RT Book, Section
T1 The relevance and future of the ultraviolet range
A1 Gómez de Castro, Ana Inés
A1 Pagano, Isabella
A1 Linsky, Jeff
AB To progress in our understanding of cool stars is instrumental to have access to UV (mid-high resolution) spectroscopy. In fact, the UV range supplies a richness of experimental data which is unmatched by any other spectral domain for the study of astrophysical plasmas since (1) almost all the resonance lines of all elements, covering plasmas from the coolest regimes (10-1000K) up to hot (some 10(5)K) temperatures are observed in the UV range, (2) the electronic transitions of the most abundant molecules, such as 112, are in the ultraviolet which is also sensitive to the presence of large molecules such as the PAHs and (3) some strong coronal lines (Fe XXII, Fe XVIII, Fe XXI) axe also observed in this range. As a consequence UV spectroscopy is instrumental to make advance on some of the key problems of modern astrophysics such as the formation of solar-like stars and planetary systems or the understanding of the solar-stellar connection and eventually of the Sun in a broad galactic context. Amazingly enough, the situation of (mid-high resolution) UV Spectroscopy is precarious; there is not any facility available in the whole planet Earth (unless FUSE that works in a very small Far-UV range) and no firm plans exist for the future. Only concerted efforts by the community will supply the information required to have the space agencies decide to release the funding needed for the support of these important Astrophysical study capabilities. This splinter session has been devoted to highlight the relevance of the UV range for the understanding of Cool Stars and to seek for world-wide coordination.
PB European Space Agency
SN 92-9092-871-9
YR 2005
FD 2005
LK https://hdl.handle.net/20.500.14352/53142
UL https://hdl.handle.net/20.500.14352/53142
LA eng
NO Ayres, T. R., Brown, A., Harper, G.M., Osten, R.A., Linsky, J. L., Wood, B. E., Redfield, S., 2003, ApJ, 583, 963Bus`a, I., Pagano, I., Rodon`o, M., & Neff, J.E. 1999, A&A, 350, 571Franchini, M., Morossi, C., Malagnini, M. L. 1998, ApJ 508, 370Gómez  de Castro, A.I., Franqueira, M., 1997, ULDA Access Guide to T Tauri Stars, ESA Pub.Gómez  de Castro, A.I., 2002, MNRAS, 332, 409Gómez  de Castro, A.I., Verdugo, V., 2003, ApJ, 597, 443Gómez  de Castro, A.I., 2004, ApSS, 292, vol.4Gómez  de Castro, A.I., Wamsteker, W., 2004, Lecture Notes and Essays in Astrophysics, in pressHerczeg, G.J., Linsky, J.L., Valenti, J.A., Johns-Krull, C.M., Wood, B.E., 2002, ApJ, 572, 310Hudson, H. S. 1991, Sol. Phys., 133, 357Lanzafame, A. C., Bus`a, I., & Rodon`o, M. 2000, A&A 362, 683Low, B.C., 2001, JGR, 106 (A11), 25141Muzzerolle, J., Calvet, N., Hartmann, L., D’Alessio, P., 2003, ApJ, 597, L149Pagano, I., Linsky, J.L., Carkner, L., Robinson, R.D., Woodgate, B., & Timothy G. 2000, ApJ, 532, 497Pagano, I., Rodon`o, M., Linsky, J. L., Neff, J. E., Walter, F. M., Kov´ari, Zs., & Matthews, L. D. 2001, A&A 365, 128Pagano, I., Linsky, J. L., Valenti, J., & Duncan, D. K. 2004, A&A 415, 331Redfield, S., Ayres, T.R., Linsky, J.L., Ake, T.B., Dupree, A.K., Robinson, R.D., & Young, P.R. 2003, ApJ 585, 993Robinson, R.D., Linsky, J.L., Woodgate, B., & Timothy G. 2001, ApJ 554, 368Uzdenski, D., 2004, ApSS, 292, vol. 4Valenti, J.A., Johns-Krull, C.M., Linsky, J.L., 2000, ApJS, 129, 399Vidal-Madjar, A.; Lecavelier des Etangs, A., D´esert, J.-M.; Ballester, G. E.; Ferlet, R.; H´ebrard, G.; Mayor, M., 2003, Nature, 422, 143Vilhu, O., Muhli, P., Huovelin, J., Hakala, P., Rucinski, S. M., Collier Cameron, A., 1998, AJ, 115, 1610Wood, B.E.,Linsky, J.L., M¨uller, H.–R., & Zank, G.P. 2001, ApJ 547, L49Wood, B.E., M¨uller, H.–R., Zank, G.P., & Linsky, J.L., 2002, ApJ 574, 412
NO 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, JUL 05-09, 2004, Hamburg, GERMANY
DS Docta Complutense
RD 2 may 2024