• All stars in one file (TXT)
• allstars.cat (ASCII)
• SIMBAD
• GCVS
• Old ephemerides

Eccentric orbit stars | Other stars

The database is described in the paper: "Up-to-date Linear Elements of Close Binaries", J.M. Kreiner, 2004, Acta Astronomica, vol. 54, pp 207-210. Please include a citation when using the database for your research. This project was partly supported by KBN grant No 2 P03D 006 22.

Current orbital phase is calculated based on YOUR COMPUTER TIME !!!!

The successive columns of tables contain:

• The name of a star in constellation order and link to times of minima calculator
• Information about minima considered in the calculation of the linear elements:
                 all - primary and secondary minima were used,
                 pri - only primary minima were used,
                 sec - only secondary minima were used.
• The time of the "artificial" minimum Mo (this is not an observational time of minimum!) used for the best fitting of straight line to the O-C diagram. The value of Mo was arbitrarily set close to JD 2,452,500.
• Mean errors of Mo (shown in round brackets).
• The current period P of the star obtained during the fitting the straight line to the O-C diagram.
• Mean errors of P (presented in round brackets). If the number of minima used to determine the elements was smaller than 8, mean errors were not calculated and an asterisk (*) appears inside the brackets.
• The number of minima used in the computation:               
  all - the number of all minima,               
  pri - the number of primary minima,               
  sec the number of secondary minima.               
         
  The number of minima according to the method of observations:               
  e photoelectric minima               
  ccd ccd minima               
  v visual minima               
  pg minima obtained from a series of photographic observations               
  p the time of mid-exposure of a photographic plate, taken when the star was near minimum. Timing isn't usually very accurate with this method.
• Years of the first and the last minimum used in the computation. (Many of the stars have a large gap with no minima observed between the first and last year of observations).
• Date when the computation was finished.