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Andrew W Howard - One of the best experts on this subject based on the ideXlab platform.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    The Astrophysical Journal, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75 M ☉ and effective temperatures of 3900-4800 K). We analyzed four years of Doppler radial velocity (RVs) data for 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0% ± 2.3% of these stars have Saturn-mass or larger planets with orbital periods <245 days, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7% ± 0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs, and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g., a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    arXiv: Earth and Planetary Astrophysics, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75Msun and effective temperatures of 3900-4800K). We analyzed four years of Doppler radial velocities data of 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0+/-2.3% of these stars have Saturn-mass or larger planets with orbital periods <245d, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7+/-0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g. a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

Eric Gaidos - One of the best experts on this subject based on the ideXlab platform.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    The Astrophysical Journal, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75 M ☉ and effective temperatures of 3900-4800 K). We analyzed four years of Doppler radial velocity (RVs) data for 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0% ± 2.3% of these stars have Saturn-mass or larger planets with orbital periods <245 days, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7% ± 0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs, and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g., a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    arXiv: Earth and Planetary Astrophysics, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75Msun and effective temperatures of 3900-4800K). We analyzed four years of Doppler radial velocities data of 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0+/-2.3% of these stars have Saturn-mass or larger planets with orbital periods <245d, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7+/-0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g. a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

Andrew W Mann - One of the best experts on this subject based on the ideXlab platform.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    The Astrophysical Journal, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75 M ☉ and effective temperatures of 3900-4800 K). We analyzed four years of Doppler radial velocity (RVs) data for 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0% ± 2.3% of these stars have Saturn-mass or larger planets with orbital periods <245 days, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7% ± 0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs, and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g., a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    arXiv: Earth and Planetary Astrophysics, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75Msun and effective temperatures of 3900-4800K). We analyzed four years of Doppler radial velocities data of 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0+/-2.3% of these stars have Saturn-mass or larger planets with orbital periods <245d, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7+/-0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g. a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

Debra A Fischer - One of the best experts on this subject based on the ideXlab platform.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    The Astrophysical Journal, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75 M ☉ and effective temperatures of 3900-4800 K). We analyzed four years of Doppler radial velocity (RVs) data for 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0% ± 2.3% of these stars have Saturn-mass or larger planets with orbital periods <245 days, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7% ± 0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs, and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g., a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

  • an understanding of the shoulder of giants jovian planets around late k dwarf stars and the trend with stellar mass
    arXiv: Earth and Planetary Astrophysics, 2013
    Co-Authors: Eric Gaidos, Debra A Fischer, Andrew W Mann, Andrew W Howard
    Abstract:

    Analyses of exoplanet statistics suggest a trend of giant planet occurrence with host star mass, a clue to how planets like Jupiter form. One missing piece of the puzzle is the occurrence around late K dwarf stars (masses of 0.5-0.75Msun and effective temperatures of 3900-4800K). We analyzed four years of Doppler radial velocities data of 110 late K dwarfs, one of which hosts two previously reported giant planets. We estimate that 4.0+/-2.3% of these stars have Saturn-mass or larger planets with orbital periods <245d, depending on the planet mass distribution and RV variability of stars without giant planets. We also estimate that 0.7+/-0.5% of similar stars observed by Kepler have giant planets. This Kepler rate is significantly (99% confidence) lower than that derived from our Doppler survey, but the difference vanishes if only the single Doppler system (HIP 57274) with completely resolved orbits is considered. The difference could also be explained by the exclusion of close binaries (without giant planets) from the Doppler but not Kepler surveys, the effect of long-period companions and stellar noise on the Doppler data, or an intrinsic difference between the two populations. Our estimates for late K dwarfs bridge those for solar-type stars and M dwarfs and support a positive trend with stellar mass. Small sample size precludes statements about Finer Structure, e.g. a "shoulder" in the distribution of giant planets with stellar mass. Future surveys such as the Next Generation Transit Survey and the Transiting Exoplanet Satellite Survey will ameliorate this deficiency.

Saadé Joelle - One of the best experts on this subject based on the ideXlab platform.

  • Symbolic methods for linear differential systems with irregular singularity
    2019
    Co-Authors: Saadé Joelle
    Abstract:

