Lines unaffected by polarization (Vela Villahoz+ 1994)
Not Available (2 data files).
Vela Villahoz, E. et al.
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1993
This section contains the publications database that collects IAC articles published in scientific journals. Please, click on the arrow to see full search filter and sort options: author, journal, year, etc..
It also provides access to IAC Preprints Repository here: https://research.iac.es/preprints/
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Li abundances in galactic C-stars (Boffin+ 1993)The equivalent widths and abundances of Lithium in galactic carbon stars are presented in Table 1. The observations were made during 1990 and 1991 in 3 different observatories: Roque de los Muchachos and Calar Alto (Spain), and La Silla (Chile). The resolving power of the spectra is 15000-2000 for the spanish observations, and about 60000 for theBoffin, H. M. J. et al.
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Hidden supernova remnants in the Large Magellanic Cloud H II complex N44We have obtained ROSAT PSPC observations of N44, one of the largest H II complexes in the Large Magellanic Cloud. The X-ray emission mostly fails within the ionized shell structures in N44. We find that one faint shell is a classical supernova remnant overlooked by previous surveys. If we model the two largest shells as pressure-driven superbubblesKennicutt, Robert C., Jr. et al.
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GRO J0422+32IAUC 5860 available at Central Bureau for Astronomical Telegrams. IAUC 5860 available at Central Bureau for Astronomical Telegrams.Zhao, P. et al.
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EVOLUCION TEMPRANA DE ESTRELLAS POCO MASIVAS Y OBJETOS EN EL LIMITE SUBESTELAREN ESTA TESIS DOCTORAL SE HAN ESTIMADO LAS ABUNDANCIAS DE LITIO EN UNA AMPLIA MUESTRA DE ESTRELLAS CON TIPOS ESPECTRALES G,K Y M, QUE COMPRENDEN DESDE LA FASE T TAURI HASTA LA EDAD DE LAS PLEYADES (-100 MILLONES DE AÑOS), PARA AYUDAR AL ENTENDIMIENTO DE LA EVOLUCION DE LAS ESTRELLAS JOVENES. LA BASE DE ESPECTROS DE RESOLUCIONES ALTA O INTERMEDIAEDUARDO LORENZO MARTIN GUERRERO DE ESCALANTE
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Evidence for an offset active nucleus in the Seyfert galaxy NGC3227THE active nuclei of Seyfert 1 galaxies are characterized by a small (˜0.03 pc) region of intense broad emission lines, indicative of gas moving at extremely high velocities and ionized by a non-thermal radiation field. These spectral features are usually explained by invoking the presence of a central supermassive black hole. Here we present twoMediavilla, E. et al.
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91993