Hostname: page-component-84b7d79bbc-fnpn6 Total loading time: 0 Render date: 2024-07-29T05:06:04.439Z Has data issue: false hasContentIssue false
  • English
  • Français

Flare-Like Events on the T-Tauri Star RU LUP1*

Published online by Cambridge University Press:  27 September 2017

F. Giovannelli ,
D. Castaldo ,
E. Covino ,
A.A. Vittone  and
C. Rossi
F. Giovannelli
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Frascati, Italy
D. Castaldo
Affiliation:
Osservatorio Astronomico di Capodimonte, Napoli, Italy
E. Covino
Affiliation:
Osservatorio Astronomico di Capodimonte, Napoli, Italy
A.A. Vittone
Affiliation:
Osservatorio Astronomico di Capodimonte, Napoli, Italy
C. Rossi
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Frascati, Italy

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A long term multifrequency campaign on the T Tauri star RU Lupi has been carried out in the X-Ray, UV optical and IR spectral regions with ASTRON and IUE satellites and ESO 1.5 m+IDS, 1.4 m CAT, 0.5 m UBVRI and 1 m IR telescopes, respectively.

We present two flare-like events occurred on April 17, 1984 and June 30, 1986. The first one was detected only in the UV, clue to lack the of simultaneous observations in other spectral regions. The second one was observed in UV, optical and IR regions showing a maximum roughly in the U band A comparison of the whole energy distribution of this event with that of a quiescent state observed on June 27 shows a flux enhancement of (89 ± 2)%. A detailed analysis of UV continuum and lines, namely N V, C I, CII, CIV, Si II and Si IV, shows that ihe surfaces fluxes of RU Lupi are always larger than those observed on typical flare stars and on the Sun by a factor of roughly 2 and 3 orders of magnitude, respectively. This fact allows us to conclude that RU Lupi activity cannot be explained even invoking a complete coverage by solar-like plages. On the contrary a patchy distribution of the emitting regions could explain the observed behaviour of this active star.

Type
Session I: Stellar Flares
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 139 - 142
Copyright
Copyright © Kluwer 1989

Footnotes

*

based on observations carried out at VILSPA with IUE satellite and at La Silla with ESO telescopes.

References

Bisnovatyi-Kogan, G.S., Lamzin, S.A.: 1977, Sov. Astron., 21, 720 Google Scholar
Covino, E., Errico, L., Vittone, A.A., Giovannelli, F.: 1988, Proceeding Convegno Nazionale Frascati, February 17-19, 1988. Google Scholar
Covino, E., Terranegrs, L., Vittone, A.A.: 1988, Mem. S.A.It., in press Google Scholar
Gahm, F.G., Nordh, H.L., Olofsson, S.G.: 1975, Icarus, 24, 372.Google Scholar
Gahm, F.G., Fregda, Kerstin, Liseau, R., Dravins, D.: 1979, Astron.Astrophys. Letters, 73, L4.Google Scholar
Giovannelli.F., Bisnovatyi-Kogan, G.S., Golynkaya, I.M., Kurt, V.G., Lamzin, S.A., Mizyakina, T.A., Shafer, E.Yu., Shamolin, V.M., Sheffer, E.K., Smirnoff, A.S., Vittone, A.A.: 1984, in Fourth European IUE Conference, ESA-SP 218, 359.Google Scholar
Giovannelli, F., Vittone, A.A., Rossi.C, Nastari,I., Bisnovatyi-Kogan, G.S., Golynskaya, I.M., Kurt, V.G., Mizyarkina, T.A., Shafer, E.Yu., Shamolin, V.M., Sheffer, E.S., Smirnoff, A.S., Lmzin, S.A., Larionov, M.G., Sidorenko, V.N.: 1986, in New Insight in Astrophysics, ESA-SP 263, 95.Google Scholar
Giovannelli, F., Rossi, C., Errico, L., De Martino, D., Vittone, A.A.: 1987, Convegno di Astronomia Infrarossa, Vulcano, September 14-18, Mem. S.A.It., 58, 205.Google Scholar
Giovannelli, F., Rossi, C., Covino, E., Errico, L., Vittone, A.A., Bisnovatyi-Kogan, G.S., Kurt, V.G., Sheffer, E.S., Lamzin, S.A.: 1988, in A Decade of UV Astronomy with WE, ESA-SP 281, vol.2, 101.Google Scholar
Lago, M.T.V.T.: 1982, Mon. Not. R. astr. Soc., 198, 445.Google Scholar
Schwartz, R.D., Heuermann, R.W.: 1981, Astron. J., 86, 1526.Google Scholar