Magnetic variability in the young solar analog KIC 10644253

Salabert, D.; Régulo, C.; García, R. A.; Beck, P. G.; Ballot, J.; Creevey, O.; Hernández, F. Pérez; Nascimento, J. D. do; Corsaro, E.; Egeland, Ricky; Mathur, S.; Metcalfe, T. S.; Bigot, Lionel; Ceillier, T.; Pallé, P. L.

doi:10.1051/0004-6361/201527978

Cited by 54 publications

(102 citation statements)

References 93 publications

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“…During maximum activity the amplitudes of the modes decrease while the frequencies increase. This has been observed on the Sun and a few solar-like stars targeted by CoRoT and Kepler (e.g., [11,12] …”

Section: Analyzing Photometric Datamentioning

confidence: 71%

Rotation and magnetic activity of oscillating solar-like stars with the Kepler mission

et al. 2017

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Abstract. For the last few decades the investigation of stellar magnetic activity has been conducted through spectroscopic and spectropolarimetric surveys. This led not only to the detection of magnetic cycles in other stars but also to variable and magnetic activity. For the Sun, the magnetic activity is described as the interaction between convection, rotation, and magnetic field. To study magnetic activity of solar-like stars we need to have the knowledge of the surface rotation period, the properties of magnetic activity, and the structure of the stars. We present the results obtained from the studies of Kepler solarlike targets in terms of rotation periods, magnetic activity proxies and magnetic activity cycles detected. We can then combine this information with asteroseismic studies to have a broader picture of stellar magnetic activity.

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Section: Analyzing Photometric Datamentioning

confidence: 71%

Rotation and magnetic activity of oscillating solar-like stars with the Kepler mission

et al. 2017

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“…This star is a particularly interesting target as it is the youngest G-type star within the solar-like oscillators observed by Kepler [5,9]. Furthermore, it exhibits temporal variations of the oscillation frequencies associated to its magnetic variability [16]. Such temporal variability of the acoustic oscillation parameters are well studied in the case of the Sun over to date two 11-year solar cycles [see e.g., 17, and references therein], but has been observed so far in only three stars: the F-type stars HD 49933 [18,19] and KIC 3733735 [20], and the solar-analog G-type star KIC 10644253 [13].…”

Section: Background Parametersmentioning

confidence: 99%

Effect ofKeplercalibration on global seismic and background parameters

Salabert¹,

García²,

Mathur

et al. 2017

EPJ Web Conf.

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Abstract. Calibration issues associated to scrambled collateral smear affecting the Kepler short-cadence data were discovered in the Data Release 24 and were found to be present in all the previous data releases since launch. In consequence, a new Data Release 25 was reprocessed to correct for these problems. We perform here a preliminary study to evaluate the impact on the extracted global seismic and background parameters between data releases. We analyze the sample of seismic solar analogs observed by Kepler in short cadence between Q5 and Q17. We start with this set of stars as it constitutes the best sample to put the Sun into context along its evolution, and any significant differences on the seismic and background parameters need to be investigated before any further studies of this sample can take place. We use the A2Z pipeline to derive both global seismic parameters and background parameters from the Data Release 25 and previous data releases and report on the measured differences.

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“…An updated version of a diagram published in [12] is shown in Figure 1, using data from [13]. More recent data have been added from [14][15][16][17][18][19][20]. All of the slower rotators (P rot > 30 days) are K-type stars, which is now understandable -magnetic braking ceases in more massive main-sequence stars before they reach these long rotation periods.…”

Section: Motivationmentioning

confidence: 99%

The impact of Gaia DR1 on asteroseismic inferences from Kepler

Metcalfe

Creevey

Saders³

2017

EPJ Web Conf.

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Abstract. The Kepler mission has been fantastic for asteroseismology of solar-type stars, but the targets are typically quite distant. As a consequence, the reliability of asteroseismic modeling has been limited by the precision of additional constraints from highresolution spectroscopy and parallax measurements. A precise luminosity is particularly useful to minimize potential biases due to the intrinsic correlation between stellar mass and initial helium abundance. We have applied the latest version of the Asteroseismic Modeling Portal (AMP) to the complete Kepler data sets for 30 stars with known rotation rates and chromospheric activity levels. We compare the stellar properties derived with and without the measured parallaxes from the first data release of Gaia. We find that in most cases the masses and ages inferred from asteroseismology shift within their uncertainties. For a few targets that show larger shifts, the updated stellar properties only strengthen previous conclusions about anomalous rotation in middle-aged stars. MotivationThe correlation between stellar mass and initial helium abundance is a long-standing problem in modeling solar-type stars. Increasing either the mass or the initial helium yields a model with a higher luminosity, so we can trade off one parameter for the other while still satisfying the observational constraints ([1]). Asteroseismic observations can reduce the severity of this problem by providing a strong constraint on the stellar radius, but the issue cannot be avoided entirely without a more direct constraint on the stellar luminosity. Without such a constraint, the correlation can lead to systematic biases in the stellar properties inferred from asteroseismology. In this paper, we examine the impact of including luminosity constraints derived from Gaia DR1 parallaxes ([2]) for a sample of 30 Kepler targets with known rotation rates ([3]) and chromospheric activity levels ([4]). Our goal is to evaluate the possibility of systematic biases in the asteroseismic masses and ages for stars with anomalous rotation compared to empirical gyrochronology relations ([5]), with implications for a new theory of magnetic evolution beyond middle age ([6]).Until recently, it was presumed that rotation and magnetism decay together throughout the lives of solar-type stars ([7, 8]). Although stars are formed with a range of initial rotation rates, the stellar winds entrained in their magnetic fields lead to angular momentum loss from magnetic braking. This forces convergence to a single rotation rate at a given mass after roughly 500 Myr. The Kepler mission allowed the measurement of rotation periods in old field stars whose masses and ages could be determined from asteroseismology. These new data revealed a population of field stars rotating

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Magnetic variability in the young solar analog KIC 10644253

Cited by 54 publications

References 93 publications

Rotation and magnetic activity of oscillating solar-like stars with the Kepler mission

Rotation and magnetic activity of oscillating solar-like stars with the Kepler mission

Effect ofKeplercalibration on global seismic and background parameters

The impact of Gaia DR1 on asteroseismic inferences from Kepler

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