"The best observing practice is to adopt a star and stick to it - *density of observation* is very critical.  Until you don't like it any more - then adopt a different star!" --Joe Patterson (Columbia University, CBA boss)

Our first observing priority are accreting white dwarfs which have been observed to host classical nova explosions. As Joe Patterson said on 2016 Apr 25, A word about this project - the long-term "old nova project". We'd like to track the evolution of nova orbital light curves, over the first few decades after outburst. The most interesting interval is the first few years, so even very recent novae (say 1-3 years) are eligible. Most novae flash orbital light curves, and most show a very characteristic light curve, suggesting heating of the secondary - a double-sinusoid with an apparent eclipse. In theory, the evolution of the "eclipse" and the double wave allows deduction of the changing pattern of heating in the binary... and that might even allow us to track the cooling of the white dwarf, decades after eruption.

Last updated by Laura Chomiuk on 2017 July 12.

Novae Edit

Nova ASASSN-17hx: RA=18:31:45.918, Dec= -14:18:55.57 Edit

  • Finder chart
  • Please get nice B, V, R, I exposures (say, just three exposures in each filter) every night you observe. You don't need to sit on this one for monitoring sequences.
  • Comparison Star: 127
  • Check Star 1: 134
  • Check Star 2: 120
  • Don't need to submit to CBA; these are for Laura! Send to instead

Nova V339 Del: RA= 20 23 30.73  Dec= +20 46 04.1 Edit

  • This is a nova that went off in 2013 that is still optically bright, at V ~ 14.5 mag. We want to monitor it to see if we can find the binary period.
  • Observe this one in V band for long time series. Don't need to submit to CBA; these are for Laura! Send to instead
  • Finder chart

Mystery Stars Edit

FY Per: RA= 04 41 56.60, Dec= +50 42 36.0 Edit

FY Per is a total mystery star.  A well-determined spectroscopic period 
of 0.2585 d, but every so often, a 90-minute photometric period pops up 
-just a few hundredths of a magnitude, but not particularly difficult to 
study since the star is 12th mag.  One of these years, we should figure 
it out!
  • Finder chart
  • Nice long sequences on this guy, preferably in V filter.

Retired (at least presently): Edit

FS Aur: 05:47:48.36, +28:35:11.2

Paloma=RX J0524+4244: 05:24:30.44, +42:44:50.8

DW Cnc: 07:58:53.07, +16:16:45.4

  • Finder chart
  • More info on Koji's intermediate polar (IP) page
  • 1.4 hour orbital period; 39 minute white dwarf spin period.
  • "DQ Her"-like, or an intermediate polar. So the white dwarf has a pretty strong magnetic field.
  • Should be in the range 15--17.5 mag. So either V band or clear monitoring may work; if you have opinions on which is better, report back!

YZ CNC: 08:10:56.65, +28:08:33.2

  • Finder chart
  • Variable Type: SU UMa type dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: V
  • Exposure Length: not specified
  • Orbital Period: 2.08 hours
  • Outburst Period: 7-10 days
  • Superoutburst Period: 100-110 days
  • Quiescence Magnitude: 14.8
  • Outburst Max Magnitude: 12.0
  • Superoutburst Max Magnitude: 11.0

AM CVn: 12:34:54.62, +37:37:44.1 --- retired as of Summer 2017

CR Boo: 13:48:55.22, +07:57:35.8

  • Variable Type: AM CVn type dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: Clear
  • Exposure Length: not specified
  • Quiescence Magnitude: ~15.0

OV Boo: 15:07:22.35, +52:30:39.8

ES Dra: 15:25:31.81, +62:01:00.0

  • Variable Type: Z Cam dwarf nova
  • Campaign Timeframe: ongoing
  • Filter to use: V (Clear if too dim)
  • Exposure Length: not specified
  • Period: 4.2 hours
  • Quiescence Magnitude: 15.4
  • Negative Superhump Magnitude: 17.0
  • Finder chart

IGR J19552+0044: 19 55 12.47 +00 45 36.6

  • Finder chart
  • Short exposures (as short as possible!)
  • Comparison Stars: 148, 145, 158

V2306 Cyg: 19 58 14.46 +32 32 42.4

V1974 Cyg: 20:30:31.61, +52:37:51.3

  • Finder chart
  • Use comparison stars 139, 142, 146
  • Filter to use: Clear

V2069 Cyg: 21 23 44.83 +42 18 01.6

V598 Peg = RX233325.92+152222: 23:33:25.99, +15:22:22.2

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