2003
DOI: 10.1051/0004-6361:20030284
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A study of λ Bootis type stars in the wavelength region beyond 7000 Å

Abstract: Abstract. The group of λ Bootis type stars comprises late B-to early F-type, Population I objects which are basically metal weak, in particular the Fe group elements, but with the clear exception of C, N, O and S. One of the theories to explain the abundance pattern of these stars involves circumstellar or interstellar matter around the objects. Hence, we have compiled all available data from the literature of well established members of the λ Bootis group redward of 7000 Å in order to find evidence for matter… Show more

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Cited by 19 publications
(24 citation statements)
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References 55 publications
(96 reference statements)
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“…The peak of the planet occurrence rate distribution, as a function of host-star mass, has a sharp cut-off at the high mass end: 1.9 +0.1 −0.5 M (Reffert et al 2015). Only around 23% of λ Boo stars have an infrared excess (Paunzen et al 2003), so a further strength of this mechanism is that it does not demand one.…”
Section: Influence On Pulsationmentioning
confidence: 99%
“…The peak of the planet occurrence rate distribution, as a function of host-star mass, has a sharp cut-off at the high mass end: 1.9 +0.1 −0.5 M (Reffert et al 2015). Only around 23% of λ Boo stars have an infrared excess (Paunzen et al 2003), so a further strength of this mechanism is that it does not demand one.…”
Section: Influence On Pulsationmentioning
confidence: 99%
“…However, the λ Bootis stars are a small group (only 2 per cent) of late-B to early-F stars that show moderate to extreme (surface) underabundances (up to a factor 100) of most Fe-peak elements, but solar abundances of lighter elements (C, N, O and S). Several members of the group exhibit a strong infrared excess and a disc (Paunzen et al 2003;Booth et al 2013).…”
Section: Introductionmentioning
confidence: 99%
“…From these references it was already clear that 1) only very few λ Bootis members were detected in the IR and 2) even fewer objects show infrared excesses. Paunzen et al (2003) presented all available data for members of the λ Bootis group in the wavelength region beyond 7000Å. The data include spectrophotometry, Johnson RIJHKLM and 13-color photometry as well as IRAS and ISO measurements.…”
Section: The Characteristics Of λ Bootis Stars In the Uv Regionmentioning
confidence: 99%