When eclipsing binaries
orbit each other closely, within about 10 days or less, Fleming and co-authors wondered, do tides -- the gravitational forces each exerts on the other -- have "dynamical consequences" to the star system?
We followed with interest the presentations on eclipsing binaries
where it was recommended that particular stars be studied including AO Cas, CQ Cep and RT Lac.
Consider long-period eclipsing binaries
. Astronomers know of several dozen such systems, in which two stars periodically eclipse each other, but only a few have been fairly well studied.
All observation and analysis files for this campaign, including working spreadsheets, PERANSO and BinaryMaker files, can be downloaded from www.variablestarssouth.org > Research Projects > Equatorial Eclipsing Binaries
> CU Hydrae > Results.
We aim to analyse one hundred eclipsing binaries
from the All Sky Automated Survey (ASAS) catalogue for variations in the times of their eclipses, which can possibly be due to the LTE.
have orbital planes close to the observer's line of sight so that components eclipse each other with a consequent periodic change in the brightness of the system.
Or, have you observed eclipsing binaries
and wondered if there was more you could do with the data?
Middleton continued his collaboration with Smits by doing further observations of W UMa-type eclipsing binaries
from Kyalami in Johannesburg.
The Handbook has revised the Section's EB Observing Programme and lists 'Beginner's Eclipsing Binaries
' and 'Priority Eclipsing Binaries
With most eclipsing binaries
, it's easy to calculate when one star begins to eclipse the other, or when the eclipse ends.
Middleton continued his collaboration with Smits by doing observations of W UMa type eclipsing binaries
. Using observations from Kyalami in Johannesburg and the 0.75m telescope of the SAAO in Sutherland, timing measurements for several systems have been obtained.
Many of them are also eclipsing binaries
. Early in 2007, Dr Boris Gaensicke at Warwick University suggested to me that it would be interesting to measure the times of eclipses of some of these SW Sex stars to check for evidence of changes in their orbital periods.
They include flare stars, Cepheid variables, eclipsing binaries
, extrasolar planetary transits, and even stars with spots.
We hope that the EB Handbook will encourage many more people to become observers of eclipsing binaries
In today's universe, the two heftiest stars with masses that have been measured directly (by the strength of their gravity in spectroscopic eclipsing binaries
) may be HD 15558 in Cassiopeia, with 152 [+ or -] 51 solar masses, and R145 in the Large Magellanic Cloud,