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ASASSN-18jj: classical nova (12.1 mag) in the LMC

AAVSO Alert Notice 633

Nova eruption of V392 Persei = TCP J04432130+4721280

30 April 2018

Event: Nova in Perseus – V392 Per = TCP J04432130+4721280

Discovered by: Yuji Nakamura (Kameyama, Mie, Japan; via CBET 4515)

Discovery magnitude: unfiltered CCD magnitude 6.2 (using a 135mm f4.0 lens; via CBET 4515)

Discovery date: 2018 April 29.474 UT (via CBET 4515)

Coordinates (2000.0): R.A. 04 43 21.38  Decl. +47 21 25.9  (from VSX)
Spectra: Hiroyuki Naito (Nayoro Observatory) and Tatsuharu Ono (Hokkaido University) report (via CBET 4515) that a low-dispersion spectrum of this object [V392 Per] was obtained on 2018 Apr. 29.58 UT using the 1.6-m Pirka telescope (+ NaCS) at the Nayoro Observatory. They report that "the spectrum shows some unidentified absorption lines on a very red continuum, which may indicate high reddening." Their spectrum can be viewed at URL

Robin Leadbeater (Wigton, Cumbria, UK) provides a R~500 spectrum taken on 2018 Apr. 29.894 UT at:

Spectroscopy indicating that V392 Per is undergoing a nova eruption was obtained by Wagner et al. (ATel #11588) on 2018 April 30.116 UT with the 2.4 m Hiltner telescope (+OSMOS) of the MDM Observatory on Kitt Peak. They report that "the spectrum is reminiscent of classical novae early in their outburst and prior to maximum light..."

Observing recommendations: Observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands (particularly B, V, I) as instrumentation permits are strongly encouraged as this bright nova evolves.

Observations reported to the AAVSO:
2017 Sep. 07.0674 UT, 16.65 CV +/-0.076 (E. Muyllaert, Oostende, Belgium);
Oct. 19.1389, 16.48 CV +/-0.030 (Muyllaert);
2018 Jan. 04.1153, <16.5 CV (Muyllaert);
Jan. 14.16786, 17.725 B  +/-0.141 (G. Stone, Auberry, CA);
Jan. 19.9181, <16.5 V (Muyllaert);
Mar. 08.0021, <16.5 CV (Muyllaert);
Apr. 21.4627, <12.5 unfiltered CCD (Y. Nakamura, Kameyama, Mie, Japan; via CBET 4515);
28.9687, 7.0 unfiltered DSLR (A. Uhrin, Randaberg, Norway, via CBET 4515);
29.0007, 7.0 unfiltered DSLR (Uhrin, via CBET 4515);
29.80600, 6.340 V +/-0.002  (T. Tordai, Budapest, Hungary);
29.81993, 6.35 CV +/-0.02 (P. Dubovsky, Kononica, Slovakia);
29.82058, 4.75 CI +/-0.01 (Dubovsky);
29.82058, 7.16 CB +/-0.04 (Dubovsky);
29.82111, -3.49 CR +/-0.03 (Dubovsky);
29.83194, 6.21 (M. Deconinck, Artignosc sur Verdon, France);
29.8507, 6.50 (I. Bryukhanov, Minsk, Belarus);
29.8694, 6.55 (Bryukhanov);
29.879, 7.3 C (J. Shears, Cheshire, UK);
29.904, 5.6 CR (D. Buczynski, Portmahomack, UK; via CBET 4515);
29.9135, 6.5 (V. Perekhrest, Ukraine);
29.9301, 6.537 V +/-0.037 (I. Miller, Swansea, UK);
29.9375, 6.5 (Uhrin);
29.9424, 7.488 B +/-0.088 (Miller);
29.9424, 6.4 (J. Toone, Shrewsbury, UK);
30.0410, 6.3 (J. O'Neill, Topsfield, MA);
30.0431, 6.8 (L. Shotter, Uniontown, PA);
30.0611, 6.5 (C. Chiselbrook, Canton, GA);
30.0955, 6.6 (S. Koontz, Houston, TX);
30.1007, 6.6 (C. Maloney, Helena, AR);
30.1111, 6.5 (H. Smith, East Lansing, MI);
30.116, 7.65 B (S. Kiyota, Kamagaya, Japan, remotely with 0.25-m f/3.4 astrograph + SBIG ST-10XME CCD (T5, iTelescope.NET at Mayhill, USA; via CBET 4515);
30.116, 6.73 V (Kiyota, via CBET 4515);
30.116, 5.23 Ic (Kiyota, via CBET 4515);
30.8167, 6.9 (G. Murawski, Suwalki, Poland);
30.8333, 6.9 (A. Tsvetkov, Zavolzhye, Russian Federation);
30.8736, 7.2 (M. Muciek, Kolobrzeg, Poland);
30.8743, 7.0 (A. Glez-Herrera, Ferrol, Spain);
30.8785, 7.0 (J. Ribeiro, Esposende, Portugal);
30.8799, 7.1 (A. Correia, Esposende, Portugal);
30.8903, 7.1 (Toone, via baavss-alert);
30.9028, 7.1 (Ribeiro);
30.9035, 7.1 (Correia);
30.9063, 7.1 (Glez-Herrera);

