Follow‐up spectroscopic observations of HD 107148 B: A new white dwarf companion of an exoplanet host star

Mugrauer, M.; Dinçel, B.

doi:10.1002/asna.201512306

Cited by 29 publications

(3 citation statements)

References 38 publications

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“…detected in our surveys. This demonstrates the efficiency of these projects and shows that the multiplicity of the exoplanet host stars is significantly underestimated (see also Mugrauer &Dinçel 2016, andMugrauer et al 2014).…”

mentioning

confidence: 76%

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

Mugrauer¹,

Ginski

Vogt

et al. 2018

Proc. IAU

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In order to determine the true impact of stellar multiplicity on the formation and evolution of planets, we initiated direct imaging surveys to search for (sub)stellar companions of exoplanet host stars on close orbits, as their gravitational impact on the planet bearing disk at first and on formed planets afterwards is expected to be maximal. According to theory these are the most challenging environments for planet formation and evolution but might occur quite frequently in the milky way, due to the large number of multiple stars within our galaxy. On this poster we showed results, obtained so far in the course of our AO and Lucky-imaging campaigns of exoplanet host stars, conducted with NACO/ESO-VLT for southern and with AstraLux/CAHA2.2m for northern targets, respectively. In addition, we introduced our new high contrast imaging survey with SPHERE/ESO-VLT to search for close companions of southern exoplanet host stars, and presented some first results.

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mentioning

confidence: 76%

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

Mugrauer¹,

Ginski

Vogt

et al. 2018

Proc. IAU

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“…Later, Mugrauer et al (2014) confirmed the WD companion as HD 107148 B (we continue to call the main sequence star HD 107148 without adding an extra "A"). For the WD companion Mugrauer & Dinçel (2016) obtained a mass of M W D = 0.56 ± 0.05 M , an effective temperature of T eff = 6150 ± 250 K, a cooling age of 2.1 ± 0.27 Gyr, a surface gravity of log g = 7.95 ± 0.09 cm s −2 and a luminosity of L = (2.0 ± 0.2) × 10 −4 L . By assuming the initial-tofinal-mass-relation for white dwarfs from Catalan et al (2008), Mugrauer & Dinçel (2016) derived a progenitor mass of 1.4 ± 0.6M , leading to an estimated total age of 6.0 ± 4.8 Gyr for the WD companion.…”

Section: Stellar Parametersmentioning

confidence: 99%

Dynamical architecture of the HD 107148 system

Eberhardt,

Trifonov,

Kürster

et al. 2022

Preprint

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We present an independent Doppler validation and dynamical orbital analysis of the two-planet system HD 107148, which was recently announced in Rosenthal et al. (2021). Our detailed analyses are based on literature HIRES data and newly obtained HARPS and CARMENES radial velocity (RV) measurements as part of our survey in search for additional planets around single planet systems. We perform a periodogram analysis of the available HIRES and HARPS precise RVs and stellar activity indicators. We do not find any apparent correlation between the RV measurements and the stellar activity indicators, thus linking the two strong periodicities to a moderately compact multipleplanet system. We carry out orbital fitting analysis by testing various one-and two-planet orbital configurations and studying the posterior probability distribution of the fitted parameters. Our results solidify the existence of a Saturn-mass planet (HD 107148 b, discovered first) with a period P b ∼ 77.2 d, and a second, eccentric (e c ∼ 0.4), Neptune-mass exoplanet (HD 107148 c), with an orbital period of P c ∼ 18.3 d. Finally, we investigate the two-planet system's long-term stability and overall orbital dynamics with the posterior distribution of our preferred orbital configuration. Our N-body stability simulations show that the system is long-term stable and exhibits large secular osculations in eccentricity but in no particular mean-motion resonance configuration. The HD 107148 system, consisting of a Solar-type main sequence star with two giant planets in a rare configuration, features a common proper motion white dwarf companion and is, therefore, a valuable target for understanding the formation and evolution of planetary systems.

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“…In the Chandra observation, the primary was detected, while Tidal star-planet interaction 23 the secondary was not. The secondary component is a white dwarf (Mugrauer & Dincel 2016). The angular separation between the components is ρ = 35.0 .…”

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confidence: 99%

Tidal star-planet interaction and its observed impact on stellar activity in planet-hosting wide binary systems

Ilic,

Poppenhaeger,

Hosseini

2022

Preprint

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Tidal interaction between an exoplanet and its host star is a possible pathway to transfer angular momentum between the planetary orbit and the stellar spin. In cases where the planetary orbital period is shorter than the stellar rotation period, this may lead to angular momentum being transferred into the star's rotation, possibly counteracting the intrinsic stellar spin-down induced by magnetic braking. Observationally, detecting altered rotational states of single, cool field stars is challenging, as precise ages for such stars are rarely available. Here we present an empirical investigation of the rotation and magnetic activity of a sample of planet-hosting stars that are accompanied by wide stellar companions. Without needing knowledge about the absolute ages of the stars, we test for relative differences in activity and rotation of the planet hosts and their co-eval companions, using X-ray observations to measure the stellar activity levels. Employing three different tidal interaction models, we find that host stars with planets that are expected to tidally interact display elevated activity levels compared to their companion stars. We also find that those activity levels agree with the observed rotational periods for the host stars along the usual rotation-activity relationships, implying that the effect is indeed caused by a tidal interaction and not a purely magnetic interaction which would be expected to affect the stellar activity, but not necessarily the rotation. We conclude that massive, close-in planets have an impact on the stellar rotational evolution, while the smaller, more distant planets do not have a significant influence.

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Follow‐up spectroscopic observations of HD 107148 B: A new white dwarf companion of an exoplanet host star

Cited by 29 publications

References 38 publications

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

Dynamical architecture of the HD 107148 system

Tidal star-planet interaction and its observed impact on stellar activity in planet-hosting wide binary systems

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