![]() ![]() This pair of lines should, therefore, yield new data about densities in observed H II regions or else, if density data already are available from radio or other observations, the lines can be used to determine the differential dust absorption between 52 and 88 micron in front of heavily obscured regions. Observations of the 51.8 (O III) line are particularly important since the previously discovered 88 micron line from the same ion also is strong. The line lies close to an atmospheric water vapor feature at 51.7 micron, but is sufficiently distant so that corrections for this feature are straightforward. Observations are consistent with the newly predicted 51.8 micron line position. ![]() #WAS THE BENSEN B9 LITTLE ZIPSTER FIXED PITCH ROTOR PLUS#The observed line strength is of 5 plus or minus 3 times 10 to the minus 15th power watt/sq cm is in good agreement with theoretical predictions. The 51.8 micron fine structure transition P2:3P2 3P1 for doubly ionized oxygen was observed in the Orion nebula. Observations of the 51.8 micron (O III) emission line in Orion Model spectral results are used to confirm the production of the UV emission lines by photoionization from X-ray and EUV photons. Our new UV observations and additional archival IUE spectra were used to discover a correlation between the strength of the high-state UV emission lines and the strength of the white dwarf magnetic field. Continuum flux distributions for these stars (from 100 to 5500 Ã…) reveal that over this entire range, none of the spectral energy distributions can be fitted by a single-valued blackbody. ![]() The high-state UV spectra are dominated by strong emission lines. Using the^ International Ultraviolet Explorer (IUE), 1200-3400 Ã… spectra were obtained of the AM Herculis stars RE 0531-46, RE 1149+28, RE 1844-74, QS Tel (RE 1938-46), and HU Aqr (RE 2107-05) and the DQ Herculis star PQ Gem (RE 0751+14). We present the first UV spectral observations of six magnetic cataclysmic variables discovered by the ROSAT Wide Field Camera (WFC). The Relationship between Ultraviolet Line Emission and Magnetic Field Strength in Magnetic Cataclysmic Variables ![]() Iron lines strongly dominate the identifications in the 2250-2930 A region, Fe II accounting for about 86 percent of the emission features and Fe I for 43 percent of the identified absorption features. A search for molecular absorption features in the 2500-2930 A interval has led to several tentative identifications, but only OH could be established as definitely present. Chromospheric emission lines have been identified with low-excitation species including H I, C I, C II, O I, Mg I, Mg II, Al II, Si I, Si II, S I, and Fe II there is no evidence for lines of C IV, N V, or other species requiring high temperatures. In the 1150-2000 A region, identifications are given primarily on the basis of low-resolution spectra. Line identifications, mean absolute 'continuum' flux measurements, integrated absolute emission- line fluxes, and measurements of selected absorption line strengths are presented for the 2250-2930 A region. The ultraviolet spectrum of Arcturus has been observed at high resolution with the IUE satellite. Line identifications, line strengths, and continuum flux measurements in the ultraviolet spectrum of ArcturusĬarpenter, K. ![]()
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |