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[PDF] Top 20 Star planet interactions: I Stellar rotation and planetary orbits

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Star planet interactions: I  Stellar rotation and planetary orbits

Star planet interactions: I Stellar rotation and planetary orbits

... of rotation do not pro- duce overlaps between the curves, indicating that the change that is due to the initial mass dominates over the change that is due to rotation (at least for the range of ... See full document

14

Star-planet-debris disc alignment in the HD 82943 system: Is planetary system coplanarity actually the norm?

Star-planet-debris disc alignment in the HD 82943 system: Is planetary system coplanarity actually the norm?

... derived planet inclinations and suggesting that the planets and debris disc are consistent with being aligned at a level similar to the Solar ...the stellar equator is inferred to be inclined by 28 ± 4 ◦ , ... See full document

6

Monte Carlo Simulations of Stellar Planet Capture and Orbital Perturbations in Rogue Star – Solar System Interactions

Monte Carlo Simulations of Stellar Planet Capture and Orbital Perturbations in Rogue Star – Solar System Interactions

... The simulations were developed in C++ code using Microsoft Visual C++ 2010 Express. The dynamical evolution of the Solar System was determined using a numerical analysis algorithm with small time increments of 600 ... See full document

12

Finding exoplanets orbiting young active stars - I. Technique

Finding exoplanets orbiting young active stars - I. Technique

... sin i that is lower than the resolution of the spectrograph, due to the fact the spot cannot be resolved ...a planet signal) then the correlation may in fact be ...uncover planet signals from ... See full document

13

Star-planet interactions and dynamical evolution of exoplanetary systems

Star-planet interactions and dynamical evolution of exoplanetary systems

... the star is less than 0.1 AU and interactions with the host through radiation, magnetism or tides may be ...of star- planet interactions because their high-precision, high-duty cycle ... See full document

7

The unstable fate of the planet orbiting the A star in the HD 131399 triple stellar system

The unstable fate of the planet orbiting the A star in the HD 131399 triple stellar system

... of planetary systems at different ages help piece together their life ...Main-sequence planetary studies have now begun to utilize white dwarf atmosphere chemical signatures in their planetary forma- ... See full document

7

MOVES – I  The evolving magnetic field of the planet hosting star HD189733

MOVES – I The evolving magnetic field of the planet hosting star HD189733

... the planet is outside the Source Sur- face, we proceed as follows to calculate the field at its po- ...the stellar field is purely radial, the merid- ional and azimuthal components are ...the ... See full document

14

Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?

Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?

... of planet-hosting stars, I have shown that there seems to be a small, global discrepancy between the results that are produced by the two ...to stellar effective temperature, with isochrone fitting ... See full document

19

Star planet interactions: II  is planet engulfment the origin of fast rotating red giants?

Star planet interactions: II is planet engulfment the origin of fast rotating red giants?

... a planet en- gulfment is compared for stars with di ff erent initial ...given planet mass and a given initial dis- tance between the star and the planet, the engulfment occurs at a higher ... See full document

16

MOVES   II  Tuning in to the radio environment of HD189733b

MOVES II Tuning in to the radio environment of HD189733b

... predicted planetary radio emis- sion could propagate, and found that HD189733b orbits in and out of regions where the planetary emission will be ab- sorbed by the stellar ...the planet ... See full document

11

Anticipating Tathreeine: searching for stable planetary orbits around a compact hierarchical triple

Anticipating Tathreeine: searching for stable planetary orbits around a compact hierarchical triple

... It has been pointed out (Perryman 2011) that, based on limited data, planets with the highest eccentricities (e > 0.8) tend to be accompanied by a stellar or brown dwarf companion. This suggests eccentricities ... See full document

133

Doppler monitoring of five k2 transiting planetary systems

Doppler monitoring of five k2 transiting planetary systems

... the planetary radius, we combined the measured transit depth with the stellar parameters derived from broadband photo- ...transiting planet candidates, especially those close to mean-motion ... See full document

16

An evaporating planet in the wind: Stellar wind interactions with the radiatively braked exosphere of GJ 436 b

An evaporating planet in the wind: Stellar wind interactions with the radiatively braked exosphere of GJ 436 b

... the stellar and planetary gravities, the stellar radiation pressure, and the inertial force linked to the non- Galilean stellar reference ...the stellar wind ...the star-Earth ... See full document

14

Stellar magnetic activity – Star-Planet Interactions

Stellar magnetic activity – Star-Planet Interactions

... by stellar rotation and produces highly structured magnetic fields; in the case of stars with a radiative core and a convective outer envelope (spectral type mid-F to early-M), this is an αΩ dynamo, while ... See full document

6

The formation of retrograde planetary orbits by close stellar encounters

The formation of retrograde planetary orbits by close stellar encounters

... the planetary system, the generation of large inclinations might be explained if stellar encounters are considered as an impetus for subsequent ...perturb planetary inclinations in sizable ... See full document

5

Influence of stellar multiplicity on planet formation. II. Planets are less common in multiple-star systems with separations smaller than 1500 AU

Influence of stellar multiplicity on planet formation. II. Planets are less common in multiple-star systems with separations smaller than 1500 AU

... circumbinary orbits (P-type; Dvorak 1982), where the planet orbits both stars ...circumstellar orbits (S-type), where the planet orbits only one of the stars ...of planet ... See full document

16

Rotation and stellar evolution

Rotation and stellar evolution

... of rotation results in a widening of the main sequence with a significant increase of the stellar luminosity for the rotating model compared to the non-rotating ... See full document

10

A gap in the mass distribution for warm Neptune and terrestrial planets

A gap in the mass distribution for warm Neptune and terrestrial planets

... Our sample contains planets with masses measured through both RVs and TTVs. A key concern is whether the use of two methods is creating the appearance of two populations in the data. For the TTV characterized planets, ... See full document

6

An accurate mass determination for Kepler 1655b, a moderately irradiated world with a significant volatile envelope

An accurate mass determination for Kepler 1655b, a moderately irradiated world with a significant volatile envelope

... • The host star Kepler-1655 is a G0V Sun-like star with a rotation period of 13.6 ±1.4 days. The mag- netic activity behavior that we observe in both our photometric and spectroscopic time series are ... See full document

21

Kepler-1649b: an exo-Venus in the solar neighborhood

Kepler-1649b: an exo-Venus in the solar neighborhood

... Distinguishing between Earth and Venus analogs is becom- ing especially important as the ongoing K2 mission, like Kepler, discovers and studies more and more Earth-sized, near- habitable zone planets ( Demory et al. 2016 ... See full document

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