Extrasolar planets in stellar multiple systems

Roell, T.; Neuhäuser, R.; Seifahrt, Andreas; Mugrauer, M.

doi:10.1051/0004-6361/201118051

Cited by 138 publications

(154 citation statements)

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“…The planet host has a stellar companion of similar mass, therefore HD 106515Ab adds to the growing census of exoplanets in multiple systems (Desidera & Barbieri 2007;Roell et al 2012). The binary separation is quite wide and plausible orbits leave dynamically stable zones up to 40−80 AU around the stars.…”

Section: Discussionmentioning

confidence: 99%

A long-period massive planet around HD 106515A

Desidera¹,

Gratton²,

Carolo³

et al. 2012

A&A

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We have performed radial velocity (RV) monitoring of the components of the binary system HD 106515 over almost 11 years using the high-resolution spectrograph SARG at Telescopio Nazionale Galileo (TNG). The primary shows long-period radial velocity variations that indicate the presence of a low-mass companion whose projected mass is in the planetary regime (m sin i = 9.33 M J ). The 9.8 year orbit is quite eccentric (e = 0.57), as is typical for massive giant planets. Our results confirm the previously made preliminary announcement of the planet by Mayor et al. (2011, A&A, submitted [arXiv:1109.2497). The secondary instead does not show significant RV variations. The two components do not differ significantly in chemical composition, as was also found for other pairs of which one component hosts giant planets. Adaptive optics images obtained with TNG/AdOpt do not reveal additional stellar companions. From the analysis of the relative astrometry of the components of the wide pair we compute an upper limit on the mass of the newly detected companion of about 0.25 M . State-of-the-art or near-future instrumentation can provide true mass determination, thanks to the availability of the wide companion HD106515B as reference. Therefore, HD 106515Ab will allow a deeper insight into the transition region between planets and brown dwarfs.

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Section: Discussionmentioning

confidence: 99%

A long-period massive planet around HD 106515A

Desidera¹,

Gratton²,

Carolo³

et al. 2012

A&A

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“…Planet-hosting stars are sometimes present in binary systems (∼10-20%; Raghavan et al 2006;Roell et al 2012). Binarity increases intrinsic X-ray activity even in long-period systems, perhaps related to initial formation (Pye et al 1994).…”

Section: Binary Systemsmentioning

confidence: 99%

A Comprehensive Statistical Assessment of Star-Planet Interaction

Miller

Gallo

Wright

et al. 2015

ApJ

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We investigate whether magnetic interaction between close-in giant planets and their host stars produce observable statistical enhancements in stellar coronal or chromospheric activity. New Chandra observations of 12 nearby (d < 60 pc) planet-hosting solar analogs are combined with archival Chandra, XMM-Newton, and ROSAT coverage of 11 similar stars to construct a sample inoculated against inherent stellar class and planet-detection biases. Survival analysis and Bayesian regression methods (incorporating both measurements errors and X-ray upper limits; 13/23 stars have secure detections) are used to test whether "hot Jupiter" hosts are systematically more X-ray luminous than comparable stars with more distant or smaller planets. No significant correlations are present between common proxies for interaction strength (M P /a 2 or 1/a) versus coronal activity (L X or L X /L bol ). In contrast, a sample of 198 FGK main-sequence stars does show a significant (∼ 99% confidence) increase in X-ray luminosity with M P /a 2 . While selection biases are incontrovertibly present within the main-sequence sample, we demonstrate that the effect is primarily driven by a handful of extreme hot-Jupiter systems with M P /a 2 > 450 M Jup AU −2 , which here are all X-ray luminous but to a degree commensurate with their Ca II H and K activity, in contrast to presented magnetic star-planet interaction scenarios that predict enhancements relatively larger in L X . We discuss these results in the context of cumulative tidal spin-up of stars hosting close-in gas giants (potentially followed by planetary infall and destruction). We also test our main-sequence sample for correlations between planetary properties and UV luminosity or Ca II H and K emission, and find no significant dependence.

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“…The frequency of these planets may have a strong influence on the overall global frequency of extrasolar planets, allowing us to study the efficiency of planet formation mechanisms. Moreover, if there is any difference in the properties of planets in binary systems with respect to planets orbiting single stars, this may unveil effects caused by additional companions in stellar systems (Desidera & Barbieri 2010;Roell et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Precise radial velocities of giant stars

Ortiz

Reffert

Trifonov

et al. 2016

A&A

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G-and K-giant stars using the Hamilton Échelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m p sin i = 6.92 +0.18 −0.24 M Jup orbiting at a p = 1.0860 +0.0006 −0.0007 au from the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e B = 0.729 +0.004 −0.003 ) binary companion with a mass of m B sin i = 0.5296 +0.0011 −0.0008 M orbiting at a close separation from the giant primary with a semi-major axis of a B = 13.56 +0.18 −0.14 au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.

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Extrasolar planets in stellar multiple systems

Cited by 138 publications

References 100 publications

A long-period massive planet around HD 106515A

A long-period massive planet around HD 106515A

A Comprehensive Statistical Assessment of Star-Planet Interaction

Precise radial velocities of giant stars

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