A giant planet orbiting the ‘extreme horizontal branch’ star V 391 Pegasi

Silvotti, R.; Schuh, S.; Janulis, R.; Solheim, J. E.; Bernabei, S.; Østensen, R. H.; Oswalt, T. D.; Bruni, I.; Gualandi, R.; Bonanno, A.; Vauclair, G.; Reed, M. D.; Chen, C. W; Leibowitz, E. M.; Paparó, M.; Baran, A.; Charpinet, S.; Dolez, N.; Kawaler, S. D.; Kurtz, D. W.; Moskalik, P.; Riddle, R. L.; Zoła, S.

doi:10.1038/nature06143

Cited by 272 publications

(286 citation statements)

References 22 publications

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“…Several evolutionary channels have been proposed: (1) commonenvelope ejection channels, leading to sdBs in binaries with orbital periods below ∼10 d and a white dwarf or low-mass main sequence companion; (2) a stable Roche lobe overflow channel resulting in binary systems with orbital periods between ∼10 d and ∼100 d and much thicker hydrogen envelopes; and (3) a double helium white dwarf merger channel that gives rise to single sdB stars with very thin hydrogen envelopes and a wider mass range (Han et al 2002(Han et al , 2003. Recently, sdBs with planetary companions were found (Silvotti et al 2007;Charpinet et al 2011;Beuermann et al 2012), rejuvenating the idea that interactions of a star with a planetary companion might also lead to Appendix A is available in electronic form at http://www.aanda.org the formation of sdBs (Soker & Harpaz 2000). The evolutionary scenarios remain largely untested.…”

Section: Introduction and State Of The Artmentioning

confidence: 99%

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

Bloemen

Aerts

et al. 2014

A&A

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We have computed a new grid of evolutionary subdwarf B star (sdB) models from the start of central He burning, taking into account atomic diffusion due to radiative levitation, gravitational settling, concentration diffusion, and thermal diffusion. We have computed the non-adiabatic pulsation properties of the models and present the predicted p-mode and g-mode instability strips. In previous studies of the sdB instability strips, artificial abundance enhancements of Fe and Ni were introduced in the pulsation driving layers. In our models, the abundance enhancements of Fe and Ni occur naturally, eradicating the need to use artificial enhancements. We find that the abundance increases of Fe and Ni were previously underestimated and show that the instability strip predicted by our simulations solves the so-called blue edge problem of the subdwarf B star g-mode instability strip. The hottest known g-mode pulsator, KIC 10139564, now resides well within the instability strip even when only modes with low spherical degrees (l ≤ 2) are considered.

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Section: Introduction and State Of The Artmentioning

confidence: 99%

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

Bloemen

Aerts

et al. 2014

A&A

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“…The exoplanet encyclopedia 2 lists (as of April 20, 2012) 11 planetary systems (16 planets/4 multiple planet systems) detected by timing. This, however, includes a planet around the single pulsating variable star V391 Peg found by the timing technique (Silvotti et al, 2007).…”

Section: Previous and Ongoing Searches Of Circumbinary Exoplanets By mentioning

confidence: 99%

The Dwarf project: Eclipsing binaries – precise clocks to discover exoplanets

et al. 2012

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“…The role of planets in the formation of these systems have been explored by Bear & Soker (2011). A very interesting case along these lines is the planet found orbiting the Horizontal Branch star V391 Pegasi (Silvotti et al 2007). …”

Section: Planets and Horizontal Branch Starsmentioning

confidence: 99%

Planets, evolved stars, and how they might influence each other.

Villaver

2011

Proc. IAU

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Abstract. Over the last 20 years planetary searches have revealed a wealth of systems orbiting stars on the main sequence. Most of these low-mass stars eventually will evolve into the Giant phases before entering the planetary nebulae (PNe) stage. In the last years, the presence of planets has also been discovered around more massive evolved stars, mostly, along the Red Giant but also along the Horizontal Branch. Moreover, disks have been found around White Dwarfs presumably formed by tidally disrupted asteroids. In all, there is evidence that an evolved (ing) star might influence the survival of planets. In this review I will try to summarize such evidence but furthermore I will present the other side of the story, that is, how the presence of a planet might alter the evolution of stars and with that the PN formation.

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A giant planet orbiting the ‘extreme horizontal branch’ star V 391 Pegasi

Cited by 272 publications

References 22 publications

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

The Dwarf project: Eclipsing binaries – precise clocks to discover exoplanets

Planets, evolved stars, and how they might influence each other.

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