Zobrazeno 1 - 2
of 2
pro vyhledávání: '"Scheggia, I."'
Autor:
Fauvaud, S., Sareyan, J. -P., Ribas, I., Rodríguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, J. H., Wolf, M., Santacana, G., Zhou, A. -Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., López-González, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. -J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Král, L., Kocián, R., Kučáková, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. -M., Kotková, L., Truparová, K., Ulusoy, C., Yasarsoy, B., Avdibegovic, A., Blauzek, M., Kliner, J., Zasche, P., Bartošíková, S., Vilášek, M., Trondal, O., Abbeel, F. Van Den, Behrend, R., Wücher, H.
Short-period high-amplitude pulsating stars of Population I ($\delta$ Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational behaviours, only one or two rad
Externí odkaz:
http://arxiv.org/abs/1004.2748
Autor:
Fauvaud, S., Sareyan, J. -P., Ribas, I., Rodriguez, E., Lampens, P., Klingenberg, G., Farrell, J. A., Fumagalli, F., Simonetti, J. H., Wolf, M., Santacana, G., Zhou, A. -Y., Michel, R., Fox-Machado, L., Alvarez, M., Nava-Vega, A., Lopez-Gonzalez, M. J., Casanova, V. M., Aceituno, F. J., Scheggia, I., Rives, J. -J., Hintz, E. G., Van Cauteren, P., Helvaci, M., Yesilyaprak, C., Graham, K. A., Kral, L., Kocian, R., Kucakova, H., Fauvaud, M., Granslo, B. H., Michelet, J., Nicholson, M. P., Vugnon, J. -M., Kotkova, L., Truparova, K., Ulusoy, C., Yasarsoy, B., Avdibegovic, A., Blazek, M., Kliner, J., Zasche, P., Bartosikova, S., Vilasek, M., Trondal, O., Van Den Abbeel, F., Behrend, R., Wuecher, H.
WOS: 000280505000008
Context. Short-period high-amplitude pulsating stars of Population I (delta Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational
Context. Short-period high-amplitude pulsating stars of Population I (delta Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=od______9436::a06cea3b29f8d7d8fb630d7fb8a4e800
https://hdl.handle.net/11454/43750
https://hdl.handle.net/11454/43750