    Cette thèse est consacrée aux méthodes symboliques de résolution locale des systèmes différentiels linéaires à coefficients dans K = C((x)), le corps des séries de Laurent, sur un corps effectif C. Plus précisément, nous nous intéressons aux algorithmes effectifs de réduction formelle. Au cours de la réduction, nous sommes amenés à introduire des extensions algébriques du corps de coefficients K (extensions algébriques de C, ramifications de la variable x) afin d’obtenir une Structure plus fine. Du point de vue algorithmique, il est préférable de retarder autant que possible l’introduction de ces extensions. Dans ce but, nous développons un nouvel algorithme de réduction formelle qui utilise l’anneau des endomorphismes du système, appelé « eigenring », afin de se ramener au cas d’un système indécomposable sur K. En utilisant la classification formelle donnée par Balser-Jurkat-Lutz, nous déduisons la Structure de l’eigenring d’un système indécomposable. Ces résultats théoriques nous permettent de construire une décomposition sur le corps de base K qui sépare les différentes parties exponentielles du système et permet ainsi d’isoler dans des sous-systèmes, indécomposables sur K, les différentes extensions de corps qui peuvent apparaître afin de les traiter séparément. Dans une deuxième partie, nous nous intéressons à l’algorithme de Miyake pour la réduction formelle. Celle-ci est basée sur le calcul du poids et d’une suite de Volevic de la matrice de valuation du système. Nous donnons des interprétations en théorie de graphe et en algèbre tropicale du poids et suites de Volevic, et obtenons ainsi des méthodes de calculs efficaces sur le plan pratique, à l’aide de la programmation linéaire. Ceci complète une étape fondamentale dans l’algorithme de réduction de Miyake. Ces différents algorithmes sont implémentés sous forme de librairies pour le logiciel de calcul formel Maple. Enfin, nous présentons une discussion sur la performance de l’algorithme de réduction avec l’eigenring ainsi qu’une comparaison en terme de temps de calcul entre notre implémentation de l’algorithme de réduction de Miyake par la programmation linéaire et ceux de Barkatou et Pflügel.This thesis is devoted to symbolic methods for local resolution of linear differential systems with coefficients in K = C((x)), the field of Laurent series, on an effective field C. More specifically, we are interested in effective algorithms for formal reduction. During the reduction, we are led to introduce algebraic extensions of the field of coefficients K (algebraic extensions of C, ramification of the variable x) in order to obtain a Finer Structure. From an algorithmic point of view, it is preferable to delay as much as possible the introduction of these extensions. To this end, we developed a new algorithm for formal reduction that uses the ring of endomorphisms of the system, called "eigenring". Using the formal classification given by Balser-Jurkat-Lutz, we deduce the Structure of the eigenring of an indecomposable system. These theoretical results allow us to construct a decomposition on the base field K that separates the different exponential parts of the system and thus allows us to isolate, in indecomposable subsystems in K, the different algebraic extensions that can appear in order to treat them separately. In a second part, we are interested in Miyake’s algorithm for formal reduction. This algorithm is based on the computation of the Volevic weight and numbers of the valuation matrix of the system. We provide interpretations in graph theory and tropical algebra of the Volevic weight and numbers, and thus obtain practically efficient methods using linear programming. This completes a fundamental step in the Miyake reduction algorithm. These different algorithms are implemented as libraries for the computer algebra software Maple. Finally, we present a discussion on the performance of the reduction algorithm using the eigenring as well as a comparison in terms of timing between our implementation of Miyake’s reduction algorithm by linear programming and the algorithms of Barkatou and Pflügel

  • Méthodes symboliques pour les systèmesdifférentiels linéaires à singularité irrégulière
    HAL CCSD, 2019
    Co-Authors: Saadé Joelle
    Abstract:

    This thesis is devoted to symbolic methods for local resolution of linear differential systems with coefficients in K = C((x)), the field of Laurent series, on an effective field C. More specifically, we are interested in effective algorithms for formal reduction. During the reduction, we are led to introduce algebraic extensions of the field of coefficients K (algebraic extensions of C, ramification of the variable x) in order to obtain a Finer Structure. From an algorithmic point of view, it is preferable to delay as much as possible the introduction of these extensions. To this end, we developed a new algorithm for formal reduction that uses the ring of endomorphisms of the system, called "eigenring". Using the formal classification given by Balser-Jurkat-Lutz, we deduce the Structure of the eigenring of an indecomposable system. These theoretical results allow us to construct a decomposition on the base field K that separates the different exponential parts of the system and thus allows us to isolate, in indecomposable subsystems in K, the different algebraic extensions that can appear in order to treat them separately. In a second part, we are interested in Miyake’s algorithm for formal reduction. This algorithm is based on the computation of the Volevic weight and numbers of the valuation matrix of the system. We provide interpretations in graph theory and tropical algebra of the Volevic weight and numbers, and thus obtain practically efficient methods using linear programming. This completes a fundamental step in the Miyake reduction algorithm. These different algorithms are implemented as libraries for the computer algebra software Maple. Finally, we present a discussion on the performance of the reduction algorithm using the eigenring as well as a comparison in terms of timing between our implementation of Miyake’s reduction algorithm by linear programming and the algorithms of Barkatou and Pflügel.Cette thèse est consacrée aux méthodes symboliques de résolution locale des systèmes différentiels linéaires à coefficients dans K = C((x)), le corps des séries de Laurent, sur un corps effectif C. Plus précisément, nous nous intéressons aux algorithmes effectifs de réduction formelle. Au cours de la réduction, nous sommes amenés à introduire des extensions algébriques du corps de coefficients K (extensions algébriques de C, ramifications de la variable x) afin d’obtenir une Structure plus fine. Du point de vue algorithmique, il est préférable de retarder autant que possible l’introduction de ces extensions. Dans ce but, nous développons un nouvel algorithme de réduction formelle qui utilise l’anneau des endomorphismes du système, appelé « eigenring », afin de se ramener au cas d’un système indécomposable sur K. En utilisant la classification formelle donnée par Balser-Jurkat-Lutz, nous déduisons la Structure de l’eigenring d’un système indécomposable. Ces résultats théoriques nous permettent de construire une décomposition sur le corps de base K qui sépare les différentes parties exponentielles du système et permet ainsi d’isoler dans des sous-systèmes, indécomposables sur K, les différentes extensions de corps qui peuvent apparaître afin de les traiter séparément. Dans une deuxième partie, nous nous intéressons à l’algorithme de Miyake pour la réduction formelle. Celle-ci est basée sur le calcul du poids et d’une suite de Volevic de la matrice de valuation du système. Nous donnons des interprétations en théorie de graphe et en algèbre tropicale du poids et suites de Volevic, et obtenons ainsi des méthodes de calculs efficaces sur le plan pratique, à l’aide de la programmation linéaire. Ceci complète une étape fondamentale dans l’algorithme de réduction de Miyake. Ces différents algorithmes sont implémentés sous forme de librairies pour le logiciel de calcul formel Maple. Enfin, nous présentons une discussion sur la performance de l’algorithme de réduction avec l’eigenring ainsi qu’une comparaison en terme de temps de calcul entre notre implémentation de l’algorithme de réduction de Miyake par la programmation linéaire et ceux de Barkatou et Pflügel

