Interferometric Astrometry of Proxima Centauri and Barnard's Star Using [ITAL]HUBBLE SPACE TELESCOPE[/ITAL] Fine Guidance Sensor 3: Detection Limits for Substellar Companions

Benedict, G. F.; McArthur, B.; Chappell, David W.; Nelan, Edmund; Jefferys, W. H.; Altena, W. van; Lee, J.; Cornell, David A.; Shelus, P. J.; Hemenway, P. D.; Franz, O. G.; Wasserman, L. H.; Duncombe, R. L.; Story, D.; Whipple, A. L.; Fredrick, L. W.

doi:10.1086/300975

Cited by 324 publications

(107 citation statements)

References 42 publications

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“…Wavelength ( Proxima (Benedict et al 1998(Benedict et al , 1999, and is consistent with the 8% flux modulation seen in Anglada-Escudé et al (2016). However, no de-trending or pre-whitening was performed to remove this slow stellar variability, as it did not affect our ability to detect flares or measure their energies.…”

Section: Identifying White Light Flaressupporting

confidence: 74%

Most Observations of Our Nearest Neighbor: Flares on Proxima Centauri

Davenport

Kipping

Sasselov

et al. 2016

ApJL

119

117

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We present a study of white light flares from the active M5.5 dwarf Proxima Centauri using the Canadian microsatellite MOST. Using 37.6 days of monitoring data from 2014 and 2015, we have detected 66 individual flare events, the largest number of white light flares observed to date on Proxima Cen. Flare energies in our sample range from 10 29 -10 31.5 erg,. The flare rate is lower than that of other classic flare stars of similar spectral type, such as UV Ceti, which may indicate Proxima Cen had a higher flare rate in its youth. Proxima Cen does have an unusually high flare rate given its slow rotation period, however. Extending the observed power-law occurrence distribution down to 10 28 erg, we show that flares with flux amplitudes of 0.5% occur 63 times per day, while superflares with energies of 10 33 erg occur ∼8 times per year. Small flares may therefore pose a great difficulty in searches for transits from the recently announced 1.27 M ⊕ Proxima b, while frequent large flares could have significant impact on the planetary atmosphere.

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Section: Identifying White Light Flaressupporting

confidence: 74%

Most Observations of Our Nearest Neighbor: Flares on Proxima Centauri

Davenport

Kipping

Sasselov

et al. 2016

ApJL

119

117

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“…The limits determined from the CES RV data can be combined with the astrometric companion limits based on the HST Fine Guidance Sensor (Benedict et al 1999). This combination is very effective since both methods are complementary to each other (the RV method is more sensitive to close-by companions while for astrometry the detectability of more distant companions is better).…”

Section: Resulting Companion Limitsmentioning

confidence: 99%

The planet search program at the ESO Coudé Echelle spectrometer

Endl

Kürster

Els

et al. 2002

A&A

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Abstract. We present the complete results of the planet search program carried out at the ESO Coudé Echelle Spectrometer (CES) on La Silla, using the Long Camera from Nov. 1992 to April 1998. The CES survey has monitored 37 late-type (F8V -M5V) stars in the southern hemisphere for variations in their differential radial velocities (RV) in order to detect Doppler reflex motions caused by planetary companions. This led to the discovery of the first extrasolar planet in an Earth-like orbit around the young (ZAMS) and active G0V star ι Horologii . Here we present the RV results for all survey stars and perform a statistical examination of the whole data-set. Each star is tested for RV variability, RV trends (linear and non-linear) and significant periodic signals. β Hyi and Ind are identified as long-term, low-amplitude RV variables. Furthermore, for 30 CES survey stars we determine quantitative upper mass-limits for giant planets based on our long-term RV results. We find that the CES Long Camera survey would have detected short-period ("51 Peg-type") planets around all 30 stars but no planets with m sin i < 1 M Jup at orbital separations larger than 2 AU. Finally, we demonstrate that the CES planet search can be continued without applying velocity corrections to the RV results coming from the currently installed Very Long Camera at the CES.

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“…Physical properties of the stars in α Centauri system. (a) Pourbaix et al (1999); (b) Benedict et al (1999 the Radau (Everarth 1985) integrators. The region between 2.0 and 2.5 AU is the outermost zone initially populated by protoplanets in our simulations and the most critical since the perturbations of the companion star are stronger.…”

Section: The Numerical Modelmentioning

confidence: 99%

Formation of terrestrial planets in close binary systems: The case ofαCentauri A

Barbieri

Marzari

Scholl

2002

A&A

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Abstract.At present the possible existence of planets around the stars of a close binary system is still matter of debate. Can planetary bodies form in spite of the strong gravitational perturbations of the companion star? We study in this paper via numerical simulation the last stage of planetary formation, from embryos to terrestrial planets in the α Cen system, the prototype of close binary systems. We find that Earth class planets can grow around α Cen A on a time-scale of 50 Myr. In some of our numerical models the planets form directly in the habitable zone of the star in low eccentric orbits. In one simulation two of the final planets are in a 2:1 mean motion resonance that, however, becomes unstable after 200 Myr. During the formation process some planetary embryos fall into the stars possibly altering their metallicity.

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Interferometric Astrometry of Proxima Centauri and Barnard's Star Using [ITAL]HUBBLE SPACE TELESCOPE[/ITAL] Fine Guidance Sensor 3: Detection Limits for Substellar Companions

Cited by 324 publications

References 42 publications

Most Observations of Our Nearest Neighbor: Flares on Proxima Centauri

Most Observations of Our Nearest Neighbor: Flares on Proxima Centauri

The planet search program at the ESO Coudé Echelle spectrometer

Formation of terrestrial planets in close binary systems: The case ofαCentauri A

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