511 research outputs found

    The Photoeccentric Effect and Proto-hot Jupiters. III. A Paucity of Proto-hot Jupiters on Super-eccentric Orbits

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    Gas giant planets orbiting within 0.1 AU of their host stars are unlikely to have formed in situ and are evidence for planetary migration. It is debated whether the typical hot Jupiter smoothly migrated inward from its formation location through the proto-planetary disk, or was perturbed by another body onto a highly eccentric orbit, which tidal dissipation subsequently shrank and circularized during close stellar passages. Socrates and collaborators predicted that the latter model should produce a population of super-eccentric proto-hot Jupiters readily observable by Kepler. We find a paucity of such planets in the Kepler sample, which is inconsistent with the theoretical prediction with 96.9% confidence. Observational effects are unlikely to explain this discrepancy. We find that the fraction of hot Jupiters with an orbital period P > 3 days produced by the star-planet Kozai mechanism does not exceed (at two-sigma) 44%. Our results may indicate that disk migration is the dominant channel for producing hot Jupiters with P > 3 days. Alternatively, the typical hot Jupiter may have been perturbed to a high eccentricity by interactions with a planetary rather than stellar companion, and began tidal circularization much interior to 1 AU after multiple scatterings. A final alternative is that early in the tidal circularization process at high eccentricities tidal circularization occurs much more rapidly than later in the process at low eccentricities, although this is contrary to current tidal theories

    The Photoeccentric Effect and Proto-Hot Jupiters I. Measuring photometric eccentricities of individual transiting planets

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    Exoplanet orbital eccentricities offer valuable clues about the history of planetary systems. Eccentric, Jupiter-sized planets are particularly interesting: they may link the "cold" Jupiters beyond the ice line to close-in hot Jupiters, which are unlikely to have formed in situ. To date, eccentricities of individual transiting planets primarily come from radial velocity measurements. Kepler has discovered hundreds of transiting Jupiters spanning a range of periods, but the faintness of the host stars precludes radial velocity follow-up of most. Here we demonstrate a Bayesian method of measuring an individual planet's eccentricity solely from its transit light curve using prior knowledge of its host star's density. We show that eccentric Jupiters are readily identified by their short ingress/egress/total transit durations -- part of the "photoeccentric" light curve signature of a planet's eccentricity --- even with long-cadence Kepler photometry and loosely-constrained stellar parameters. A Markov Chain Monte Carlo exploration of parameter posteriors naturally marginalizes over the periapse angle and automatically accounts for the transit probability. To demonstrate, we use three published transit light curves of HD 17156 b to measure an eccentricity of e = 0.71 +0.16/-0.09, in good agreement with the discovery value e = 0.67+/-0.08 based on 33 radial-velocity measurements. We present two additional tests using actual Kepler data. In each case the technique proves to be a viable method of measuring exoplanet eccentricities and their confidence intervals. Finally, we argue that this method is the most efficient, effective means of identifying the extremely eccentric, proto hot Jupiters predicted by Socrates et al. (2012).Comment: ApJ, 756, 122. Received 2012 April 5; accepted 2012 July 9; published 2012 August 2

    Conclusion: Re-evaluating Eclecticism

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    When looking at the original data analysis, we see a variety of approaches used to examine the discourse data of focus. The analysis is rich and includes a wide array of features. Conversely, the three single perspective analyses conducted for this Forum each drew upon different linguistic details to support their conclusions with different insights

    A Pragmatics Perspective

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    In this conversation, a husband and wife discuss upcoming vacation plans (see Appendix A for the full transcript). It seems that the wife is guiding much of the conversation through attentiongetting phrases and by explicitly stating what she hopes the talk will accomplish. The husband, on the other hand, answers the wife and, at times, tries to add his opinion but is not able to get it out because the wife is talking over him or continues talking. Of the three excerpts we are focusing on (see Appendix B), the husband talks most in excerpt B, calculating expenses. There are instances of implicature (Grice, 1975), where one spouse understands unstated or implied meanings, and cases where one or both spouses are attending to negative or positive face needs (Brown & Levinson, 1987)

    A Counter Perspective

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    It was with great interest that I read the Stubbe, Lane, Hilder, Vine, Vine, Marra, Holmes, and Weatherall (2003) article analyzing workplace interaction. It demonstrated the varied ways the same material could be dissected and the diverse conclusions that could be drawn from approaches of conversation analysis, interactional sociolinguisitcs, politeness theory, critical discourse analysis, and discursive psychology. However, I found myself disagreeing with the general analyses made by the writers in all five approaches. It seems that, in looking to properly use linguistic, paralinguistic, and discourse features in ways championed by each approach, the analysts tailored their discussions to fit with the general assumptions and foci inherent to each style, and in consequence, to ignore the big picture (or what I term the common sense view that we, as social beings, have of an interaction from our general social knowledge)
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