Charts: Charts with a comparison star sequence for V392 Per maybe created using the AAVSO Variable Star Plotter (VSP) and the name V392 Per. Observers need to be aware of a magnitude 15.0 star 8.5" to the North of the variable.

Submit observations: Please submit observations to the AAVSO International Database using the name V392 PER.

AAVSO Forums: V392 Per is the topic of the AAVSO Time Sensitive Alerts forum thread
and the AAVSO Novae forum thread

a. The object was designated TCP J04432130+4721280 when the report of a possible nova was posted to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). It was later determined that this object was the CV (UG-type dwarf nova) V392 Per. Information in this Alert Notice taken from CBET 4515 is noted as such. Other information was sent to the AAVSO via submissions to the AAVSO International Database, posts to the AAVSO forums, and emails.

b. The dwarf nova (UG) range of V392 Per was V = 14.1–16.9. Observations in the AAVSO International Database show bright dwarf nova outbursts of V392 Per in:
 - March (or earlier) 2013: max mag V=14.1 on ~Mar. 20; beginning of outburst unknown but at V=14.637(25) on March 5 (M. Simonsen, Imlay City, MI); return to quiescence unknown but at V=14.632(26) on April 23 (G. Sjoberg, Duxbury, MA); and
 - January 2016: max mag V=13.6 on ~Apr. 1; beginning of outburst ~Jan. 4 at V=15.945(44) (Simonsen); return to quiescence unknown but at V=14.513(48) on Apr. 27 (S. Johnston, Warrington, Cheshire, UK).

c. P. Schmeer (Saarbruecken-Bischmisheim, Germany) writes that "the ASAS-SN Sky Patrol recorded a dwarf nova outburst with a very slow (GK Per-like) rise in 2016 February/March....the very slow rise to outburst maximum indicates a long orbital period." He also reports V392 Persei is located 6 degrees WNW of alpha Aurigae (Capella).

d. Position end figures
- D. Buczynski (Portmahomack, UK, 2018 Apr. 29.9042 UT): 21.39s, 25.9"
- S. Kiyota (Kamagaya, Japan, 2018 Apr. 30.116 UT, via CBET 4515): 21.36s, 26.18"

e. Images
- D. Buczynski (Portmahomack, UK, 2018 Apr. 29.9042 UT):

Congratulations to Yuji Nakamura on his latest discovery!

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

AAVSO Alert Notice 617

Multiwavelength observations of YZ Cnc, SU UMa, and CR Boo outbursts

5 March 2018

Bob Jacobs (Ph.D. candidate, Radboud University) and Drs. Samaya Nissanke (Radboud University), Jennifer Barnes (Columbia University), and Deanne Coppejans (Northwestern University) have requested AAVSO observers' assistance in monitoring the cataclysmic variables YZ Cnc, SU UMa, and CR Boo. The goal is to build good multicolor light curves of two outbursts of CR Boo and two superoutbursts each of YZ Cnc and SU UMa.

