2010
DOI: 10.1051/0004-6361/201015529
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A Renaissance study of Am stars

Abstract: Aims. Triggered by the study of Carquillat & Prieur (2007, MNRAS, 380, 1064 of Am binaries, I reanalyse their sample of 60 orbits to derive the mass ratio distribution (MRD), assuming as they did a priori functional forms, i.e. a power law or a Gaussian. The sample is then extended using orbits published by several groups and a full analysis of the MRD is made, without any assumption on the functional form. Methods. I derive the MRD using a Richardson-Lucy inversion method, assuming a fixed mass of the Am prim… Show more

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Cited by 17 publications
(32 citation statements)
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“…Furthermore, the photometric data along with the deduced gravity (log g = 4.25- Wonnacott et al 1994) for IK Peg A is consistent with it being a relatively young star that has not significantly evolved away from the zero-age main sequence. The mass estimate for IK Peg A places it at the low end of the range applicable to Am stars, which varies from 1.6 to about 2.2 M (Boffin 2010), and this is consistent with its marginal Am spectroscopic status.…”
Section: Ik Pegasi: Past Present and Futuresupporting
confidence: 70%
See 1 more Smart Citation
“…Furthermore, the photometric data along with the deduced gravity (log g = 4.25- Wonnacott et al 1994) for IK Peg A is consistent with it being a relatively young star that has not significantly evolved away from the zero-age main sequence. The mass estimate for IK Peg A places it at the low end of the range applicable to Am stars, which varies from 1.6 to about 2.2 M (Boffin 2010), and this is consistent with its marginal Am spectroscopic status.…”
Section: Ik Pegasi: Past Present and Futuresupporting
confidence: 70%
“…The small excesses in barium and strontium, Smalley et al (1996), suggest might be the result of either radiative levitation or a consequence of mass transfer during the systems common envelope stage of evolution (to be discussed shortly). The latter scenario is possibly favored since IK Peg A is also a known low-amplitude δ Scuti variable (Kurtz 1978;Wonnacott et al 1994), and such pulsational activity, in the absence of any strong magnetic fields, is likely to disrupt the diffusion process thought otherwise to be responsible for the Am phenomenon in general (Gonzalez et al 1980;Boffin 2010). In summary, the available observational data indicates that IK Peg A has a near solar abundance, exhibiting only small under/over abundances making it a marginal Am star.…”
Section: Ik Pegasi: Past Present and Futurementioning
confidence: 92%
“…One way to accomplish this is to look at the distribution of log Y (and not of Y; see Boffin 2010) and compare this with some given a priori distributions. Another way is to use a method to numerically invert the equation that links the observed distribution of Y with that of q.…”
Section: Methodsmentioning
confidence: 99%
“…Assuming that the binary mass ratio distribution is flat (Boffin 2010) and that the initial binary frequency was 20%, about 1.7% of 4-7M ☉ stars would have had companions of 0.8M ☉ . In a Kroupa (2001) initial mass function, 1.3% of 0.08-100M ☉ stars lie in the mass range 4-7M ☉ .…”
Section: Binary Mass Transfermentioning
confidence: 99%