THREE-DIMENSIONAL GAS DYNAMIC SIMULATION OF THE INTERACTION BETWEEN THE EXOPLANET WASP-12b AND ITS HOST STAR

Bisikalo, D. V.; Kaygorodov, P. V.; Ionov, D. E.; Shematovich, V. I.; Lämmer, H.; Fossati, L.

doi:10.1088/0004-637x/764/1/19

Cited by 145 publications

(108 citation statements)

References 21 publications

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“…We find that no lines or continuum absorption sources appear in the NUV (NUVA, NUVB, NUVC filters) space-based wavelengths unless the cloud temperatures are below 10,000 K ( Figure 6). This suggests that whatever caused the early ingress in WASP-12b (Fossati et al 2010;Haswell et al 2012;Nichols et al 2015) was not from shocked stellar wind gas but is more likely planetary gas as has been previously suggested (Lanza 2009;Lai, Helling & van den Heuvel 2010;Bisikalo et al 2013a;Bisikalo et al 2013b;Cherenkov, Bisikalo & Kaigorodov 2014;Lanza 2015). An escaping atmosphere of WASP-12b would also explain the variability in the complete set of near-UV observations (Fossati et al 2010;Haswell et al 2012;Sing et al 2013;Nichols et al 2015).…”

Section: Discussionsupporting

confidence: 51%

“…Our conclusions add to a body of theoretical work suggesting that UV asymmetry observations are not suitable approach for exoplanet magnetic field detection (Ben-Jaffel & Ballester 2014;Grießmeier 2015;Alexander et al 2015). Additionally, our modeling of lower temperature clouds suggests that the UV and optical observations are likely caused by gas from the planetary atmosphere (Lai, Helling & van den Heuvel 2010;Bisikalo et al 2013a;Bisikalo et al 2013b;Cherenkov, Bisikalo & Kaigorodov 2014). Therefore, any future models attempting to explain the early UV observation need to include planetary gas in their simulations.…”

Section: Discussionmentioning

confidence: 57%

“…Using the plasma photoionization and microphysics code CLOUDY (Ferland et al 1998;Ferland et al 2013) we explore whether there is a UV absorbing species in the stellar wind that can cause an early UV ingress in the transits of closein exoplanets due to the presence of a magnetic (Vidotto, Jardine & Helling 2011a) or non-magnetic (Lai, Helling & van den Heuvel 2010;Bisikalo et al 2013a;Bisikalo et al 2013b) bow shock compressing the coronal plasma. We find under realistic physical conditions for the corona (Table 1; § 3) that there aren't any species that can cause an absorption with sufficient opacity for all UV wavelengths and also for all other wavelengths between X-ray and radio (Figures 4 and 5).…”

Section: Discussionmentioning

confidence: 99%

“…A model ignoring magnetic fields has recently been proposed to explain the WASP-12b HST observations (Bisikalo et al 2013a;Bisikalo et al 2013b; see also Lai, Helling & van den Heuvel 2010). These authors perform hydrodynamic simulations in 3-D and looked at the interaction between the stellar wind and the escaping planetary atmosphere.…”

Section: Introductionmentioning

confidence: 99%

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Investigation of the environment around close-in transiting exoplanets using cloudy

Turner

Christie

Arras

et al. 2016

Mon. Not. R. Astron. Soc.

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It has been suggested that hot stellar wind gas in a bow shock around an exoplanet is sufficiently opaque to absorb stellar photons and give rise to an observable transit depth at optical and UV wavelengths. In the first part of this paper, we use the CLOUDY plasma simulation code to model the absorption from X-ray to radio wavelengths by 1-D slabs of gas in coronal equilibrium with varying densities (10 4 − 10 8 cm −3 ) and temperatures (2000 − 10 6 K) illuminated by a solar spectrum. For slabs at coronal temperatures (10 6 K) and densities even orders of magnitude larger than expected for the compressed stellar wind (10 4 − 10 5 cm −3 ), we find optical depths orders of magnitude too small (> 3 × 10 −7 ) to explain the ∼ 3% UV transit depths seen with Hubble. Using this result and our modeling of slabs with lower temperatures (2000 − 10 4 K), the conclusion is that the UV transits of WASP-12b and HD 189733b are likely due to atoms originating in the planet, as the stellar wind is too highly ionized. A corollary of this result is that transport of neutral atoms from the denser planetary atmosphere outward must be a primary consideration when constructing physical models. In the second part of this paper, additional calculations using CLOUDY are carried out to model a slab of planetary gas in radiative and thermal equilibrium with the stellar radiation field. Promising sources of opacity from the X-ray to radio wavelengths are discussed, some of which are not yet observed.

