QR Vul - HD192685 - HR 7739
AD: +20 15 15.9 - DEC: +25 35 31.0 - Mag: 4.759 - Sp: B3Ve
QR Vul is a Be Star, identified as variable in photometry - K. Pavlovski et al UBV photometry of Be stars at Hvar: 1972-1990
During our observing session at the Spectro Workshop at the Observatory of Haute-Provence, an outburst was first reported in August 2008. The H-alpha line showed a double peak emission as the previous observation in Sept 2007 was showing the line in absorption. The emission completely disappeared between march 2009 and June 2009.
A new outburst has been again observed during the 2011 OHP spectro workshop. As this star was more closely monitored thanks to the ArasBeAm portal linked to the Be spectrum database BeSS (GEPI- Meudon, Paris Observatory), it seems the outburst occured between June 2nd and August 1st.
H-alpha line - Heliocentric velocity corrected, atmospheric lines removed
From V.Desnoux (Paris, June with C9 - Lhires3 and 1200 l/mm grating - OHP, August with C8 - Lhires3 and 2400l/mm grating)
Using the spectra collected in the BeSS database, it was interesting to look at the equivalent width evolution as a marker of the emission strengh of the H-alpha line. All data processed using Visual Spec. Error on the equivalent width is calculated using the formula from Chalabaev, A. and Maillard, J.P. (1983) - it takes into account the S/N calculated on the region 6592-6595 angstrom and the sampling factor.
Equivalent Width evolution over time computed on all the spectra from the BeSS database
Zoom on the 3 years period from the last observed outburst
Time diagram summary of the H-alpha line - first spectrum in 2003, By C.Neiner at Pic du Midi
The continuum is scaled in the region 6592-6595 angstrom - Heliocentric velocity is corrected using the values in the header of the BESS VO-Table file. This page is generated by Visual Spec.
Some Articles referring to QR Vul
Pavlovski & Bozic 1982; Harmanec et al. 1982b; Barker 1982