Publications of the Astronomical Society of the Pacific, Volume 106, Issues 695-702Astronomical Society of the Pacific, 1994 |
From inside the book
Results 1-3 of 76
Page 135
... lines can be used for the solution of the inverse problem , that seemed inappropriate here . The observed lines are quite shallow . The identifications of some of the blending lines are uncertain , which does not allow us to treat them ...
... lines can be used for the solution of the inverse problem , that seemed inappropriate here . The observed lines are quite shallow . The identifications of some of the blending lines are uncertain , which does not allow us to treat them ...
Page 246
... lines measured by Wright were usable . Lines were identified on the tracings with the aid of Davis ' ( 1947 ) identification of the spectrum of ẞ Pegasi . Lines denoted as blended in that reference were not measured . Many additional lines ...
... lines measured by Wright were usable . Lines were identified on the tracings with the aid of Davis ' ( 1947 ) identification of the spectrum of ẞ Pegasi . Lines denoted as blended in that reference were not measured . Many additional lines ...
Page 877
... lines and extremely broad emission features , especially at the He II lines . Identifications for some lines are marked . 1-5 1991 give V = 15.585 ± 0.011 . There are just two images each in U and B , but they yield ( B - V ) = + 0.834 ...
... lines and extremely broad emission features , especially at the He II lines . Identifications for some lines are marked . 1-5 1991 give V = 15.585 ± 0.011 . There are just two images each in U and B , but they yield ( B - V ) = + 0.834 ...
Other editions - View all
Common terms and phrases
abundance additional analysis appear associations assumed Astronomical average binary blue bright calibration catalog central clouds cluster color compared correction derived detection determined discussed distance distribution dwarf eclipse effects emission errors estimate et al evidence evolution field Figure flux frame function galaxies giants given groups included increase indices less light limit lines luminosity magnitude mass mean measured MNRAS nebulae noted objects observations obtained optical orbital PASP period phase photometric pixels position possible present probably quasars range ratio reduced reference region relation relative rotation sample scale scatter secondary shown similar sources spectral spectrum standard stars stellar stellar winds suggests surface survey Table telescope temperature tion University values variability velocity wavelength X-ray