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Section: Discussionsupporting

confidence: 51%

Section: Discussionmentioning

confidence: 57%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Investigation of the environment around close-in transiting exoplanets using cloudy

Turner

Christie

Arras

et al. 2016

Mon. Not. R. Astron. Soc.

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“…According to these data, the beginning of the transit in some light curves leads the beginning of the transit in the visible by approximately 50 min, testifying to the presence of absorbing material located ahead of the planet at a distance of roughly four to five planetary radii. Bisikalo et al [270] proposed that the earlier eclipse could arise due to the formation of a closed, aspherical envelope around WASP-12b, whose size substantially exceeds the limits of its Roche lobe.…”

Section: Uv Line Emission From the Atmospheres Of Exoplanetsmentioning

confidence: 99%

Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

et al. 2016

Self Cite

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Abstract-The article presents a review of scientific problems and methods of ultraviolet astronomy, focusing on perspective scientific problems (directions) whose solution requires UV space observatories. These include reionization and the history of star formation in the Universe, searches for dark baryonic matter, physical and chemical processes in the interstellar medium and protoplanetary disks, the physics of accretion and outflows in astrophysical objects, from Active Galactic Nuclei to close binary stars, stellar activity (for both low-mass and high-mass stars), and processes occurring in the atmospheres of both planets in the solar system and exoplanets. Technological progress in UV astronomy achieved in recent years is also considered. The well advanced, international, Russian-led Spektr-UV (World Space Observatory-Ultraviolet) project is described in more detail. This project is directed at creating a major space observatory operational in the ultraviolet (115-310 nm). This observatory will provide an effective, and possibly the only, powerful means of observing in this spectral range over the next ten years, and will be an powerful tool for resolving many topical scientific problems.

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Hot Jupiters accreting onto their parent stars: Effects on the stellar activity

et al. 2021

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Hot Jupiters (HJs) are massive gaseous planets orbiting close to their host stars.Due to their physical characteristics and proximity to the central star, HJs are the natural laboratories to study the process of stellar-planet interaction (SPI). Phenomena related to SPI may include the inflation and evaporation of planetary atmospheres, the formation of cometary tails and bow shocks and magnetospheric interaction between the magnetic field of the planet and that of the star. Several works suggest that some systems show enhanced stellar activity in phase with the planetary rotation period. In this work, we use a 3D magneto-hydrodynamic model that describes a system composed by a star and a HJ and that includes the corresponding planetary and stellar winds. The aim is to investigate whether the material evaporating from the planet interacts with the stellar extended corona, and generates observable features. Our simulation shows that, in some conditions, the planetary wind expands and propagates mainly along the planetary orbit. Moreover, part of the planetary wind collides with the stellar wind and a fraction of the planet's outflow is funneled by the stellar magnetic field and hits the stellar surface. In both events, the material is heated up to temperatures of a few MK by a shock. These phenomena could manifest in the form of enhanced stellar activity at some orbital phases of the planet.

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THREE-DIMENSIONAL GAS DYNAMIC SIMULATION OF THE INTERACTION BETWEEN THE EXOPLANET WASP-12b AND ITS HOST STAR

Cited by 145 publications

References 21 publications

Investigation of the environment around close-in transiting exoplanets using cloudy

Investigation of the environment around close-in transiting exoplanets using cloudy

Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

Hot Jupiters accreting onto their parent stars: Effects on the stellar activity

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