  • Méthodes symboliques pour les systèmes différentiels linéaires à singularité irrégulière
    HAL CCSD, 2019
    Co-Authors: Saadé Joelle
    Abstract:

    This thesis is devoted to symbolic methods for local resolution of linear differential systems with coefficients in K = C((x)), the field of Laurent series, on an effective field C. More specifically, we are interested in effective algorithms for formal reduction. During the reduction, we are led to introduce algebraic extensions of the field of coefficients K (algebraic extensions of C, ramification of the variable x) in order to obtain a Finer Structure. From an algorithmic point of view, it is preferable to delay as much as possible the introduction of these extensions. To this end, we developed a new algorithm for formal reduction that uses the ring of endomorphisms of the system, called "eigenring". Using the formal classification given by Balser-Jurkat-Lutz, we deduce the Structure of the eigenring of an indecomposable system. These theoretical results allow us to construct a decomposition on the base field K that separates the different exponential parts of the system and thus allows us to isolate, in indecomposable subsystems in K, the different algebraic extensions that can appear in order to treat them separately. In a second part, we are interested in Miyake’s algorithm for formal reduction. This algorithm is based on the computation of the Volevic weight and numbers of the valuation matrix of the system. We provide interpretations in graph theory and tropical algebra of the Volevic weight and numbers, and thus obtain practically efficient methods using linear programming. This completes a fundamental step in the Miyake reduction algorithm. These different algorithms are implemented as libraries for the computer algebra software Maple. Finally, we present a discussion on the performance of the reduction algorithm using the eigenring as well as a comparison in terms of timing between our implementation of Miyake’s reduction algorithm by linear programming and the algorithms of Barkatou and Pflügel.Cette thèse est consacrée aux méthodes symboliques de résolution locale des systèmes différentiels linéaires à coefficients dans K = C((x)), le corps des séries de Laurent, sur un corps effectif C. Plus précisément, nous nous intéressons aux algorithmes effectifs de réduction formelle. Au cours de la réduction, nous sommes amenés à introduire des extensions algébriques du corps de coefficients K (extensions algébriques de C, ramifications de la variable x) afin d’obtenir une Structure plus fine. Du point de vue algorithmique, il est préférable de retarder autant que possible l’introduction de ces extensions. Dans ce but, nous développons un nouvel algorithme de réduction formelle qui utilise l’anneau des endomorphismes du système, appelé « eigenring », afin de se ramener au cas d’un système indécomposable sur K. En utilisant la classification formelle donnée par Balser-Jurkat-Lutz, nous déduisons la Structure de l’eigenring d’un système indécomposable. Ces résultats théoriques nous permettent de construire une décomposition sur le corps de base K qui sépare les différentes parties exponentielles du système et permet ainsi d’isoler dans des sous-systèmes, indécomposables sur K, les différentes extensions de corps qui peuvent apparaître afin de les traiter séparément. Dans une deuxième partie, nous nous intéressons à l’algorithme de Miyake pour la réduction formelle. Celle-ci est basée sur le calcul du poids et d’une suite de Volevic de la matrice de valuation du système. Nous donnons des interprétations en théorie de graphe et en algèbre tropicale du poids et suites de Volevic, et obtenons ainsi des méthodes de calculs efficaces sur le plan pratique, à l’aide de la programmation linéaire. Ceci complète une étape fondamentale dans l’algorithme de réduction de Miyake. Ces différents algorithmes sont implémentés sous forme de librairies pour le logiciel de calcul formel Maple. Enfin, nous présentons une discussion sur la performance de l’algorithme de réduction avec l’eigenring ainsi qu’une comparaison en terme de temps de calcul entre notre implémentation de l’algorithme de réduction de Miyake par la programmation linéaire et ceux de Barkatou et Pflügel