Download A Practical Guide to Lightcurve Photometry and Analysis by Brian D. Warner PDF

By Brian D. Warner

A sensible consultant to Lightcurve Photometry and research offers, for
those with entry to even a modest telescope and CCD digital camera, all the
information had to participate in the clinical learn of asteroids and
variable stars.

Using commercially to be had gear, beginner astronomers can
determine the rotation price, dimension, and form of asteroids. equally, it
is attainable to find the scale, temperature, and orbits of stars in
binary structures through the use of this robust technique.

A useful consultant to Lightcurve Photometry and research comprises all the
material wanted for readers to appreciate the speculation, and stay away from the
practical pitfalls of lightcurve photometry. precise examples are
given for acquiring info, and naturally for the fascinating and rewarding
task of studying the knowledge to figure out the actual homes of the
object.

Any collage pupil or beginner astronomer who desires to transcend mere
imaging with a CCD digital camera and input the difficult international of "real
science" through the lightcurves of asteroids and binary stars will find
everything useful during this book.

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Extra resources for A Practical Guide to Lightcurve Photometry and Analysis

Sample text

Over time, just as with film, PMTs have been tailored to favor certain spectral regions and, also as with film, the use of PMTs required that a color system be devised so that measurements among observers could be accurately compared. L. W. Morgan devised what would become the most commonly used photometric standard to date. Using the 1P21 PMT and a carefully constructed set of filters, they created the UBV system. This system defines three broad pass bands. The U band favors the UV region with a peak of about 3500 Å.

5 magnitudes or less. The group, generally known as SR, is usually broken into several groups, SRA through SRD, and probably more, depending on who’s doing the classification. The SRA stars have periods longer than 35 days, while the SRBs have less well-defined periods starting at 20 days. Again, the term period is used loosely since these red giant and supergiant stars do not show the higher degree of regularly of even the not-so-regular long-period variables. 1 Extra-Solar Planets As of mid-2005, more than 150 planets circling a star other than ours were known and the number is constantly growing.

In this case, you are not getting a good statistical profile of the star and so the accuracy of your photometry suffers. , have 2–3 pixels per FWHM. If your site has regular periods of better than average seeing, use the best seeing your site provides to determine the best pixel size. When the seeing deteriorates, you can go to 2x2 or even 3x3 binning to get a better pixel match. This allows you “the best of all worlds” and doesn’t keep you from taking advantage of those better nights. If those nights of exceptional seeing are not very common, then you’re probably better off working with the lower side of average when making your decision.

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