Using the naked eye, binoculars or telescopes, the variable star and nearby non-variable stars of known brightness are observed, and the brightness of the variable star, at a particular time, is estimated by comparing it with the appearance of these adjacent comparison stars.
The AAVSO, mentioned in the introductory paragraph above, has an online facility called the Variable Star Plotter which displays and prints charts that show one or more variable stars and the adjacent comparison stars.
The example shown is for the variable star BH Cru, which is shown in the centre of the chart as an open circle, surrounded by four straight lines. On examination of this star through powerful binoculars or a small telescope, it may be considered that it is brighter than the comparison star labelled 82 and fainter than the comparison star labelled 70. Thus, the magnitude (a measure of brightness) would be between 7.0 and 8.2 (the decimal places are omitted from the chart so that they would not be confused with faint stars).
To narrow down the magnitude estimation, it may be considered that the variable is brighter than 78 but fainter than 74, in which case you would estimate the magnitude of BH Cru to be 7.6, mid way between the magnitudes of the two comparison stars. If, on the other hand, BH Cru appeared to be identical in brightness to one of the comparison stars, say 74, then you would note that your estimate of the magnitude would be 7.4.
After you have made and documented your observations, you may submit them online to the AAVSO International Database. Having done that, you can plot a light curve on the AAVSO web site, and select the option to highlight your own observations. With practice, and using techniques described by the AAVSO, you can become proficient. Your observations then may be no more than 0.2 magnitude units away from the actual magnitude of the variable star. An error of 0.2 magnitude sounds large.
However, the long period Mira type variables, which are popular targets for visual variable star observers, with periods of many months, have quite large amplitudes (often several magnitudes). In this case, an error of about 0.2 magnitude will not be important, since averaging the results will minimize the random errors.
The visual observation of variable stars is described in detail on the AAVSO web site. On the Home Page, click the links to: Observing>Observing Manuals>Visual Observing Manuals.
About the author
- Roy Axelsen is Section Director of the Variable Stars Section of the AAQ and won the Page Medal in 2016.
- Variable Stars2019.06.25Photometry of Variable Stars
- Variable Stars2019.06.25The visual observation of variable stars
- Variable Stars2017.03.22Digital single lens photometry in white light: a new concept tested on data from the high amplitude δ Scuti star V703 Scorpii
- Variable Stars2016.10.14The high amplitude δ Scuti star AD Canis Minoris