Presentation on theme: "Visual Observations of Delta Cephei: Time to Update the Finder Chart David Turner Saint Marys University."— Presentation transcript:
Visual Observations of Delta Cephei: Time to Update the Finder Chart David Turner Saint Marys University
Cephei has a long history as a variable star, its variability being discovered by John Goodricke in October His friend Edward Piggot had discovered the variability of the Cepheid Aquilae a month earlier in September 1784.
Polaris the brightest of 40 classical Cepheids visible without optical aids. Cephei Aquilae
The ready accessibility of δ Cephei for amateur or student observations has been pointed out in the literature from time to time, e.g. van de Kamp, Sky & Telescope, 12, 208, 1953.
Recent article on δ Cephei on the AAVSO website.
AAVSO finder chart with ζ Cep and ε Cep as reference stars.
A more detailed comparison chart for δ Cephei from the AAVSO. Problem: ζ is clearly brighter than ι to the eye, and closer to β in brightness.
Specifically: 10 years of regular observation by two AAVSO observers (AAP, SSW) relative to the photoelectric light curve. Visual observations do not match the amplitude or extrema of δ Cep.
Alternate method (Turner JRASC, 93, 228, 1999).
Alternate comparison chart for δ Cephei tied to photoelectric V-magnitudes from the Bright Star Catalogue. At faint limits the eye can distinguish differences of 0 m.1 or better (Turner 2000).
An accurate ephemeris for a Cepheid is essential for proper phasing of the observations. For δ Cephei: HJD max = d E
First observations of δ Cephei tied to the alternate comparison chart.
Phased photoelectric observations of δ Cephei from the literature.
A comparison of eye V magnitudes with the photoelectric V light curve. Note the 0 m.15 offset.
A similar comparison with eye estimates by the author for η Aquilae. There is no offset here.
Ditto for ζ Geminorum.
A combination of observations from with every five data points averaged in phase. The results are comparable to photoelectric data.
Additional observations of δ Cephei from 2009.
... and from 2010.
A study of the evolutionary period decrease in δ Cephei from 230 years of observation. John Goodricke David Turner
The problem lies in the adopted reference magnitudes for the two main comparison stars: ζ Cep and ε Cep. van de Kamp (1953) lists values of 3.60 and 4.36 for the stars from Potsdam Durchmusterung photovisual pv magnitudes. Their photoelectric V magnitudes are 3.35 and 4.19, respectively, while AAVSO chart values are 3.6 and 4.2. Since all good eye estimates of δ Cephei are made under normal light conditions, the use of AAVSO charts artificially depresses the observed light amplitude and skews light maximum from its true brightness.
StarVB VSpTV trans V chart ζ Cep K1.5 Ib ε Cep F0 IV ι Cep K0 III α Cep A7 V υ Cep A2 Ia α Lac A1 V
The study by Richard Stanton (JAAVSO, 10, 1, 1981) relating pe V magnitudes to visual magnitudes on AAVSO charts. He derived the relationship: m vis = V (B V) 0.15
Ron Zissels (1998) study of the visual magnitude system adopted the same formula… for observations with the dark-adapted eye.
The wavelength dependence of the photoelectric V filter relative to that for the dark-adapted eye.
But the eyes spectral response for normal lighting conditions is much closer to the wavelength sensitivity of the Johnson V filter.
Since most observations of Cephei are done in normal lighting conditions, use of a comparison chart with star magnitudes adjusted for dark adaption is inappropriate. Observations near the visual limit are also more accurate than those made of bright stars using telescopes, so the ideal observations of δ Cephei are made by eye or binoculars before the eye becomes dark adapted.