Solar-stellar connection: the frequency of maximum oscillation power from solar data

Barban, C.; Beuret, M.; Baudin, F.; Belkacem, K.; Goupil, M. J.; Samadi, R.

doi:10.1088/1742-6596/440/1/012031

Cited by 5 publications

(6 citation statements)

References 3 publications

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“…This can be explained by the fact that the error bar on ν max given by Ballot et al is an internal error that is quite small (1 per cent). As shown by Barban et al (2013), the method adopted to infer ν max from the power spectra affects its value. Furthermore, one can expect differences between the observational value of ν max and the theoretical value, which obeys the scaling relation (e.g.…”

Section: Observational Constraints Restitutionmentioning

confidence: 99%

Asteroseismology for “à la carte” stellar age-dating and weighing

Lebreton

Goupil

2014

A&A

160

168

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Context. In the context of the space missions CoRoT, Kepler, Gaia, TESS, and PLATO, precise and accurate stellar ages, masses, and radii are of paramount importance. For instance, they are crucial for constraining scenarii of planetary formation and evolution. Aims. We aim at quantifying how detailed stellar modelling can improve the accuracy and precision on age and mass of individual stars. To that end, we adopt a multifaceted approach where we carefully examine how the number of observational constraints as well as the uncertainties on observations and on model input physics affect the results of age-dating and weighing. Methods. We modelled in detail the exoplanet host-star HD 52265, a main-sequence, solar-like oscillator that CoRoT observed for four months. We considered different sets of observational constraints (Hertzsprung-Russell data, metallicity, various sets of seismic constraints). For each case, we determined the age, mass, and properties of HD 52265 inferred from stellar models, and we quantified the impact of the model input physics and free parameters. We also compared model ages with ages derived by empirical methods or Hertzsprung-Russell diagram inversion. Results. For our case study HD 52265, our seismic analysis provides an age A = 2.10−2.54 Gyr, a mass M = 1.14−1.32 M , and a radius R = 1.30−1.34 R , which corresponds to age, mass, and radius uncertainties of ∼10, ∼7, and ∼1.5 per cent, respectively. These uncertainties account for observational errors and current state-of-the-art stellar model uncertainties. Our seismic study also provides constraints on surface convection properties through the mixing-length, which we find to be 12−15 per cent lower than the solar value. On the other hand, because of helium-mass degeneracy, the initial helium abundance is determined modulo the mass value. Finally, we evaluate the seismic mass of the exoplanet to be M p sin i = 1.17−1.26 M Jupiter , much more precise than what can be derived by Hertzsprung-Russell diagram inversion. Conclusions. We demonstrate that asteroseismology allows us to substantially improve the age accuracy that can be achieved with other methods. We emphasize that the knowledge of the mean properties of stellar oscillations -such as the large frequency separation -is not enough to derive accurate ages. We need precise individual frequencies to narrow the age scatter that is a result of the model input physics uncertainties. Further progress is required to better constrain the physics at work in stars and the stars helium content. Our results emphasize the importance of precise classical stellar parameters and oscillation frequencies such as will be obtained by the Gaia and PLATO missions.

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Section: Observational Constraints Restitutionmentioning

confidence: 99%

Asteroseismology for “à la carte” stellar age-dating and weighing

Lebreton

Goupil

2014

A&A

160

168

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“…Our adopted stellar mass and radius for HD 42618 are based on the relations of Torres et al (2010) using our spectroscopic constraints on T eff , log g, and [Fe/H]. HD 42618 was also target of the CoRoT mission (Baglin et al 2009), with a preliminary detection of solar-like oscillations presented by Barban et al (2013). We performed an independent asteroseismic analysis of the CoRoT photometry (see Section 5.1.1), which yielded a mass and radius in agreement with our adopted values.…”

