An Introduction to Close Binary Stars

By R. Hilditch. 2001

471 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/fe05f554872afa85a01f8fc8aa4c0a90f610db0e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

1. J. Southworth
2. J. Winn
3. Nuno C. Santos
4. M. Perryman
5. F. Bouchy
6. C. Mordasini
7. M. Mayor
8. S. Udry

Citations in the corpus

• The First DIRECT Distance Determination to a Detached Eclipsing Binary in M33 (2006, background): “Hilditch (2001) estimates the effect to be ∼ 50% for hydrogen lines and ∼ 10% for helium lines, for velocity differences between components of less than 200 km s−1.”
• Forty eclipsing binaries in the Small Magellanic Cloud: fundamental parameters and Cloud distance (2003, background): “tre of mass (see e.g., Kopal 1959, Hilditch 2001 for descriptions and bibliographic references).”
• The Rossiter-McLaughlin effect of CoRoT-3b and HD 189733b (2009, methodology): “The RV curve is modelled by the standard orbital equations (Mayor & Queloz 1995; Hilditch 2001) and by the code presented in Giménez (2006b) for the RM effect.”
• Transits and Occultations (2010, background): “Modelers of eclipsing binary stars have long needed to take into account these and other subtle effects (Kallrath & Milone 2009, Hilditch 2001).”
• Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, methodology): “(2008) WASP-7 97± 13 Hellier et al. (2009b) 6400± 100 Hellier et al. (2009b) 0.00± 0.10 Hellier et al. (2009b) XO-4 165.8± 6.2 Narita et al. (2010) 6397± 70 McCullough et al.”
• Ten eclipsing binaries in the Small Magellanic Cloud: fundamental parameters and SMC distance (2002, background): “…systems considered here may have significant tidal distortions, in which case the centre of light (specifically, the weighted mean line velocity) will not follow the cen- c© 0000 RAS, MNRAS 000, 000–000 tre of mass (see e.g., Kopal 1959, Hilditch 2001 for descriptions and bibliographic references).”
• KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, background): ““Why does nature form exoplanets easily?,” ponders Heng (2012). Both planetary formation scenarios of core accretion and gravitational collapse require complex processes at work and even more so for the violent environments of CBPs.”
• Search for brown-dwarf companions of stars (2010, methodology): “To develop our approach, we list the standard formulae (e.g. Hilditch 2001) applicable to such a system.”
• Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, background): “XO-3 is also known to exhibit a large spin–orbit misalignment (Hébrard et al. 2008; Winn et al. 2009) suggestive of dynamical evolution through gravitational interactions (e.g. Fabrycky & Winn 2009). In the following analysis I adopt the constraints e = 0.2884 ± 0.0035 and ω = 346.3 ± 1.3, taken fro”