Previous outbursts of V745 Sco occurred in 1937 and 1989. The 1937 outburst was detected in 1958 (in decline at magnitude 11.0 on 1937 May 11,; the outburst had occurred within the previous 19 days) by Lukas Plaut on plates taken by Hendrik van Gent at the Leiden Observatory; the object was later assigned the GCVS name V745 Sco. On July 30, 1989, William Liller discovered on a sky patrol film a 10th magnitude star that was not there the night before. Its position coincided with the nova that flared up on May 10, 1937, known as Nova Sco 1937 = V745 Sco.
V745 Sco 2014 Eruption
On February 6, 2014, I detected V745 Sco in outburst during an early morning observing session. This was the third outburst since the discovery in 1937 and the first visual detection of an outburst of V745 Sco!
The first CCD image was taken by Steve O’ Connor (OCN, St. Georges, Bermuda) shown below at maximum light remotely using the iTel17, Siding Spring, NSW, Australia. (centre of image).
Alert Notice 496: Outburst of the recurrent nova V745 Sco
February 7, 2014
Event: Outburst of the recurrent nova V745 Sco
Discovery by: Rod Stubbings (Tetoora Road, VIC, Australia)
Discovery magnitude: 9.0 (visual)
Discovery date: 2014 February 6.694 UT
Coordinates: R.A. 17 55 22.27 Dec. -33 14 58.5 (2000.0)
Observing Recommendations: This recurrent nova is fading quickly. Follow-up observations of all types (visual, CCD, DSLR) are strongly encouraged, as is spectroscopy. V745 Sco is currently a pre-dawn object, posing an additional challenge. AAVSO Nova Section advisor Dr Jeno Sokoloski (Columbia University) has requested as much photometry and spectroscopy as possible. Professional researchers are planning multiwavelength observations for V745 Sco, and your observations will be extremely important for correlation of these multiwavelength data.
Outbursts of recurrent novae are relatively rare events. Each outburst is an opportunity to add to the study of the relationship between recurrent novae and the progenitors of Type-Ia supernovae, so the most complete coverage possible is important.
Dr Bradley Schaefer (Louisiana State University) suggests that fast time-series of this nova may be useful to detect possible flaring activity as was observed during the outburst of U Scorpii in 2010. He suggests that coincident time-series by multiple observers would be most useful for such a study, with a V-filter being preferred.
Observations reported to the AAVSO:
2013 Oct. 27.41528 UT, 28.42639, 28.44375, 29.44167, 2014 Jan. 12.73958, Feb. 01.1, 13.98 I (MLF, L. Monard, Calitzdorp, South Africa, via cba-chat);
03.1, 13.78 I (Monard, via cba-chat);
05.696, 06.694, 9.0 (Stubbings);
06.745, 9.0 (CMQ, P. Camilleri, Warners Bay, Newcastle, NSW, Australia);
06.77330, 8.66 V +/-0.06 (OCN, S. O’Connor, St. Georges, Bermuda, remotely using iTel17, Siding Spring, NSW, Australia);
06.77390, 9.46 B +/-0.07 (O’Connor, remotely);
06.77450, 7.98 R +/-0.05 (O’Connor, remotely);
07.102, 9.04 V (Monard, via cba-chat);
07.104, 7.40 I (Monard, via cba-chat);
07.34557, 9.483V +/-0.010 (HMB, J. Hambsch, Mol, Belgium, remotely at San Pedro de Atacama, Chile);
07.35522, 9.485 V +/-0.010 (Hambsch, remotely);
07.36012, 9.490 V +/-0.009 (Hambsch, remotely);
07.36503, 9.520 V +/-0.008 (Hambsch, remotely);
07.37016, 9.515 V +/-0.009 (Hambsch, remotely);
07.37464, 9.508 V +/-0.008 (Hambsch, remotely);
07.38047, 9.549 V +/-0.008 (Hambsch, remotely);
07.38520, 9.563 V +/-0.008 (Hambsch, remotely);
07.76300, 10.07 V +/-0.03 (O’Connor, remotely);
07.76500, 8.91 R +/-0.09 (O’Connor, remotely);
07.76600, 8.15 I +/-0.01 (O’Connor, remotely);
07.80903, 10.1 (PEX, A. Pearce, Nedlands, W. Australia);
07.85833, 10.2 (Pearce);
Charts: Charts for V745 Sco may be created using the AAVSO Variable Star Plotter (VSP) at http://www.aavso.org/vsp.
Submit observations: Please submit observations to the AAVSO International Database using the name V745 SCO.
a. Initially announced in AAVSO Special Notice #380 (M. Templeton).
b. Confirmed by Steve O’Connor (OCN, St. Georges, Bermuda) and Paul Camilleri (CMQ, Warners Bay, Newcastle, NSW, Australia); see Observations above.
c. Previous outbursts occurred in 1937 and 1989. The 1937 outburst was detected in 1958 (in decline at magnitude 11.0 on 1937 May 11.1 UT; outburst had occurred within the previous 19 days) by Lukas Plaut on plates taken by Hendrik van Gent at the Leiden Observatory; the object was announced as Nova Sco 1937 and later assigned the GCVS name V745 Sco. The 1989 outburst was detected on 1989 July 30.08 UT by William Liller (LIW, Vina del Mar, Chile), at magnitude 9.7 (PROBLICOM discovery using 2415 film with orange filter). [This Alert Notice originally reported that the 1989 outburst was discovered on 1989 August 1.55 UT by Mati Morel (MMAT, Thornton, NSW, Australia) at visual magnitude 10.4 and in decline. Morel’s observation was the first one recorded in the AAVSO International Database, not the discovery one. Our sincere apologies to Bill Liller for the error.]
d. Dr Bradley Schaefer (Louisiana State University) reports (2010ApJS..187..275S) in his comprehensive analysis of the 10 known galactic recurrent novae (including V745 Sco) that the median interval between recurrent novae outbursts is 24 years. The interval since the 1989 outburst of V745 Sco is 24.10 years.
Congratulations to Rod Stubbings on his detection of the outburst of this difficult pre-dawn recurrent nova!
This AAVSO Alert Notice was prepared by Elizabeth O. Waagen.
The professional community were pursuing this one with multiwavelength observations (including satellite X-ray and gamma-ray observations, and radio observations).
The Astronomers Telegram
Evolving early, hard X-ray emission of V745 Sco
Near-infrared observations of recurrent nova V745 Sco
Nova V745 Sco shows fastest rise of super-soft X-ray emission: 3-4 days after eruption
Optical observations of the recurrent nova V745 Sco
Early Optical Spectroscopic Evolution of V745 Sco
The symbiotic recurrent nova V745 Sco is confirmed as a bright super-soft source.
Fermi-LAT Gamma-ray Observations of Recurrent Nova V745 Sco
Detection of Rising Radio Emission from V745 Sco
Fading and probable quasi-periodic oscillation in the Swift X-ray observations of symbiotic recurrent nova V745 Sco
NuSTAR observation of V475 Sco
Chandra detection of X-ray emission lines from the blast wave of V745 Sco