Predicted properties of eclipsing binaries observable by Gaia
(2005) Symposium - The Three-Dimensional Universe with Gaia 576. p.569-572- 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 bse-code 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 bse-code 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 limb-darkening 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 HR-diagram, 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 Three-Dimensional Universe with Gaia
- conference location
- Paris, France
- conference dates
- 2004-10-04 - 2004-10-07
- external identifiers
-
- wos:000229610000108
- scopus:23744467498
- ISSN
- 0379-6566
- 1609-042X
- language
- English
- LU publication?
- yes
- id
- 63db4c80-d5c7-4bba-9683-70609536ed09 (old id 615719)
- alternative location
- http://adsabs.harvard.edu/abs/2005ESASP.576..569D
- date added to LUP
- 2016-04-01 12:35:08
- date last changed
- 2024-01-09 01:43:06
@inproceedings{63db4c80-d5c7-4bba-9683-70609536ed09,
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 bse-code 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 limb-darkening 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 HR-diagram, 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 = {{0379-6566}},
keywords = {{Population synthesis; Binaries; Eclipses; Gaia}},
language = {{eng}},
pages = {{569--572}},
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}},
}