Predicted properties of eclipsing binaries observable by Gaia
(2005) Symposium  The ThreeDimensional Universe with Gaia 576. p.569572 Abstract
 Using a population synthesis model we estimate the fraction of stars of different types that are likely to show eclipses, as a function of the period. The population model is based on the bsecode from Hurley et al. (2002) which is a rapid binary evolution code that include all common effects in close binaries such as mass transfer, tidal locking, wind etc. We use this to evolve millions of systems from original distributions in separation, mass and eccentricity, with ages between zero and 12 Gyr, to get a population of systems representative of our Galaxy. The binary data from our model are then analysed in order to, statistically, see how many eclipsing systems we should have. This is done with a simple model where we neglect... (More)
 Using a population synthesis model we estimate the fraction of stars of different types that are likely to show eclipses, as a function of the period. The population model is based on the bsecode from Hurley et al. (2002) which is a rapid binary evolution code that include all common effects in close binaries such as mass transfer, tidal locking, wind etc. We use this to evolve millions of systems from original distributions in separation, mass and eccentricity, with ages between zero and 12 Gyr, to get a population of systems representative of our Galaxy. The binary data from our model are then analysed in order to, statistically, see how many eclipsing systems we should have. This is done with a simple model where we neglect limbdarkening and other complicating effects. Assuming a random distribution of the inclination angle the probability of an eclipse of a given depth, Am, can easily be calculated. Adding a reasonable fraction of true single stars, we can finally estimate the fraction of eclipsing binaries in limited areas of the HRdiagram, as a function of the period. A first comparison with observational data from the Hipparcos mission shows quite satisfying agreement, and extrapolation to Gaia should thus be a natural application. We find that Gaia will observe about 500 000 eclipsing binaries, this (surprisingly) small number arises from the fact that many eclipsing systems will not be detected by Gaia. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/615719
 author
 Dischler, Johann ^{LU} and Söderhjelm, Staffan ^{LU}
 organization
 publishing date
 2005
 type
 Chapter in Book/Report/Conference proceeding
 publication status
 published
 subject
 keywords
 Population synthesis, Binaries, Eclipses, Gaia
 host publication
 European Space Agency, (Special Publication) ESA SP
 volume
 576
 pages
 569  572
 publisher
 European Space Agency
 conference name
 Symposium  The ThreeDimensional Universe with Gaia
 conference location
 Paris, France
 conference dates
 20041004  20041007
 external identifiers

 wos:000229610000108
 scopus:23744467498
 ISSN
 1609042X
 03796566
 language
 English
 LU publication?
 yes
 id
 63db4c80d5c74bba968370609536ed09 (old id 615719)
 alternative location
 http://adsabs.harvard.edu/abs/2005ESASP.576..569D
 date added to LUP
 20160401 12:35:08
 date last changed
 20210217 03:16:37
@inproceedings{63db4c80d5c74bba968370609536ed09, abstract = {Using a population synthesis model we estimate the fraction of stars of different types that are likely to show eclipses, as a function of the period. The population model is based on the bsecode from Hurley et al. (2002) which is a rapid binary evolution code that include all common effects in close binaries such as mass transfer, tidal locking, wind etc. We use this to evolve millions of systems from original distributions in separation, mass and eccentricity, with ages between zero and 12 Gyr, to get a population of systems representative of our Galaxy. The binary data from our model are then analysed in order to, statistically, see how many eclipsing systems we should have. This is done with a simple model where we neglect limbdarkening and other complicating effects. Assuming a random distribution of the inclination angle the probability of an eclipse of a given depth, Am, can easily be calculated. Adding a reasonable fraction of true single stars, we can finally estimate the fraction of eclipsing binaries in limited areas of the HRdiagram, as a function of the period. A first comparison with observational data from the Hipparcos mission shows quite satisfying agreement, and extrapolation to Gaia should thus be a natural application. We find that Gaia will observe about 500 000 eclipsing binaries, this (surprisingly) small number arises from the fact that many eclipsing systems will not be detected by Gaia.}, author = {Dischler, Johann and Söderhjelm, Staffan}, booktitle = {European Space Agency, (Special Publication) ESA SP}, issn = {1609042X}, language = {eng}, pages = {569572}, publisher = {European Space Agency}, title = {Predicted properties of eclipsing binaries observable by Gaia}, url = {http://adsabs.harvard.edu/abs/2005ESASP.576..569D}, volume = {576}, year = {2005}, }