Indications for an influence of hot Jupiters on the rotation and activity of their host stars

Poppenhaeger, Katja; Wolk, S. J.

doi:10.1051/0004-6361/201423454

Cited by 126 publications

(131 citation statements)

References 47 publications

Supporting

Mentioning

123

Contrasting

Order By: Relevance

“…Moreveor, the existence of the stationary state implies that stars hosting close-in companions may not be as strongly braked by their wind as their counterparts without companions. Therefore, the gyrochronology law for exoplanets host must be calibrated on a suitable sample and take this effect into account (see Pont 2009;Lanza 2010;Poppenhaeger & Wolk 2014).…”

Section: Resultsmentioning

confidence: 99%

Evolution of angular-momentum-losing exoplanetary systems

Damiani

Lanza

2015

A&A

View full text Add to dashboard Cite

Aims. We assess the importance of tidal evolution and its interplay with magnetic braking in the population of hot-Jupiter planetary systems. Methods. By minimizing the total mechanical energy of a given system under the constraint of stellar angular momentum loss, we rigorously find the conditions for the existence of dynamical equilibrium states. We estimate their duration, in particular when the wind torque spinning down the star is almost compensated for by the tidal torque spinning it up. We introduce dimensionless variables to characterize the tidal evolution of observed hot Jupiter systems and discuss their spin and orbital states using generalized Darwin diagrams based on our new approach. Results. We show that their orbital properties are related to the effective temperature of their host stars. The long-term evolution of planets orbiting F-and G-type stars is significantly different owing to the combined effect of magnetic braking and tidal dissipation. The existence of a quasi-stationary state, in the case of short-period planets, can significantly delay their tidal evolution that would otherwise bring the planet to fall into its host star. Most of the planets known to orbit F-type stars are presently found to be near this stationary state, probably in a configuration not too far from what they had when their host star settled on the zero-age main sequence. Considering the importance of angular momentum loss in the early stages of stellar evolution, our results indicate that it has to be considered to properly test the migration scenarios of planetary system formation.

show abstract

Section: Resultsmentioning

confidence: 99%

Evolution of angular-momentum-losing exoplanetary systems

Damiani

Lanza

2015

A&A

View full text Add to dashboard Cite

show abstract

“…If the stellar rotation period is longer than the orbital period of the planet, it is possible that the tidal interaction induces a torque on the host star and reduces the stellar spin-down with age (Poppenhaeger & Wolk 2014). Based on measured X-ray luminosities Poppenhaeger & Wolk predict stellar ages of binaries, where the primary features a hot Jupiter in a close orbit.…”

Section: Angular Momentum Transfer From Hot Jupiters To Their Host Starsmentioning

confidence: 99%

“…For the three binaries among our targets we derive X-ray based age estimates, using the relationship from Poppenhaeger & Wolk (2014) . The upper limits for the X-ray luminosity of the secondaries provide lower limits for their ages.…”

Section: Angular Momentum Transfer From Hot Jupiters To Their Host Starsmentioning

confidence: 99%

High-energy irradiation and mass loss rates of hot Jupiters in the solar neighborhood

Salz

Schneider

Czesla

et al. 2015

A&A

View full text Add to dashboard Cite

Giant gas planets in close proximity to their host stars experience strong irradiation. In extreme cases photoevaporation causes a transonic, planetary wind and the persistent mass loss can possibly affect the planetary evolution. We have identified nine hot Jupiter systems in the vicinity of the Sun, in which expanded planetary atmospheres should be detectable through Lyα transit spectroscopy according to predictions. We use X-ray observations with Chandra and XMM-Newton of seven of these targets to derive the highenergy irradiation level of the planetary atmospheres and the resulting mass loss rates. We further derive improved Lyα luminosity estimates for the host stars including interstellar absorption. According to our estimates WASP-80 b, WASP-77 b, and WASP-43 b experience the strongest mass loss rates, exceeding the mass loss rate of HD 209458 b, where an expanded atmosphere has been confirmed. Furthermore, seven out of nine targets might be amenable to Lyα transit spectroscopy. Finally, we check the possibility of angular momentum transfer from the hot Jupiters to the host stars in the three binary systems among our sample, but find only weak indications for increased stellar rotation periods of WASP-77 and HAT-P-20.

show abstract

“…However, in the cases of stars with hot Jupiters, the rotation and the activity tracers can be affected by the interaction with the planet, thus biasing the estimate of the age of the host star. Pillitteri et al (2010Pillitteri et al ( , 2011Pillitteri et al ( , 2014; Poppenhaeger et al (2013);Poppenhaeger & Wolk (2014) and Schröter et al (2011) have found that the hot Jupiter hosting stars HD 189733 and CoRoT-2A have most likely been spun up by their close in planets, and thus their activity and rotation have been enhanced, thereby mimicking the behavior of younger stars. In HD 189733, activity tracers like X-ray luminosity would assign an age in the range 0.6-1.1 Gyr (Melo et al 2006;Sanz-Forcada et al 2011), while the stellar companion is much older.…”

Section: Age Of Wasp-18mentioning

confidence: 99%

No X-rays from WASP-18

Pillitteri

Wolk

Sciortino

et al. 2014

A&A

View full text Add to dashboard Cite

About 20% of the >1000 known exoplanets are Jupiter analogs orbiting very close to their parent stars. It is still under debate to what detectable level such hot Jupiters possibly affect the activity of the host stars through tidal or magnetic star-planet interaction. In this paper we report on an 87 ks Chandra observation of the hot Jupiter hosting star WASP-18. This system is composed of an F6 type star and a hot Jupiter of mass 10.4 M Jup orbiting in less than 20 hr around the parent star. On the basis of an isochrone fitting, WASP-18 is thought to be 600 Myr old and within the range of uncertainty of 0.5-2 Gyr. The star is not detected in X-rays down to a luminosity limit of 4 × 10 26 erg/s, which is more than two orders of magnitude lower than expected for a star of this age and mass. This value proves an unusual lack of activity for a star with an estimated age around 600 Myr. We argue that the massive planet can play a crucial role in disrupting the stellar magnetic dynamo created within its thin convective layers. Other additional 212 X-ray sources are detected in the Chandra image. We list them and briefly discuss their nature.

show abstract

Indications for an influence of hot Jupiters on the rotation and activity of their host stars

Cited by 126 publications

References 47 publications

Evolution of angular-momentum-losing exoplanetary systems

Evolution of angular-momentum-losing exoplanetary systems

High-energy irradiation and mass loss rates of hot Jupiters in the solar neighborhood

No X-rays from WASP-18

Contact Info

Product

Resources

About