Nightly observations of these stars in any Johnson-Cousins band are requested. When an appropriate outburst occurs, observers should switch to multiple observations per night in 3 or more (more preferred) Johnson-Cousins bands (U, B, V, R, I, J, H, K) spread across the spectrum if possible. It is essential to switch to the higher cadence and multiple bands as soon as possible after the outburst begins. Continue until the star returns to minimum, then resume nightly observations. Visual observations are welcome and are encouraged.

The astronomers want to catch the target outbursts as early as possible. If you see an outburst beginning, please notify the AAVSO immediately via the forum thread for this campaign, and submit your observation(s) as soon as possible.

The astronomers provide the following background information: "Last year's Nobel Prize in Physics went to three researchers in the field of gravitational waves. Two weeks later gravitational wave astronomers announced the discovery of a gravitational wave signal from a merger of two neutron stars. This system also emitted optical light right after the merger and it was observed by many telescopes on the southern hemisphere. The new type of transient was called a "kilonova" or "macronova". When two neutron stars merge, they emit large amounts of matter in ejecta (on the order of 1/100th-1/10th the mass of the Sun). These ejecta are neutron rich. Atoms in the ejecta will capture these neutrons and become much heavier than the atoms created in supernovae. They subsequently decay to stable elements like gold and platinum, heating up the ejecta and making it emit optical and infrared light. Kilonovae could account for all of the gold and platinum in the universe. That's why we would like to observe more kilonovae and test this hypothesis (plus many more). Kilonova observations will also put tighter constraints on gravitational waveforms and therefore the theory of General Relativity. Because kilonovae last for only ~10 days, it's important to catch them as early as possible, which requires good observing strategies.

"In order to observe more kilonovae the Radboud University, KU Leuven and NOVA are building the optical telescope BlackGEM in Chile. Upon an alert from the gravitational wave observatories, BlackGEM, together with other observatories, will try to discover the kilonova as quickly as possible. In order to find optimal observing strategies to find the kilonova as quickly as possible, we are trying to simulate how many transients of each type (e.g. Supernovae, dwarf novae, AM CVNs etc.) one would see in what parts of the sky with BlackGEM in each of its color-bands. These transients could be false-positives in the search for the kilonova: they may be indistinguishable from kilonovae. We want to have as few false-positives and as many correctly identified kilonovae as possible. The simulator will also be applicable in other fields of astronomy where estimates are needed for the variability of the night sky.

"For our simulation we use photometry from telescopes to model the temporal evolution of transients. Thanks to the AAVSO community we already have excellent multi-color light curves for SS Cyg and Z Cam type cataclysmic variable outbursts (U Gem and RX And). Unfortunately there aren't yet any light curves available for SU UMa or AM CVn type outbursts with sufficient multi-color coverage to use in our models.

"With your help we look forward to seeing the first well-sampled multi-color observations of CR Boo, SU UMa, and YZ Cnc in outburst."


Name R.A. (2000.0) Dec (2000.0)
YZ Cnc 08 10 56.65 +28 08 33.2
SU UMa 08 12 28.28 +62 36 22.3
CR Boo 13 48 55.22 +07 57 35.7

Charts with comparison star sequences for YZ Cnc, SU UMa, and CR Boo may be plotted using the AAVSO Variable Star Plotter (VSP).

Please submit observations to the AAVSO International Database using the names YZ CNC, SU UMA, and CR BOO.

This observing campaign is being followed on the AAVSO Campaigns and Observing Reports online forum at

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.

It’s all about the  standstills, those episodes where the star gets stuck at a mid-point between maximum and minimum. If it doesn’t exhibit standstills it isn’t a Z Cam star.

Data from Catalina Real Time Survey 

Drake et al. 2009, ApJ, 696, 87

Northern CVs brighter than 17th magnitude here.

Southern CV's brighter than 17th magnitude here.


