ejected into the space surrounding it. |