February 10, 2017: Dr. Ed Sion (Villanova University) and colleagues have requested AAVSO observers' assistance in monitoring the symbiotic-type recurrent nova IM Nor in support of observations with the Hubble Space Telescope Cosmic Origins Spectrograph scheduled for 2017 February 13 - 17 UT.
These observations are part of a study on short orbital period recurrent novae as Supernovae Type Ia progenitors.
October 19, 2016: Dr. Edward Sion (Villanova University) has requested AAVSO observers' assistance in monitoring the recurrent nova CI Aql in support of observations with the Hubble Space Telescope Cosmic Origins Spectrograph scheduled for October 31 - November 2, 2016, and November 3 - November 5, 2016. These observations are part of a study on short orbital period recurrent novae as Supernovae Type Ia progenitors.
October 4, 2016: Dr. Ashley Pagnotta (Louisiana State University) has requested AAVSO assistance in monitoring the recurrent nova V2487 Oph in order to catch and observe its next outburst.
April 8, 2016: The symbiotic recurrent nova T CrB has entered a super-active state, and it is brighter and bluer than it has been since before its last outburst in 1946. Multicolor and visual ongoing observations are requested.
February 13, 2006: The recurrent nova RS Oph appears to be in a very rare outburst, as seen by the following AAVSO observations:
FEB 13.1631 2453779.6631 4.8 Visual RWG Wolfgang Renz, Germany
FEB 10.2100 2453776.71 11.0 Visual GRL Bjorn Granslo, Norway
FEB 08.2493 2453774.7493 10.9 Visual GZN Alfredo Gonzales-Herrera, Spain
The outburst was first detected by Kiyotaka Kanai (Gunma,Isezaki-shi) and Hiroaki Narumi (Ehime,Kita-gun) and reported to the VSNet-Alert mailing list.
January 28, 2010: The recurrent nova U Sco has been reported in outburst, and confirming observations and immediate reporting are urgently requested.
U Sco is located at coordinates RA: 16 22 30.80 , Dec: -17 52 43.0 (J2000).
February 8, 2010: Dr. Bradley Schaefer has requested increased optical coverage of the recurrent nova U Scorpii through the end of February 2010 at least. Of greatest interest are calibrated multicolor photometry to follow the evolution of the optical spectrum throughout the outburst, and intensive time-series photometry to study flickering in the system and to time the eclipses. Recent photometry of U Scorpii has indicated that the nova ejecta shell has become optically thin, making the central star visible again.