Last updated 15:30 UT on 26 May 2018

New outbursts and unusual activity reported in the last 72 hours


TT Boo

V436 Cen
V442 Cen
X Leo
BV Pup
V729 Sgr

Current superoutbursts (since ...)
SDSS J141118.31+481257.6 :# (20180519, precursor to superoutburst?)
ER UMa (20180514)
ATLAS18olb (20180512)
OY Car (20180511; UGSU, eclipsing, Porb= 0.0631209247 d)
RZ LMi (20180505; ER UMa subtype)
MM Hya (20180504)
V362 Lib (20180504)
NY Her (20180503)

Z Cam-type dwarf novae at standstill
AT Cnc (20180202–20180508)
TZ Per (since 20171226)
HL CMa (20171221–20180426) 
IW And (since about 20171219)
NY Ser # (~20180120–20180317, ~56 days; UGSU)
Z Cam (20170405–20171207, 246 days)
IW And (20170812–20170831, 19 days)
OQ Car (20160415–20170826, 498 days)

# indicates a noteworthy or unusual outburst
:  indicates confirmation required
'Activity At A Glance' is gleaned from observations reported to AAVSO MyNewsFlash, BAAVSS-Alert, CVnet-Outburst, VSObs-share and VSNET-outburst. We sincerely thank all the observers who contribute timely observations and reports of activity to these email lists.


Updated May 21 2018

For new papers on CV's see astro-ph

M. J. Darnley, S. Starrfield

Mariko Kimura, Keisuke Isogai, Taichi Kato, Kenta Taguchi, Yasuyuki Wakamatsu, Franz-Josef Hambsch, Berto Monard, Gordon Myers, Shawn Dvorak, Peter Starr, Stephen M. Brincat, Enrique de Miguel, Joseph Ulowetz, Hiroshi Itoh, Geoff Stone, Daisaku Nogami

Joseph Patterson et al.

Paula Szkody, Mark E. Everett, Zhibin Dai, Donald Serna-Grey

John R. Thorstensen, Frederick A. Ringwald, Cynthia J. Taylor, Holly A. Sheets, Christopher S. Peters, Julie N. Skinner, Erek H. Alper, Kathryn E. Weil

Mariko Kato (Keio Univ.), Izumi Hachisu (Univ. of Tokyo), Hideyuki Saio (Tohoku Univ.)

E. Aydi, K. L. Page, N. P. M. Kuin, M. J. Darnley, F. M. Walter, P. Mróz, D. Buckley, S. Mohamed, P. Whitelock, P. Woudt, S. C. Williams, M. Orio, R. E. Williams, A. P. Beardmore, J. P. Osborne, A. Kniazev, V. A. R. M. Ribeiro, A. Udalski, J. Strader, L. Chomiuk

Michael M. Shara, Trisha F. Doyle, Ashley Pagnotta, James T. Garland, Tod R. Lauer, David Zurek, Edward A. Baltz, Ariel Goerl, Attay Kovetz, Tamara Machac, Juan Madrid, Joanna Mikolajewska, J. D. Neill, Dina Prialnik, Doug L. Welch, Ofer Yaron

J.M Hameury & J.P Lasota

V. V. Lukin, K. L. Malanchev, N. I. Shakura, K. A. Postnov, V. M. Chechetkin, V. P. Utrobin

Authors: A. F. Pala, B. T. Gänsicke, D. Townsley, D. Boyd, M. J. Cook, D. De Martino, P. Godon, J. B. Haislip, A. A. Henden, I. Hubeny, K. M. Ivarsen, S. Kafka, C. Knigge, A. P. LaCluyze, K. S. Long, T. R. Marsh, B. Monard, J. P. Moore, G. Myers, P. Nelson, D. Nogami, R. Pickard, G. Poyner, D. E. Reichart, D. Rodriguez Perez, M. R. Schreiber, J. Shears, E. M. Sion, R. Stubbings, P. Szkody, M. Zorotovic

Liam K Hardy, Martin J McAllister, Vik S Dhillon, Stuart P Littlefair, Madelon C P Bours, Elme Breedt, Tim Butterley, Anurak Chakpor, Puji Irawati, Paul Kerry, Tom R Marsh, Steven G Parsons, Chris D J Savoury, Richard W Wilson, Patrick A Woudt