The Henize sample of S stars

Eck, S. Van; Jorissen, A.

doi:10.1051/0004-6361:20021415

Cited by 38 publications

(55 citation statements)

References 15 publications

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“…The source V1261 Ori (HD 35155, HIP 25092) is an extrinsic S star that shows evidence of mass-transfer activity and is therefore also classified as a symbiotic star (Ake et al 1991;Van Eck & Jorissen 2002). As an extrinsic S star, it is the outcome of a previous mass transfer which polluted it in carbon and s-process elements.…”

Section: V1261 Orimentioning

confidence: 99%

Roche-lobe filling factor of mass-transferring red giants: the PIONIER view

Boffin

Hillen

Berger³

et al. 2014

A&A

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Using the PIONIER visitor instrument that combines the light of the four Auxiliary Telescopes of ESO's Very Large TelescopeInterferometer, we precisely measure the diameters of several symbiotic and related stars: HD 352, HD 190658, V1261 Ori, ER Del, FG Ser, and AG Peg. These diameters -in the range of 0.6−2.3 milli-arcsec -are used to assess the filling factor of the Roche lobe of the mass-losing giants and provide indications on the nature of the ongoing mass transfer. We also provide the first spectroscopic orbit of ER Del, based on CORAVEL and HERMES/Mercator observations. The system is found to have an eccentric orbit with a period of 5.7 years. In the case of the symbiotic star FG Ser, we find that the diameter changes by 13% over the course of 41 days, while the observations of HD 352 are indicative of an elongation. Both these stars are found to have a Roche filling factor close to 1, as is most likely the case for HD 190658 as well, while the three other stars have factors below 0.5-0.6. Our observations reveal the power of interferometry for the study of interacting binary stars; the main limitation in our conclusions is the poorly known distances of the objects.

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Section: V1261 Orimentioning

confidence: 99%

Roche-lobe filling factor of mass-transferring red giants: the PIONIER view

Boffin

Hillen

Berger³

et al. 2014

A&A

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“…This parameter is defined as Sb = (s 2 −s 0 2 ) 1/2 , where s is the standard deviation of a Gaussian fitted to the CORAVEL cross-correlation dip (see Baranne et al 1979) and s 0 the instrumental width (7 km s −1 for CORAVEL at the Haute-Provence Observatory; for details see Jorissen & Mayor 1988;Van Eck & Jorissen 2000, also Paper II). Indeed, Fig.…”

Section: Intrinsic Width Of Spectral Linesmentioning

confidence: 99%

Spectroscopic binaries among Hipparcos M giants

Famaey¹,

Pourbaix²,

Frankowski³

et al. 2009

A&A

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Context. This paper is a follow-up on the vast effort to collect radial velocity data for stars belonging to the Hipparcos survey. Aims. We aim at extending the orbital data available for binaries with M giant primaries. The data presented in this paper will be used in the companion papers of this series to (i) derive the binary frequency among M giants and compare it to that of K giants (Paper II); and (ii) analyse the eccentricity -period diagram and the mass-function distribution (Paper III). Methods. Keplerian solutions are fitted to radial-velocity data. However, for several stars, no satisfactory solution could be found, even though the radial-velocity standard deviation is greater than the instrumental error, because M giants suffer from intrinsic radialvelocity variations due to pulsations. We show that these intrinsic radial-velocity variations can be linked with both the average spectral-line width and the photometric variability. Results. We present an extensive collection of spectroscopic orbits for M giants with 12 new orbits, plus 17 from the literature. On top of these, 1 preliminary orbit yielded an approximate value for the eccentricity and the orbital period. Moreover, to illustrate how the large radial-velocity jitter present in Mira and semi-regular variables may easily be confused with orbital variations, we also present examples of pseudo-orbital variations (in S UMa, X Cnc, and possibly in HD 115 521, a former IAU radial-velocity standard). Because of this difficulty, M giants involving Mira variables were excluded from our monitored sample. We finally show that the majority of M giants detected as X-ray sources are actually binaries. Conclusions. The data presented in this paper considerably increase the orbital data set for M giants, and will allow us to conduct a detailed analysis of the eccentricity -period diagram in a companion paper (Paper III).

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“…The connection between the yellow symbiotic and barium stars has already been well established using the abundance patterns of post-iron-peak elements (Smith et al 1996(Smith et al , 1997Pereira, Smith, & Cunha 1998;Smith, Pereira, & Cunha 2001). Given the already established connection between the barium and yellow symbiotics, it is a '' real puzzle '' why hitherto just a few symbiotics of spectral type S have been recognized (Van Eck & Jorissen 2002;Jorissen 2003). The symbiotic characteristics displayed by HD 35155 make it worth investigating its pattern of postiron-peak abundances.…”

Section: Introductionmentioning

confidence: 99%

Abundances of Post–Iron‐Peak Elements in HD 35155: A Symbiotic Star of Spectral Type S

Vanture

Wallerstein

Gallino

et al. 2003

ApJ

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We present abundances of Ti, Fe, and Ni as well as 10 post-iron-peak elements in the extrinsic, Galactic S star HD 35155. This star is of interest because it shows many characteristics of symbiotic stars and displays the same pattern of abundance enhancements observed in yellow symbiotic stars. It is clear that HD 35155 is associated with the symbiotic stars and provides an important link between the symbiotic phenomena and chemically peculiar stars. In addition, the abundance ratio of heavy to light s-process elements correlates with the metallicity of HD 35155, as is expected if the 13 C neutron source drives the s-process. Our models predict that the abundance of lead should be enhanced by a factor of between 50 to 500 in HD 35155.

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The Henize sample of S stars

Cited by 38 publications

References 15 publications

Roche-lobe filling factor of mass-transferring red giants: the PIONIER view

Roche-lobe filling factor of mass-transferring red giants: the PIONIER view

Spectroscopic binaries among Hipparcos M giants

Abundances of Post–Iron‐Peak Elements in HD 35155: A Symbiotic Star of Spectral Type S

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