Coordinated observations of stellar flares were obtained with lUE and several ground-based facilities in March 1984.The simultaneous observations allowed it to cover a wide range of wavelengths from ii5nm to 6cm.We intend to study the effect ofthe observed flares at different atmospheric heights in order to estimate the energy budget,the time scales and the cooling processes.Our observations includetime-resolved IUE spectroscopy at SWP(115-195nm) and LWP(190-320nm),optical spectroscopy at the ESO 3.6m+IDS (355-440nm),high resolution spectroscopy at the ESO 1.4m CAT+CES(653-659nm),narrow band H alpha and wide band optical photometry, infrared photometry at 2.2microns and microwave observations at 2,6 and 20 cm We present for some flare events,among the results,the first detection of infrared flux decrease -or "negative flare"-in coincidence with the flux increase at the other wavelengths:the broadening and changes of the Balmer H lines,He and high excitation lines;the appearance of higher members of the Balmer serie;the enhancements of Mg II doublet and Fe II blend (260nm);and the flare detection at 2cm and 6cm

Coordinated IUE and ground-based observations of stellar flares: YZ CMi, Proxima Cen and AD Leo

Russo, G.;
1986

Abstract

Coordinated observations of stellar flares were obtained with lUE and several ground-based facilities in March 1984.The simultaneous observations allowed it to cover a wide range of wavelengths from ii5nm to 6cm.We intend to study the effect ofthe observed flares at different atmospheric heights in order to estimate the energy budget,the time scales and the cooling processes.Our observations includetime-resolved IUE spectroscopy at SWP(115-195nm) and LWP(190-320nm),optical spectroscopy at the ESO 3.6m+IDS (355-440nm),high resolution spectroscopy at the ESO 1.4m CAT+CES(653-659nm),narrow band H alpha and wide band optical photometry, infrared photometry at 2.2microns and microwave observations at 2,6 and 20 cm We present for some flare events,among the results,the first detection of infrared flux decrease -or "negative flare"-in coincidence with the flux increase at the other wavelengths:the broadening and changes of the Balmer H lines,He and high excitation lines;the appearance of higher members of the Balmer serie;the enhancements of Mg II doublet and Fe II blend (260nm);and the flare detection at 2cm and 6cm
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11588/892441
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