Eclipsing binary statistics  Theory and observation
(2005) In Astronomy & Astrophysics 442(3). p.10031013 Abstract
 The expected distributions of eclipsedepth versus period for eclipsing binaries of different luminosities are derived from largescale population synthesis experiments. Using the rapid Hurley et al. BSE binary evolution code, we have evolved several hundred million binaries, starting from various simple input distributions of masses and orbitsizes. Eclipse probabilities and predicted distributions over period and eclipsedepth (P/Delta m) are given in a number of mainsequence intervals, from Ostars to brown dwarfs. The comparison between theory and Hipparcos observations shows that a standard (Duquennoy & Mayor) input distribution of orbitsizes ( a) gives reasonable numbers and P/Delta mdistributions, as long as the massratio... (More)
 The expected distributions of eclipsedepth versus period for eclipsing binaries of different luminosities are derived from largescale population synthesis experiments. Using the rapid Hurley et al. BSE binary evolution code, we have evolved several hundred million binaries, starting from various simple input distributions of masses and orbitsizes. Eclipse probabilities and predicted distributions over period and eclipsedepth (P/Delta m) are given in a number of mainsequence intervals, from Ostars to brown dwarfs. The comparison between theory and Hipparcos observations shows that a standard (Duquennoy & Mayor) input distribution of orbitsizes ( a) gives reasonable numbers and P/Delta mdistributions, as long as the massratio distribution is also close to the observed flat ones. A random pairing model, where the primary and secondary are drawn independently from the same IMF, gives more than an order of magnitude too few eclipsing binaries on the upper main sequence. For a set of eclipsing OBsystems in the LMC, the observed perioddistribution is different from the theoretical one, and the input orbit distributions and/or the evolutionary environment in LMC has to be different compared with the Galaxy. A natural application of these methods are estimates of the numbers and properties of eclipsing binaries observed by largescale surveys like Gaia. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/218913
 author
 Söderhjelm, Staffan ^{LU} and Dischler, Johann ^{LU}
 organization
 publishing date
 2005
 type
 Contribution to journal
 publication status
 published
 subject
 keywords
 stars : evolution, stars : formation, binaries : eclipsing, methods : miscellaneous, binaries : general, stars : statistics
 in
 Astronomy & Astrophysics
 volume
 442
 issue
 3
 pages
 1003  1013
 publisher
 EDP Sciences
 external identifiers

 wos:000232562700027
 scopus:27344446181
 ISSN
 00046361
 DOI
 10.1051/00046361:20042541
 language
 English
 LU publication?
 yes
 id
 3ebdfbbd4a13446fbbc5137b07b1ee42 (old id 218913)
 date added to LUP
 20160401 17:15:21
 date last changed
 20210217 03:51:58
@article{3ebdfbbd4a13446fbbc5137b07b1ee42, abstract = {The expected distributions of eclipsedepth versus period for eclipsing binaries of different luminosities are derived from largescale population synthesis experiments. Using the rapid Hurley et al. BSE binary evolution code, we have evolved several hundred million binaries, starting from various simple input distributions of masses and orbitsizes. Eclipse probabilities and predicted distributions over period and eclipsedepth (P/Delta m) are given in a number of mainsequence intervals, from Ostars to brown dwarfs. The comparison between theory and Hipparcos observations shows that a standard (Duquennoy & Mayor) input distribution of orbitsizes ( a) gives reasonable numbers and P/Delta mdistributions, as long as the massratio distribution is also close to the observed flat ones. A random pairing model, where the primary and secondary are drawn independently from the same IMF, gives more than an order of magnitude too few eclipsing binaries on the upper main sequence. For a set of eclipsing OBsystems in the LMC, the observed perioddistribution is different from the theoretical one, and the input orbit distributions and/or the evolutionary environment in LMC has to be different compared with the Galaxy. A natural application of these methods are estimates of the numbers and properties of eclipsing binaries observed by largescale surveys like Gaia.}, author = {Söderhjelm, Staffan and Dischler, Johann}, issn = {00046361}, language = {eng}, number = {3}, pages = {10031013}, publisher = {EDP Sciences}, series = {Astronomy & Astrophysics}, title = {Eclipsing binary statistics  Theory and observation}, url = {http://dx.doi.org/10.1051/00046361:20042541}, doi = {10.1051/00046361:20042541}, volume = {442}, year = {2005}, }