THE ASTEROSEISMIC POTENTIAL OF
                    <i>KEPLER</i>
                    : FIRST RESULTS FOR SOLAR-TYPE STARS

Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; García, Rafael A.; Houdek, G.; Karoff, C.; Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Brown, Timothy M.; Christensen‐Dalsgaard, J.; Gilliland, Ronald L.; Kjeldsen, H.; Borucki, W. J.; Koch, David; Jenkins, Jon M.; Ballot, J.; Basu, Sarbani; Bazot, M.; Bedding, Timothy R.; Benomar, O.; Bonanno, A.; Brandão, I. M.; Bruntt, H.; Campante, Tiago L.; Creevey, O.; Mauro, M. P. Di; Doğan, G.; Dreizler, S.; Eggenberger, P.; Esch, Lisa; Fletcher, S.M.; Frandsen, S.; Gai, Ning; Gaulme, P.; Handberg, R.; Hekker, S.; Howe, R.; Huber, Daniel; Korzennik, S. G.; Lebrun, Jean-Claude; Leccia, S.; Martić, M.; Mathur, S.; Mosser, B.; New, R.; Quirion, Pierre-Olivier; Régulo, C.; Roxburgh, I. W.; Salabert, D.; Schou, J.; Sousa, S. G.; Stello, D.; Verner, G. A.; Arentoft, T.; Barban, C.; Belkacem, K.; Benatti, S.; Biazzo, K.; Boumier, P.; Bradley, P. A.; Broomhall, Anne-Marie; Buzasi, Derek L.; Claudi, R.; Cunha, M. S.; D’Antona, Francesca; Deheuvels, S.; Derekas, A.; Hernández, A. García; Giampapa, M. S.; Goupil, J. M.; Gruberbauer, M.; Guzik, Joyce A.; Hale, Steven J.; Ireland, Michael; Kiss, L. L.; Kitiashvili, Irina; Kolenberg, K.; Korhonen, H.; Kosovichev, A. G.; Kupka, F.; Lebreton, Y.; Leroy, B.; Ludwig, H.‐G.; Mathis, S.; Michel, E.; Miglio, A.; Montalbán, J.; Moya, A.; Noels, Alfred F.; Noyes, R. W.; Pallé, P. L.; Piau, L.; Preston, H. L.; Cortés, T. Roca; Roth, M.; Sato, Kumiko; Schmitt, J. H. M. M.; Serenelli, Aldo; Aguirre, V. Silva; Stevens, I. R.; Suárez, J. C.; Suran, M. D.; Trampedach, Regner; Turck‐Chièze, S.; Uytterhoeven, K.; Ventura, R.; Wilson, Paul

doi:10.1088/2041-8205/713/2/l169

Cited by 135 publications

(81 citation statements)

References 38 publications

(41 reference statements)

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“…Based on the Kepler experience with mode amplitudes as a function of stellar parameters, 22 TESS can be expected to detect p-mode oscillations on about 6000 stars brighter than V ¼ 7.5, including (a) the majority of all stars brighter than V ¼ 4. stars, and (d) virtually all the giant stars. Stars that are not suitable for planet searching but are appropriate for asteroseismology (such as giants) can be added to the TESS input catalog at minimal cost.…”

Section: Asteroseismologymentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,030

1,691

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Abstract. The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I C ≈ 4 − 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

show abstract

Section: Asteroseismologymentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,030

1,691

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show abstract

“…While the exoplanet yield has been wildly successful (e.g., Jenkins et al 2015), Kepler has been equally fruitful in studying the astrophysics of field stars. For the first time, asteroseismology with Kepler has provided information on the internal structure of stars besides our Sun, which places powerful constraints on their masses, radii, and ages (Chaplin et al 2010;Chaplin & Miglio 2013). Kepler 's precision light curves have also enabled stellar rotation to be characterized for tens of thousands of stars McQuillan et al 2014), shedding new light on angular momentum and dynamo evolution.…”

Section: Kepler Datamentioning

confidence: 99%

The Kepler Catalog of Stellar Flares

Davenport

2016

ApJ

312

423

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A homogeneous search for stellar flares has been performed using every available Kepler light curve. An iterative light curve de-trending approach was used to filter out both astrophysical and systematic variability to detect flares. The flare recovery completeness has also been computed throughout each light curve using artificial flare injection tests, and the tools for this work have been made publicly available. The final sample contains 851,168 candidate flare events recovered above the 68% completeness threshold, which were detected from 4041 stars, or 1.9% of the stars in the Kepler database. The average flare energy detected is ∼10 35 erg. The net fraction of flare stars increases with g−i color, or decreasing stellar mass. For stars in this sample with previously measured rotation periods, the total relative flare luminosity is compared to the Rossby number. A tentative detection of flare activity saturation for low-mass stars with rapid rotation below a Rossby number of ∼0.03 is found. A power-law decay in flare activity with Rossby number is found with a slope of −1, shallower than typical measurements for X-ray activity decay with Rossby number.

show abstract

“…Based on the Kepler experience with mode amplitudes as a function of stellar parameters, 21 TESS can be expected to detect p-mode oscillations on about 6,000 stars brighter than V = 7.5, including (a) the majority of all stars brighter than V = 4. than the Sun, (c) about 2,000 upper-main-sequence and subgiant stars, and (d) virtually all the giant stars. Stars that are not suitable for planet searching but are appropriate for asteroseismology (such as giants) can be added to the TESS input catalog at minimal cost.…”

Section: Asteroseismologymentioning

confidence: 99%

Transiting Exoplanet Survey Satellite (TESS)

Ricker

Winn²,

Vanderspek³

et al. 2014

SPIE Proceedings

746

288

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The Transiting Exoplanet Survey Satellite (TESS ) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its two-year mission, TESS will employ four wide-field optical CCD cameras to monitor at least 200,000 main-sequence dwarf stars with I C < ∼ 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from one month to one year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10-100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every four months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations.

show abstract

THE ASTEROSEISMIC POTENTIAL OF KEPLER : FIRST RESULTS FOR SOLAR-TYPE STARS

Cited by 135 publications

References 38 publications

Transiting Exoplanet Survey Satellite

Transiting Exoplanet Survey Satellite

The Kepler Catalog of Stellar Flares

Transiting Exoplanet Survey Satellite (TESS)

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