By folding light curve data, phase plots provide a way to construct and analyze a variable star's light curve using multiple measurements.
Light Curve Analysis Aov ANOVA
ANOVA/Aov (Analysis Of Variance) is a simple yet powerful statistical model used to find a repeatable period in a variety of scattered light curve data points.
Why Study Variable Stars
From measuring the distances to galaxies to discovering new planets, studying variable stars allows us to refine our current understanding of astrophysics and get to the heart of how our universe works.
Catalog of Rectilinear Elements
The Catalog of Rectilinear Elements provides linear fits for those systems whose motion does not appear to be Keplerian
SIMBAD can be accessed via CDS and Stelle Doppie. Using SIMBAD, stellar data and summaries and publication information can be accessed.
Online Catalogs Overview
This video goes over the online catalogs CDS Strausbourg, Stelle Doppie, SiMBAD, and VizieR
Differential Photometry is comparing the difference between a target star and a comparison star, and eliminates all other observational variables.
The Landolt catalog has become the de facto standard for transforming to the UBVR CIC system, and place photometric observations on a common platform.
Standard Photometric Stars
Photometric-standard stars are stars that have had their light output in various passbands of photometric system measured very carefully. They provide a means to not only calibrate your photometric system, but give a common “yardstick” from which all measurements can be compared.
Extinction is the removal of light through dust, gas, or atmosphere, or the overall dimming of starlight by interstellar matter. Extinction comes in two types: Interstellar and Atmospheric.
Counts focuses on all measured values within an aperture as opposed to focusing on data contained within a single pixel.
Some photometry projects are variable stars, supernova study, asteroids and comets, UBVRI, and exoplanets.
Comparison stars provide a baseline from which to compare with, and it is important that comp stars are stable and un-variable. Software such as AstroImageJ can help locate comparison stars.
Variable Stars and their Relation to Stellar Evolution
This video covers a high level view of the stellar life cycle as relating to variable stars, discussing pre-main sequence, the main sequence, after the main sequence, and after the AGB
Variable Star Overview
Variable stars have a varying light output as seen from our vantage point; their light output can be affected by extrinsic and intrinsic variables.
Difference Between Nova and Supernova
Stars can go nova multiple times, and is an accretion-explosion cycle; while supernovas only occur once in a star's lifetime and are caused by a high mass star core collapse, releasing great amounts of energy
WCS Coordinates Using MaximDL
This tutorial will show you how to access your star images on BARC, opening them in MaximDL, applying WCS coordinates, and saving the files.
The World Coordinate System (WCS) is the RA and Dec embedded in a FITS image. Multiple tools, such as astrometry.net and MaximDL can insert WCS coordinates into the image
UBVRI & JC filters
The UBVRI system covers all of the visual spectrum and some on the shorter and longer sides, and is the most commonly used system with a large network of standard stars.
Binning is a method of combining pixels on a CCD chip into one “super” pixel. This provides some advantages and disadvantages.