First Results from the CHARA Array. V. Binary Star Astrometry: The Case of 12 Persei

Bagnuolo, W. G.; Taylor, Stuart F.; McAlister, Harold A.; Brummelaar, T. ten; Gies, Douglas R.; Ridgway, Stephen T.; Sturmann, J.; Sturmann, L.; Turner, N.; Berger, David H.; Gudehus, D. H.

doi:10.1086/501232

Cited by 25 publications

(10 citation statements)

References 9 publications

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“…12 Per : for this P = 331 d double‐lined spectroscopic binary Bagnuolo et al (2006) recently obtained precise values for the orbital parallax π= 41.19 ± 0.21 mas and the mass sum M Σ = 2.622 ± 0.034 M ⊙ . With reference to the mass ratio q = 0.897 ± 0.007 formerly derived by Barlow, Scarfe & Fekel (1998) individual masses of M A = 1.382 ± 0.019 M ⊙ and M B = 1.240 ± 0.017 M ⊙ follow.…”

Section: Visual and Spectroscopic Binaries Or Multiple Systemsmentioning

confidence: 96%

Nearby stars of the Galactic disc and halo – IV

Fuhrmann

2008

Monthly Notices RAS

193

165

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The Milky Way Galaxy has an age of about 13 billion years. Solar‐type stars evolve all the long way to the realm of degenerate objects on essentially this time‐scale. This, as well as the particular advantage that the Sun offers through reliable differential spectroscopic analyses, render these stars the ideal tracers for the fossil record of our parent spiral. Astrophysics is a science that is known to be notoriously plagued by selection effects. The present work – with a major focus in this fourth contribution on model atmosphere analyses of spectroscopic binaries and multiple star systems – aims at a volume‐complete sample of about 300 nearby F‐, G‐, and K‐type stars that particularly avoids any kinematical or chemical pre‐selection from the outset. It thereby provides an unbiased record of the local stellar populations – the ancient thick disc and the much younger thin disc. On this base, the detailed individual scrutiny of the long‐lived stars of both populations unveils the thick disc as a single‐burst component with a local normalization of no less than 20 per cent. This enormous fraction, combined with its much larger scaleheight, implies a mass for the thick disc that is comparable to that of the thin disc. On account of its completely different mass‐to‐light ratio the thick disc thereby becomes the dark side of the Milky Way, an ideal major source for baryonic dark matter. This massive, ancient population consequently challenges any gradual build‐up scenario for our parent spiral. Even more, on the supposition that the Galaxy is not unusual, the thick disc – as it emerges from this unbiased spectroscopic work – particularly challenges the hierarchical cold‐dark‐matter‐dominated formation picture for spiral galaxies in general.

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Section: Visual and Spectroscopic Binaries Or Multiple Systemsmentioning

confidence: 96%

Nearby stars of the Galactic disc and halo – IV

Fuhrmann

2008

Monthly Notices RAS

193

165

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“…At the time of writing this paper over a third of the papers published by our group and our collaborators are based on data obtained with CHARA/CLIMB. Some areas of research have been particularly productive, for example oblate fast rotators (McAlister et al, 2005;van Belle et al, 2006;Aufdenberg et al, 2006), Be stars (Gies et al, 2007;Touhami et al, 2013) Exoplanet host stars (Baines et al, 2007(Baines et al, , 2008a(Baines et al, ,b, 2009(Baines et al, , 2010bvon Braun et al, 2011a,b;Baines et al, 2011a;von Braun et al, 2012;Baines et al, 2012) the fundamental parameters of a wide range of stellar types (Berger et al, 2006a;Ciardi et al, 2007;Boyajian et al, 2008Boyajian et al, , 2009Baines et al, 2010aBaines et al, , 2011bSimon & Schaefer, 2011;Boyajian et al, 2012a,b;Baines et al, 2013;Boyajian et al, 2013) and binary and multiple star systems (Bagnuolo et al, 2006;Csizmadia et al, 2009;Farrington et al, 2010;Raghavan et al, 2010;O'Brien et al, 2011;ten Brummelaar et al, 2011;Raghavan et al, 2012). More recently we have obtained the first images based solely on CLIMB data.…”

Section: Resultsmentioning

confidence: 99%

The Classic/Climb Beam Combiner at the Chara Array

Brummelaar

Sturmann

Ridgway

et al. 2013

J. Astron. Instrum.

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In the same way that every telescope has multiple instruments and cameras, an interferometric array like the CHARA Array will have numerous beam combiners at the back end. And like the instruments of a single telescope, each of these combiners will be optimized for a particular kind of observation or scientific program. In this paper we describe the CLASSIC and CLIMB beam combiners of the CHARA Array. Both are open air, aperture plane, wide bandwidth single spectral channel instruments optimized for sensitivity. CLASSIC is the original two beam combiner used for the first science at CHARA, and it still has the faintest magnitude limit. CLIMB is a three beam expansion of CLASSIC that can also provide closure phase measurements.

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“…Bagnuolo et al (2006) Beta Lyrae is the prototypical binary caught still in its rapid mass transfer phase. The rate is 10 −5 M per year say Nazarenko and Glazunova (2006).…”

Section: Binary Evolutionmentioning

confidence: 99%

Astrophysics in 2006

2007

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The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries.Comment: 244 pages, no figure

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First Results from the CHARA Array. V. Binary Star Astrometry: The Case of 12 Persei

Cited by 25 publications

References 9 publications

Nearby stars of the Galactic disc and halo – IV

Nearby stars of the Galactic disc and halo – IV

The Classic/Climb Beam Combiner at the Chara Array

Astrophysics in 2006

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