WD2256+249
Basic Info
2MASS 22584811+2515439, GD 245, EG232, KUV2256+249
RA/DE = 22:58:48.1 +25:15:44
V = 13.68, Bt=13.955, Vt=12.579, r'=13.861, J=11.675,
K=10.915
According to Schmidt et al (1995) this is a binary system, consisting
of a hot WD (spectral type A2, Teff = 22,170 K) and brown dwarf (spectral
type M3.5 MS, Teff = 3560 K). The LC variation is due to the WD heating
the co-rotating front side of the brown dwarf, which then radiates at hotter
temperature. The authors also write "The sinusoidal modulation is indicative
of reprocessing of white dwarf emission by the orbiting secondary." I'm
confused by whether they are invoking both effecst to account for the sinusoidal
modulation. They give the following ephemeris: HJDmax = 2449627.0524(8)
+ 0.173661(14) × E. The orbital period corresponds to 4.16786(34)
hours. The LC by Ayiomamitis has maximum brightness at HJD = 2455807.47604.
This means that E = 35589 ± 3. Since the SE on E >> 0.5, we
are unable to refine the period. To improve on the period accuracy by factor
10 would require two LCs like that of Ayoimamitis 100 days apart. Or, we
could match the Schmidt et al period accuracy every 10 days.
Observation Summary
This target was abandoned as soon as I realized that it is a well-studied WD/M4 binary. Here's an article about it: link
YYYYMMDD Length JD start - JD end Filter Observer RMS10 Sine Amplitude & Period
20110902 7.8 hrs 5806.662 - 5806.989 C Foote, Jerry 1.6 mmag, 50.6 ± 0.3 mmag, 4.20 hr
20110902 7.8 hrs 5806.664 - 5806.988 C Foote, Cindy 2.5 mmag, 51.7 ± 0.5 mmag, 4.18 hr
20110903 8.2 hrs 5807.663 - 5808.005 Rc Garlitz 3.7 mmag 81.8 ± 0.8 mmag, 4.18 hr
20110902 5.1 hrs 5807.226 - 5807.435 C Ogmen 2.0 mmag 60.5 ± 0.4 mmag, 4.44 hr
20110902 8.1 hrs 5807.268 - 5807.605 C Ayiomamitis 4.0 mmag 49.1 ± 0.8 mmag, 4.22 hr
Light Curves
raw spo
raw spo
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raw spo
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raw spo
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raw spo Maximum brightness is at UT = 23.290 ± 0.015, or HJD = 2455807.47604 ± 0.00063.
Finder Images
Aladin image.
WebMaster: B.
Gary. This site opened: 2011.09.01. Last Update: 2011.09.06