Eclipsing Binaries (EBs)

A colleague and I are compiling a series of times of minima (ToM) for a number of eclipsing binaries we observed. For poorly observed systems we are compiling additional TOMs using SuperWasp data. Obviously, some of the SuperWasp data are better than others. Just because Peranso can compute a ToM does not necessarily indicate that the ToM is accurate enough to be useful. So, I am wondering about just how accurate a ToM should be relative to O-C to be valuable enough to publish.

Hi,

recently after observing W Umi, I found per Muniwin datamining that i also have a minimum of CzeV 257 UMi or GSC 4638-934, cze: (The Czech variable star cataloge).

Yesterday i got a VSP finderchart, today not?

https://www.aavso.org/apps/vsp/chart/X25579ABZ.png

Also VSX + VSP seems to have missing properties? Max, Min, Period, Epoch.

Hi there

First, thanks to all the organisers and presenters of the EB webinar - I learned a lot!

As I was listening, I wondered if it is possible to detect changes in the spectrum of an EB if it is comprised of two widely different spectral types? If so, and you track it over a minimum, there should be some interesting dynamics to observe. I do  spectroscopy and have just started to do do the simulatneous photometry so it might be  a nice project...

Thanks

Kevin

I observed KID 03644542 about 12 hours ago and it was noticably dimmer than the comparison star 84 https://www.aavso.org/apps/vsp/chart/?fov=60.0&scale=D&star=KID+03644542&orientation=reversed&maglimit=10.5&resolution=150&other=gcvs&north=down&east=right&type=chart

This could go on the new equipment and instrumentation page, but this is very EB-centric.

I will buy a computer (refurbished) in order to transition to Linux. Part of the motivation is to learn Phoebe 2.2 (Linux only, command line does not put me off.). Given the likely amount of data crunching, I seek advice.

As a bright star monitor participant, I have been observing an EA that is listed as an A0 type in VSX.  Over the course of the past 12 months+, I have noted that the star is consistenly much brighter in the Johnson V, Counsins R, and Cousins I bands than Johnson B.  My limited understanding of the typical A0 spectrum would suggest that B should be the brightest band of the four.  Could there be something about this EA geometry that would have the other three bands brighter than B in this case?

This is probably the most interesting and weird eclipsing variable I have been able to solve since I started analyzing light curves.

In the framework of a project to update VSX with the latest information from the GCVS and adding information that was missing in thousands of records, I am giving special attention to eclipsing binaries (as announced in the EB webinar last month).
The goal is to add elements to the largest possible number of eclipsing binaries to leave a clean sample of objects that really need observations to find their periods.

When is the next Thuban & companion Eclipse: Date and Time??

You are all invited to join a live “EB discussion” webinar on this Wednesday, April 15, at 12 noon PDT = 3PM EDT = 1900 UT.

This was prompted by the question "How do you plan eclipse observations, especially for systems with long periods (> few days) and possibly-uncertain ephemerides?"

The tentative agenda is:

• Gary Billings enjoys stars with little observational history, so the ephemerides can be so far off that an all-night run on the appointed night sometimes detects no fade at all.  He’ll describe his approach and some examples.