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The Galactic formation rate of eccentric neutron star-white dwarf binaries

Kalogera, V.; Kim, Chunglee LU ; Lorimer, D.R.; Ihm, M. and Belczynski, K. (2005) Binary Radio Pulsars, 2005 In Astronomical Society of the Pacific Conference Series 328. p.261-267
Abstract (Swedish)
Abstract in Undetermined

n this paper we consider the population of eccentric binaries with a neutron star and a white dwarf that has been revealed in our galaxy in recent years through binary pulsar observations. We apply our statistical analysis method (Kim, Kalogera, & Lorimer 2003)and calculate the Galactic formation rate of these binaries empirically. We then compare our results with rate predictions based on binary population synthesis from various research groups and for various ranges of model input parameters. For our reference moel, we find the Galactic formation rate of these eccentric systems to be ~7 per Myr, about an order of magnitude smaller than results from binary evolution estimations. However, the... (More)
Abstract in Undetermined

n this paper we consider the population of eccentric binaries with a neutron star and a white dwarf that has been revealed in our galaxy in recent years through binary pulsar observations. We apply our statistical analysis method (Kim, Kalogera, & Lorimer 2003)and calculate the Galactic formation rate of these binaries empirically. We then compare our results with rate predictions based on binary population synthesis from various research groups and for various ranges of model input parameters. For our reference moel, we find the Galactic formation rate of these eccentric systems to be ~7 per Myr, about an order of magnitude smaller than results from binary evolution estimations. However, the empirical estimates are calculated with no correction for pulsar beaming, and therefore they should be taken as lower limits. Despite uncertainties that exceed an order of magnitude, there is significant overlap of the various rate calculations. This consistency lends confidence that our current understanding of the formation of these eccentric NS-WD binaries is reasonable. (Less)
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author
organization
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type
Chapter in Book/Report/Conference proceeding
publication status
published
subject
in
Astronomical Society of the Pacific Conference Series
volume
328
pages
261 - 267
conference name
Binary Radio Pulsars, 2005
language
English
LU publication?
yes
id
a289dd9b-8ce9-4c76-a2d2-a8fe5e98f197 (old id 1457709)
alternative location
http://arxiv.org/abs/astro-ph/0408247v1
date added to LUP
2009-08-10 15:23:53
date last changed
2016-04-16 12:10:01
@misc{a289dd9b-8ce9-4c76-a2d2-a8fe5e98f197,
  abstract     = {<b>Abstract in Undetermined</b><br/><br>
n this paper we consider the population of eccentric binaries with a neutron star and a white dwarf that has been revealed in our galaxy in recent years through binary pulsar observations. We apply our statistical analysis method (Kim, Kalogera, &amp; Lorimer 2003)and calculate the Galactic formation rate of these binaries empirically. We then compare our results with rate predictions based on binary population synthesis from various research groups and for various ranges of model input parameters. For our reference moel, we find the Galactic formation rate of these eccentric systems to be ~7 per Myr, about an order of magnitude smaller than results from binary evolution estimations. However, the empirical estimates are calculated with no correction for pulsar beaming, and therefore they should be taken as lower limits. Despite uncertainties that exceed an order of magnitude, there is significant overlap of the various rate calculations. This consistency lends confidence that our current understanding of the formation of these eccentric NS-WD binaries is reasonable.},
  author       = {Kalogera, V. and Kim, Chunglee and Lorimer, D.R. and Ihm, M. and Belczynski, K.},
  language     = {eng},
  pages        = {261--267},
  series       = {Astronomical Society of the Pacific Conference Series},
  title        = {The Galactic formation rate of eccentric neutron star-white dwarf binaries},
  volume       = {328},
  year         = {2005},
}