Zobrazeno 1 - 2
of 2
pro vyhledávání: '"Johannessen F."'
Autor:
Mukadam A. S., Kepler S. O., Winget D. E., Nather R. E., Kilic M., Mullally F., Hippel T. von, Kleinman S. J., Nitta A., Guzik J. A., Bradley P. A., Matthews J., Sekiguchi K., Sullivan D. J., Shobbrook R. R., Birch P., Jiang X. J., Xu D. W., Joshi S., Ashoka B.N., Ibbetson P., Leibowitz E., Ofek E. O., Meištas E. G., Janulis R., Ališauskas D., Kalytis R., Handler G., Kilkenny D., O’Donoghue D., Kurtz D. W., Müller M., Moskalik P., Ogłoza W., Zoła S., Krzesiński J., Johannessen F., Gonzalez-Perez J. M., Solheim J-E., Silvotti R., Bernabei S., Vauclair G., Dolez N., Fu J. N., Chevreton M., Manteiga M., Súarez O., Ulla A., Cunha M. S., Metcalfe T. S., Kanaan A., Fraga L., Costa A. F. M., Giovannini O., Fontaine G., Bergeron P., O’Brien M. S., Sanwal D., Wood M. A., Ahrens T. J., Silvestri N., Klumpe E. W., Kawaler S. D., Riddle R., Reed M. D., Watson T. K.
Publikováno v:
Open Astronomy, Vol 12, Iss 1, Pp 71-103 (2003)
We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. Based on observations that span 31 years, we conclude that the period 213.132605 s observed in ZZ Ceti
Externí odkaz:
https://doaj.org/article/2f43468678c44bc7b5f349f3b424d8fd
Autor:
Kurtz D. W., Kawaler S.D., Riddle R. L., Reed M.D., Cunha M. S., Wood M., Silvestri N., Watson T.K., Dolez N., Moskalik P., Zola S., Pallier E., Guzik J.A., Metcalfe T. S., Mukadam A., Nather R.E., Winget D.E., Sullivan D. J., Sullivan T., Sekiguchi K., Jiang X.J., Shobbrook R.R., Birch P.V., Ashoka B. N., Seetha S., Joshi S., Girish V., O’Donoghue D., Handler G., Mueller M., Perez J.M. Gonzalez, Solheim J.-E., Johannessen F., Ulla A., Kepler S.O., Kanaan A., Costa A.da, Fraga L., Giovannini O., Matthews J. M., Cameron C., Vauclair G., Nitta A., Kleinman S. J.
Publikováno v:
Open Astronomy, Vol 12, Iss 1, Pp 105-117 (2003)
HR1217 is a prototypical rapidly oscillating Ap star that has presented a test to the theory of nonradial stellar pulsation. Prior observations showed a clear pattern of five modes with alternating frequency spacings of 33.3 μHz and 34.6 μHz, with
Externí odkaz:
https://doaj.org/article/4538bab4b5ef4b12b0054b3ec3821434