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Stars, Interstellar Medium and the Galaxy Commons™
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- Planetary systems (3)
- Astrobiology (1)
- Brown dwarfs (1)
- Convection (1)
- Infrared: planetary systems (1)
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- Methods: N-body simulations (1)
- Outflows (1)
- Planets and satellites: atmospheres (1)
- Planets and satellites: composition (1)
- Planets and satellites: fundamental parameters (1)
- Planets and satellites: general (1)
- Planets and satellites: individual: HAT-P-7 (1)
- Planet–star interactions (1)
- Stars: activity (1)
- Stars: individual (GJ 581) (1)
- Stars: individual (HD 40307) (1)
- Stars: interiors (1)
- Stars: low-mass (1)
- Stars: oscillations (including pulsations) (1)
- Stars: rotation (1)
- Stars: winds (1)
- Starspots Online-only material: color figures (1)
- Techniques: photometric (1)
- Turbulence (1)
Articles 1 - 6 of 6
Full-Text Articles in Stars, Interstellar Medium and the Galaxy
Infrared Eclipses Of The Strongly Irradiated Planet Wasp-33b, And Oscillations Of Its Host Star, Drake Deming, Jonathan D. Fraine, Pedro V. Sada, Nikku Madhusudhan, Heather A. Knutson, Joseph Harrington, Jasmina Blecic, Sarah Nymeyer, Alexis M.S. Smith, Brian Jackson
Infrared Eclipses Of The Strongly Irradiated Planet Wasp-33b, And Oscillations Of Its Host Star, Drake Deming, Jonathan D. Fraine, Pedro V. Sada, Nikku Madhusudhan, Heather A. Knutson, Joseph Harrington, Jasmina Blecic, Sarah Nymeyer, Alexis M.S. Smith, Brian Jackson
Brian Jackson
We observe two secondary eclipses of the strongly irradiated transiting planet WASP-33b, in the Ks band at 2.15 μm, and one secondary eclipse each at 3.6 μm and 4.5 μm using Warm Spitzer. This planet orbits an A5V δ-Scuti star that is known to exhibit low-amplitude non-radial p-mode oscillations at about 0.1% semi-amplitude. We detect stellar oscillations in all of our infrared eclipse data, and also in one night of observations at J band (1.25 μm) out of eclipse. The oscillation amplitude, in all infrared bands except Ks, is about the same as in the optical. However, the stellar oscillations …
The Evil-Mc Model For Ellipsoidal Variations Of Planet-Hosting Stars And Applications To The Hat-P-7 System, Brian K. Jackson, Nikole K. Lewis, Jason W. Barnes, L. Drake Deming, Adam P. Showman, Jonathan J. Fortney
The Evil-Mc Model For Ellipsoidal Variations Of Planet-Hosting Stars And Applications To The Hat-P-7 System, Brian K. Jackson, Nikole K. Lewis, Jason W. Barnes, L. Drake Deming, Adam P. Showman, Jonathan J. Fortney
Brian Jackson
We present a new model for Ellipsoidal Variations Induced by a Low-Mass Companion, the EVIL-MC model. We employ several approximations appropriate for planetary systems to substantially increase the computational efficiency of our model relative to more general ellipsoidal variation models and improve upon the accuracy of simpler models. This new approach gives us a unique ability to rapidly and accurately determine planetary system parameters. We use the EVIL-MC model to analyze Kepler Quarter 0-2 (Q0-2) observations of the HAT-P-7 system, an F-type star orbited by a ~ Jupiter-mass companion. Our analysis corroborates previous estimates of the planet-star mass ratio q …
Constraining Tidal Dissipation In Stars From The Destruction Rates Of Exoplanets, Kaloyan Penev, Brian Jackson, Federico Spada, Nicole Thom
Constraining Tidal Dissipation In Stars From The Destruction Rates Of Exoplanets, Kaloyan Penev, Brian Jackson, Federico Spada, Nicole Thom
Brian Jackson
We use the distribution of extrasolar planets in circular orbits around stars with surface convective zones detected by ground-based transit searches to constrain how efficiently tides raised by the planet are dissipated on the parent star. We parameterize this efficiency as a tidal quality factor (Q*). We conclude that the population of currently known planets is inconsistent with Q* < 107 at the 99% level. Previous studies show that values of Q* between 105 and 107 are required in order to explain the orbital circularization of main-sequence low-mass binary stars in clusters, suggesting that different dissipation mechanisms might be acting in the two cases, most likely due to the very different tidal forcing frequencies relative to the stellar rotation frequency occurring for star-star versus planet-star systems.
Kepler And Ground-Based Transits Of The Exo-Neptune Hat-P-11b, Drake Deming, Pedro V. Sada, Brian Jackson, Steven W. Peterson, Eric Agol, Heather A. Knutson, Donald E. Jennings, Flynn Haase, Kevin Bays
Kepler And Ground-Based Transits Of The Exo-Neptune Hat-P-11b, Drake Deming, Pedro V. Sada, Brian Jackson, Steven W. Peterson, Eric Agol, Heather A. Knutson, Donald E. Jennings, Flynn Haase, Kevin Bays
Brian Jackson
We analyze 26 archival Kepler transits of the exo-Neptune HAT-P-11b, supplemented by ground-based transits observed in the blue (B band) and near-IR (J band). Both the planet and host star are smaller than previously believed; our analysis yields Rp = 4.31 R⊕ ± 0.06 R ⊕ and Rs = 0.683 R☉ ± 0.009 R☉, both about 3σ smaller than the discovery values. Our ground-based transit data at wavelengths bracketing the Kepler bandpass serve to check the wavelength dependence of stellar limb darkening, and the J-band transit provides a precise and independent constraint on the transit duration. Both the limb darkening …
Tidal Limits To Planetary Habitability, Rory Barnes, Brian Jackson, Richard Greenberg, Sean N. Raymond
Tidal Limits To Planetary Habitability, Rory Barnes, Brian Jackson, Richard Greenberg, Sean N. Raymond
Brian Jackson
The habitable zones (HZs) of main-sequence stars have traditionally been defined as the range of orbits that intercept the appropriate amount of stellar flux to permit surface water on a planet. Terrestrial exoplanets discovered to orbit M stars in these zones, which are close-in due to decreased stellar luminosity, may also undergo significant tidal heating. Tidal heating may span a wide range for terrestrial exoplanets and may significantly affect conditions near the surface. For example, if heating rates on an exoplanet are near or greater than that on Io (where tides drive volcanism that resurfaces the planet at least every …
The Hd 40307 Planetary System: Super-Earths Or Mini-Neptunes?, Rory Barnes, Brian Jackson, Sean N. Raymond, Andrew A. West, Richard Greenberg
The Hd 40307 Planetary System: Super-Earths Or Mini-Neptunes?, Rory Barnes, Brian Jackson, Sean N. Raymond, Andrew A. West, Richard Greenberg
Brian Jackson
Three planets with minimum masses less than 10 M⊕ orbit the star HD 40307, suggesting these planets may be rocky. However, with only radial velocity data, it is impossible to determine if these planets are rocky or gaseous. Here we exploit various dynamical features of the system in order to assess the physical properties of the planets. Observations allow for circular orbits, but a numerical integration shows that the eccentricities must be at least 10–4. Also, planets b and c are so close to the star that tidal effects are significant. If planet b has tidal parameters similar to the …