The NASA Exoplanet Archive: Data and Tools for Exoplanet Research

Akeson, Rachel; Chen, Xi; Ciardi, David R.; Crane, Megan; Good, J. C.; Harbut, M.; Jackson, E. S.; Kane, Stephen R.; Laity, A. C.; Leifer, Stephanie; Lynn, Mary R.; McElroy, D. B.; Papin, M.; Plavchan, Peter; Ramírez, Solange; Rey, Raquel Oreiro; Braun, Kaspar von; Wittman, M.; Abajian, M.; Ali, B.; Beichman, Charles; Beekley, A.; Berriman, G. Bruce; Berukoff, S. J.; Bryden, G.; Chan, Ben; Groom, Steven L.; Lau, Chun‐Sean; Payne, A. N.; Regelson, Moira; Saucedo, M.; Schmitz, Marion; Stauffer, J.; Wyatt, P.; Zhang, A.

doi:10.1086/672273

Cited by 658 publications

(430 citation statements)

References 38 publications

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“…In addition to planet catalogs produced by the Kepler team, detailed planet validation has been performed by Lissauer et al (2012Lissauer et al ( , 2014 on mulit-planet systems, and on large samples (1000ʼs) of KOIs by Mullally et al (2015) and Morton et al (2016). The NASA Exoplanet Archive (Akeson et al 2013) hosts a cumulative list of dispositions for every KOI. All of these catalogs combined provide high-quality vetting of the Kepler planet candidate lists.…”

Section: False Positive Identificationmentioning

confidence: 99%

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

et al. 2017

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The California-Kepler Survey (CKS) is an observational program developed to improve our knowledge of the properties of stars found to host transiting planets by NASA's Kepler Mission. The improvement stems from new high-resolution optical spectra obtained using HIRES at the W. M. Keck Observatory. The CKS stellar sample comprises 1305 stars classified as Kepler objects of interest, hosting a total of 2075 transiting planets. The primary sample is magnitude-limited ( < Kp 14.2) and contains 960 stars with 1385 planets. The sample was extended to include some fainter stars that host multiple planets, ultra-short period planets, or habitable zone planets. The spectroscopic parameters were determined with two different codes, one based on template matching and the other on direct spectral synthesis using radiative transfer. We demonstrate a precision of 60K in T eff , 0.10dex in g log , 0.04dex in [ ] Fe H , and 1.0 -km s 1 in V i sin . In this paper, we describe the CKS project and present a uniform catalog of spectroscopic parameters. Subsequent papers in this series present catalogs of derived stellar properties such as mass, radius, and age; revised planet properties; and statistical explorations of the ensemble. CKS is the largest survey to determine the properties of Kepler stars using a uniform set of high-resolution, high signal-tonoise ratio spectra. The HIRES spectra are available to the community for independent analyses.

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Section: False Positive Identificationmentioning

confidence: 99%

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

et al. 2017

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“…In summary, we used the Lomb-Scargle (LS; Scargle 1982) approach as implemented by the NASA Exoplanet Archive Periodogram Service 12 (Akeson et al 2013). We looked for periods between 0.05 and 35 days, with the upper limit being set by roughly half the campaign length.…”

Section: Finding Periodsmentioning

confidence: 99%

Rotation of Late-type Stars in Praesepe with K2

Rebull

Stauffer

Hillenbrand

et al. 2017

ApJ

102

133

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We have Fourier-analyzed 941 K2 light curves (LCs) of likely members of Praesepe, measuring periods for 86% and increasing the number of rotation periods (P) by nearly a factor of four. The distribution of P versus -( ) V K s , a mass proxy, has three different regimes:, where the rotation rate rapidly slows as mass decreases; 1.3< -( ) V K s <4.5, where the rotation rate slows more gradually as mass decreases; andwhere the rotation rate rapidly increases as mass decreases. In this last regime, there is a bimodal distribution of periods, with few between ∼2 and ∼10 days. We interpret this to mean that once M stars start to slow down, they do so rapidly. The K2 period-color distribution in Praesepe (∼790 Myr) is much different than that in the Pleiades (∼125 Myr) for late F, G, K, and early-M stars; the overall distribution moves to longer periods and is better described by two line segments. For mid-M stars, the relationship has a similarly broad scatter and is steeper in Praesepe. The diversity of LCs and of periodogram types is similar in the two clusters; about a quarter of the periodic stars in both clusters have multiple significant periods. Multi-periodic stars dominate among the higher masses, starting at a bluer color in Praesepe ( -( ) V K s ∼1.5) than in the Pleiades ( -( ) V K s ∼2.6). In Praesepe, there are relatively more LCs that have two widely separated periods, D > P 6 days. Some of these could be examples of M star binaries where one star has spun down but the other has not.

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“…For Jupiter mass planets, Reiners & Christensen (2010) predict that the magnetic field will be similar to the Jovian values (about 10G in the polar regions). The data is taken from exoplanet.eu (Schneider et al 2011), and the NASA exoplanet archive (Akeson et al 2013). We only chose exoplanets whose relative radius and mass uncertainties are below 50%.…”

Section: Introductionmentioning

confidence: 99%

Estimating the Magnetic Field Strength in Hot Jupiters

Yadav

Thorngren

2017

ApJL

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A large fraction of known Jupiter like exoplanets are inflated as compared to Jupiter. These "hot" Jupiters orbit close to their parent star and are bombarded with intense starlight. Many theories have been proposed to explain their radius inflation and several suggest that a small fraction of the incident starlight is injected in to the planetary interior which helps to puff up the planet. How will such energy injection affect the planetary dynamo? In this Letter, we estimate the surface magnetic field strength of hot Jupiters using scaling arguments that relate energy available in planetary interiors to the dynamo generated magnetic fields. We find that if we take into account the energy injected in the planetary interior that is sufficient to inflate hot Jupiters to observed radii, then the resulting dynamo should be able generate magnetic fields that are more than an order of magnitude stronger than the Jovian values. Our analysis highlights the potential fundamental role of the stellar light in setting the field strength in hot Jupiters.

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The NASA Exoplanet Archive: Data and Tools for Exoplanet Research

Cited by 658 publications

References 38 publications

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

Rotation of Late-type Stars in Praesepe with K2

Estimating the Magnetic Field Strength in Hot Jupiters

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The NASA Exoplanet Archive: Data and Tools for Exoplanet Research

Cited by 658 publications

References 38 publications

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets*

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets*

Rotation of Late-type Stars in Praesepe with K2

Estimating the Magnetic Field Strength in Hot Jupiters

Contact Info

Product

Resources

About

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*