Binaries in the Praesepe and Coma Star Clusters and Their Implications for Binary Evolution

Abt, Helmut A.; Willmarth, Daryl W.

doi:10.1086/307569

Cited by 46 publications

(84 citation statements)

References 39 publications

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“…For the mass-ratio we obtained M 1 /M 2 = 1.82 ± 0.01 which agrees with Shorlin et al (2002). For the γ-velocity we found γ = −0.4 km s −1 , a value very close to that of Abt & Willmarth (1999) who were able to measure only the radial velocity of the primary.…”

Section: Hd 434supporting

confidence: 84%

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A search for SB2 systems among selected Am binaries

et al. 2004

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Abstract. We report on the detection of secondary spectra in five spectroscopic binary systems: HD 434, HD 861, HD 108642, HD 178449, and HD 216608. High signal-to-noise high resolution spectroscopic observations were carried out at the Bulgarian NAO Rozhen as part of an extended project concerned mainly with Am stars in binary systems. Our knowledge about early type binaries has serious gaps. This is true especially when it is only based on older photographic techniques. We concluded that photographic data involving longer orbital periods (where Doppler shifts due to the orbital motion are comparable or even less than the rotational broadening of the spectral lines) and early type stars (that have only a few and usually broad lines) should be revisited or at least used with caution. We demonstrate that for the five systems how CCD observations made with 2-m class telescopes can discover the binary nature or secondary spectra of many currently unresolved SB1 systems. Important astrophysical information such as the atmospheric parameters and the mass ratios are used to unravel previous misinterpretations of the data leading often to spurious orbits.

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Section: Hd 434supporting

confidence: 84%

“…HD 108642 HD 108642 (HIP 60890, m V = 6.5) is a well-known SB1 system. The most recent orbital elements are by Abt & Willmarth (1999): P = 11.7843 days, e = 0.0, γ = −0.7 km s −1 , and K = 41.14 km s −1 . According to Abt & Morell (1995) v sin i = 13 km s −1 , while Landstreet (1998) obtained v sin i < 4.5 km s −1 .…”

Section: Hd 434mentioning

confidence: 99%

A search for SB2 systems among selected Am binaries

et al. 2004

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“…The two measured radial velocities are also in agreement (see also Table 1) with the cluster mean. Fossati et al (2008) also collected the radial velocity measurements obtained in the past by Abt (1970), Conti et al (1974), Abt & Willmarth (1999), and Madsen et al (2002), concluding that all of these measurements are consistent with both each another and the cluster mean. In particular, Conti et al (1974) measured the radial velocity 33 times over 14 years.…”

Section: Close Companionmentioning

confidence: 61%

Explaining the Praesepe blue straggler HD 73666

Fossati¹,

Mochnacki²,

Landstreet³

et al. 2010

A&A

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Aims. The blue straggler phenomenon is not yet well explained by current theory, although evolutionary models of star clusters require a good knowledge of it. We attempt to develop a formation scenario for HD 73666, a blue straggler member of the Praesepe cluster. Methods. We compile the known physical properties of HD 73666 found in the literature, focusing in particular on possible binarity and the abundance pattern. Results. HD 73666 appears to be slowly rotating, have no detectable magnetic field, and have normal abundances, thereby excluding close binary evolution and mass transfer processes. There is no evidence of a hot radiation source. Conclusions. With the use of theoretical results on blue straggler formation present in literature, we are able to conclude that HD 73666 was probably formed by physical collision involving at least one binary system, between 5 and 350 Myr (50 Myr if the star is an intrinsic slow rotator) ago.

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“…The star was found to be an SB1 spectroscopic binary by Abt & Willmarth (1999) with P = 7.2204 days and with a practically circular orbit. Pribulla et al (2009c) combined new DDO RVs with those published by Abt & Willmarth (1999) to arrive at a circular orbit with the best period of P = 7.220299(18) days.…”

Section: Hd 73709 In Praesepementioning

confidence: 99%

Eclipsing binaries in the MOST satellite fields

et al. 2010

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Sixteen new eclipsing binaries have been discovered by the MOST satellite among guide stars used to point its telescope in various fields. Several previously known eclipsing binaries were also observed by MOST with unprecedented quality. Among the objects we discuss in more detail are short-period eclipsing binaries with eccentric orbits in young open clusters: V578 Mon in NGC 2244 and HD 47934 in NGC 2264. Long nearly-continuous photometric runs made it possible to discover three long-period eclipsing binaries with orbits seen almost edge-on: HD 45972 with P = 28.1 days and two systems (GSC 154 1247 and GSC 2141 526) with P > 25 days. The high precision of the satellite data led to discoveries of binaries with very shallow eclipses (e.g., HD 46180 with A = 0.016 mag, and HD 47934 with A = 0.025 mag). Ground-based spectroscopy to support the space-based photometry was used to refine the models of several of the systems.

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Binaries in the Praesepe and Coma Star Clusters and Their Implications for Binary Evolution

Cited by 46 publications

References 39 publications

A search for SB2 systems among selected Am binaries

A search for SB2 systems among selected Am binaries

Explaining the Praesepe blue straggler HD 73666

Eclipsing binaries in the MOST satellite fields

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