Section: Stellar Propertiesmentioning

confidence: 99%

Three Temperate Neptunes Orbiting Nearby Stars*

Fulton

Howard

Weiss

et al. 2016

ApJ

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We present the discovery of three modestly irradiated, roughly Neptune-mass planets orbiting three nearby Solartype stars. HD 42618 b has a minimum mass of 15.4±2.4 Å M , a semimajor axis of 0.55 au, an equilibrium temperature of 337 K, and is the first planet discovered to orbit the solar analogue host star, HD 42618. We also discover new planets orbiting the known exoplanet host stars HD 164922 and HD 143761 (ρ CrB). The new planet orbiting HD 164922 has a minimum mass of 12.9±1.6 Å M and orbits interior to the previously known Jovian mass planet orbiting at 2.1 au. HD 164922 c has a semimajor axis of 0.34 au and an equilibrium temperature of 418 K. HD 143761 c orbits with a semimajor axis of 0.44 au, has a minimum mass of 25±2 Å M , and is the warmest of the three new planets with an equilibrium temperature of 445 K. It orbits exterior to the previously known warm Jupiter in the system. A transit search using space-based CoRoT data and ground-based photometry from the Automated Photometric Telescopes (APTs) at Fairborn Observatory failed to detect any transits, but the precise, high-cadence APT photometry helped to disentangle planetary-reflex motion from stellar activity. These planets were discovered as part of an ongoing radial velocity survey of bright, nearby, chromospherically inactive stars using the Automated Planet Finder (APF) telescope at Lick Observatory. The high-cadence APF data combined with nearly two decades of radial velocity data from Keck Observatory and gives unprecedented sensitivity to both short-period low-mass, and long-period intermediate-mass planets.

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“…Using the masses, effective temperatures, and radii of Kepler M-star targets as determined by Dressing & Charbonneau (2013), as well as ν max, 3140 µHz (Barban et al 2013), this relation yields ν max values in the range 6.4 -31.6 mHz, corresponding to periods between 0.5 and 2.6 minutes. This is at least a factor of 80 shorter than the shortest period in our stellar sample.…”

Section: Periodicitiesmentioning

confidence: 99%

M-Dwarf Rapid Rotators and the Detection of Relatively Young Multiple M-Star Systems

Rappaport

Swift

Levine

et al. 2014

ApJ

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We have searched the Kepler light curves of ∼ 3900 M-star targets for evidence of periodicities that indicate, by means of the effects of starspots, rapid stellar rotation. Several analysis techniques, including Fourier transforms, inspection of folded light curves, 'sonograms', and phase tracking of individual modulation cycles, were applied in order to distinguish the periodicities due to rapid rotation from those due to stellar pulsations, eclipsing binaries, or transiting planets. We find 178 Kepler M-star targets with rotation periods, P rot , of < 2 days, and 110 with P rot < 1 day. Some 30 of the 178 systems exhibit two or more independent short periods within the same Kepler photometric aperture, while several have three or more short periods. Adaptive optics imaging and modeling of the Kepler pixel response function for a subset of our sample support the conclusion that the targets with multiple periods are highly likely to be relatively young physical binary, triple, and even quadruple M star systems. We explore in detail the one object with four incommensurate periods all less than 1.2 days, and show that two of the periods arise from one of a close pair of stars, while the other two arise from the second star, which itself is probably a visual binary. If most of these M-star systems with multiple periods turn out to be bound M stars, this could prove a valuable way of discovering young hierarchical M-star systems; the same approach may also be applicable to G and K stars. The ∼5% occurrence rate of rapid rotation among the ∼ 3900 M star targets is consistent with spin evolution models that include an initial contraction phase followed by magnetic braking, wherein a typical M star can spend several hundred Myr before spinning down to periods longer than 2 days.

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Solar-stellar connection: the frequency of maximum oscillation power from solar data

Cited by 5 publications

References 3 publications

Asteroseismology for “à la carte” stellar age-dating and weighing

Asteroseismology for “à la carte” stellar age-dating and weighing

Three Temperate Neptunes Orbiting Nearby Stars*

M-Dwarf Rapid Rotators and the Detection of Relatively Young Multiple M-Star Systems

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