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Dzmitry Shvaiba - One of the best experts on this subject based on the ideXlab platform.
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socio economic security of the Hierarchical System
Social Science Research Network, 2018Co-Authors: Dzmitry ShvaibaAbstract:The paradox of financial and economic reality lies in the fact that it coexists and phenomena of financial evolution, and processes of conventional (non-transient) type. On the one hand, the economy is changing technologies, goods, organizations and structures. In this sense, it is evolutionary. On the other hand, the acts of these shifts do not exhaust the essence of financial and economic functioning. The huge role is played by the moments of economic strength of financial entities, coordination of costs and results, demand and supply, anti-crisis formation. The study of these moments is the prerogative of classical science. This means that science as a whole is not able to refute the classical approaches and absolutize fresh, non-traditional views (synergetic, evolutionary) on the concept or Vice versa. The synthesis of classical and fresh non-standard financial and economic doctrines is necessary.
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structural stability and socio economic security of the Hierarchical System
Social Science Research Network, 2018Co-Authors: Dzmitry ShvaibaAbstract:The financial and economic macro-System mixes different Hierarchical structures: functional, sectoral, territorial. Its Hierarchical structure has the ability to be different from the Hierarchical structure of the organization - the micro level segment. Socio - economic security of the highest value of the hierarchy is an array of criteria and points that ensure the freedom of the country's economy, its strength and stability, the capacity for constant renewal and self-improvement. Socio - economic security of any country is an important high-quality feature of the financial and economic System of the state, which determines its ability to maintain the normal circumstances of life of the population, to ensure the provision of resources for the establishment of the economy, and, in addition, to ensure the national and state interests. Social and economic security guarantees stable financial and economic growth, sufficient provision of social needs, effective management, protection of financial and economic interests at the state and global levels. Socio-economic security of the lowest value of the hierarchy (enterprise) - a provision of its security from the adverse effects of external and internal hazards, destabilizing moments, which guarantees the stable implementation of financial and economic interests and goals of the work.
Leslie Hebb - One of the best experts on this subject based on the ideXlab platform.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
The Astrophysical Journal, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis ɑ = 0.370^(+0.007)_(-0.006) AU with a large eccentricity (e = 0.85^(+0.08)_(-0.07)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 ± 0.002), Hierarchically separated (a = 1.68 ± 0.03 AU) giant planet (7.3 ± 0.4 M J_(up)). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 ± 0.3 M J_(up) and confirm its photometrically measured eccentricity, refining the value to e = 0.83 ± 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9^(+8)_(-6) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370 +0.007/-0.006 AU with a large eccentricity e=0.85 +0.08/-0.07 measured via the "photoeccentric effect." It exhibits transit timing variations induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e=0.184 +/- 0.002), Hierarchically-separated (a=1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 MJup). We combine sixteen quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer (HIRES) on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of inner planet to be 2.5+/-0.3MJup and confirm its photometrically-measured eccentricity, refining the value to e=0.83+/-0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that, despite their sizable eccentricities, the planets are coplanar to within 9 +8/-6 degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1m-class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
Rebekah I Dawson - One of the best experts on this subject based on the ideXlab platform.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
The Astrophysical Journal, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis ɑ = 0.370^(+0.007)_(-0.006) AU with a large eccentricity (e = 0.85^(+0.08)_(-0.07)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 ± 0.002), Hierarchically separated (a = 1.68 ± 0.03 AU) giant planet (7.3 ± 0.4 M J_(up)). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 ± 0.3 M J_(up) and confirm its photometrically measured eccentricity, refining the value to e = 0.83 ± 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9^(+8)_(-6) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370 +0.007/-0.006 AU with a large eccentricity e=0.85 +0.08/-0.07 measured via the "photoeccentric effect." It exhibits transit timing variations induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e=0.184 +/- 0.002), Hierarchically-separated (a=1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 MJup). We combine sixteen quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer (HIRES) on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of inner planet to be 2.5+/-0.3MJup and confirm its photometrically-measured eccentricity, refining the value to e=0.83+/-0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that, despite their sizable eccentricities, the planets are coplanar to within 9 +8/-6 degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1m-class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
Ruth Murrayclay - One of the best experts on this subject based on the ideXlab platform.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
The Astrophysical Journal, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis ɑ = 0.370^(+0.007)_(-0.006) AU with a large eccentricity (e = 0.85^(+0.08)_(-0.07)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 ± 0.002), Hierarchically separated (a = 1.68 ± 0.03 AU) giant planet (7.3 ± 0.4 M J_(up)). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 ± 0.3 M J_(up) and confirm its photometrically measured eccentricity, refining the value to e = 0.83 ± 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9^(+8)_(-6) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370 +0.007/-0.006 AU with a large eccentricity e=0.85 +0.08/-0.07 measured via the "photoeccentric effect." It exhibits transit timing variations induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e=0.184 +/- 0.002), Hierarchically-separated (a=1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 MJup). We combine sixteen quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer (HIRES) on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of inner planet to be 2.5+/-0.3MJup and confirm its photometrically-measured eccentricity, refining the value to e=0.83+/-0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that, despite their sizable eccentricities, the planets are coplanar to within 9 +8/-6 degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1m-class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
Phillip A Cargile - One of the best experts on this subject based on the ideXlab platform.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
The Astrophysical Journal, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis ɑ = 0.370^(+0.007)_(-0.006) AU with a large eccentricity (e = 0.85^(+0.08)_(-0.07)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 ± 0.002), Hierarchically separated (a = 1.68 ± 0.03 AU) giant planet (7.3 ± 0.4 M J_(up)). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 ± 0.3 M J_(up) and confirm its photometrically measured eccentricity, refining the value to e = 0.83 ± 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9^(+8)_(-6) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
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large eccentricity low mutual inclination the three dimensional architecture of a Hierarchical System of giant planets
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Rebekah I Dawson, John Asher Johnson, Daniel C Fabrycky, Daniel Foremanmackey, Ruth Murrayclay, Lars A Buchhave, Phillip A Cargile, Kelsey I Clubb, Benjamin J Fulton, Leslie HebbAbstract:We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) System to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370 +0.007/-0.006 AU with a large eccentricity e=0.85 +0.08/-0.07 measured via the "photoeccentric effect." It exhibits transit timing variations induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e=0.184 +/- 0.002), Hierarchically-separated (a=1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 MJup). We combine sixteen quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer (HIRES) on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of inner planet to be 2.5+/-0.3MJup and confirm its photometrically-measured eccentricity, refining the value to e=0.83+/-0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that, despite their sizable eccentricities, the planets are coplanar to within 9 +8/-6 degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1m-class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
