Search Publications
A library of IUE white dwarf spectra for stellar population analyses.
Bonatto, C.; Bica, E.; Giovannini, O.
We present high Signal to Noise ratio IUE spectra of different classes of white dwarfs, to be used as templates for stellar population analyses in the ultraviolet region. We present average stellar parameters associated to each group. The library contains 6 groups for DA's, 2 for DO's and 5 for DB's. We also present equivalent widths of spectral f…
First catalogue of stars with the photoelectric astrolabe in San Juan.
Wang, Z.; Zhao, G.; Lu, L. +9 more
On the basis of data observed in San Juan of Argentina with the photoelectric astrolabe mark II (PA II) of Beijing Astronomical Observatory from 23 Feb., 1992 to 28 Feb., 1995, residuals of 7200 stars are reduced from about 230000 observations of stars. The mean precision of the residuals is +/-0.046". Using the data, the first catalogue of stars …
Astrometric positions of stars associated with nebulosities in the southern hemisphere.
Rousseau, J. M.; Perie, J. P.
Several stars associated with nebulosities and cited by S. van den Bergh and W. Herbst are included in the preliminary programme for the HIPPARCOS mission. When performing preparatory measurements of plates, we encountered difficulties in identifying certain of these objects when relying only on coordinates, which led us to take advantage of this …
EUV spectral lines from solar wind source regions: The resonance doublets of N V, MG X and SI XII, and the Fe XII λ1242 forbidden line.
Spadaro, D.; Ventura, R.
We present numerical simulations of intensities and profiles of the N V λ1239 and λ 1243, Mg X λ610 and λ625, Si XII λ499 and λ521, and Fe XII λ1242 lines expected from an equatorial and polar coronal hole at solar minimum, when observed on the plane of the sky in the 1.2Rsun_-8Rsun_ range of heliocentric distance. The radial…
Geminga in the Space Telescope Era.
Caraveo, P. A.; Bignami, G. F.; Mignani, R. +1 more
The distance to Geminga inferred from the γ-ray flux, the interstellar absorption of the soft X-ray emission and the proper motion measured for its optical counterpart, range from tens of parsecs to an upper limit of severl hundreds of parsecs. These distance estimates, however, are based on a number of assumptions on the emission mechanisms, on t…