Patrician culture, public ritual and political authority in Virginia, 1680-1740

During the political squabbles in Virginia that alienated royal governors, burgesses, councilors, and freeholders from one another between 1680 and 1740, middling planters displayed a tendency to ignore the wisdom of their social and economic betters and swayed the colony toward a new political style. When it suited their aspirations, governors, councilors, and burgesses plunged into the business of wooing the freeholders and thus encouraged the electoral ascendancy of the colony\u27s middling men, but at other times they viewed the changes in Virginia\u27s political etiquette suspiciously and objected to what they interpreted as a dangerous trend toward too much popular participation in politics. Politically embattled gentlemen feared any decline in the deference they and their fathers had come to expect from their constituents, and they looked for ways to consolidate, legitimize, and sometimes regain their claims to deference and thus power.;In the seventeenth century the fiat of wealth was accepted as sufficient proof of political legitimacy, but in the context of the profound reordering of social relationships that accompanied the rise of black slavery in the Chesapeake, material things emerged as an important, even essential, prop to any claim to political or social leadership. Virginians and their English cousins had always used material things as a device by which they could measure, compare, and classify each other and gain some sense of whether another household\u27s links to their own were fragile and unconnected or knit with the knot of collateral concern. Material possessions had long served as an essential measure of a man\u27s political worthiness, but in the 1720s the gentry feared that the traditional instruments of prestige--generous holdings in land, labor, and livestock--had lost much of their clout and that the distinctions between rich and poor had grown too thin. In the absence of any persuasive distinctions between the social origins of the colony\u27s emerging native-born elite and the middling sorts, and as blacks emerged by about 1720 as the colony\u27s permanent poor, the gentry sought new ways to distinguish inferiors from superiors. New material possessions filled that need, and new distinctions in dress, housing, diet, and burial customs began to re-clarify the boundaries between the colony\u27s humbler residents and its nascent elite. The effect of the distinctions between the new, elite culture and the older, traditional culture shared by everyone else was the legitimization of the gentry\u27s claim to exercise political power over their fellows and the preservation of their social and political hegemony

Masses, radii, and orbits of small Kepler planets : The transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O).Peer reviewedFinal Accepted Versio

ICAR: endoscopic skull‐base surgery

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Masses, radii, and orbits of small Kepler planets: the transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O)

Perinatal distress in 1p36 deletion syndrome can mimic hypoxic ischemic encephalopathy

1p36 deletion syndrome is a well-described condition with a recognizable phenotype, including cognitive impairment, seizures, and structural brain anomalies such as periventricular leukomalacia (PVL). In a large series of these individuals by Battaglia et al., \u201cbirth history was notable in 50% of the cases for varying degrees of perinatal distress.\u201d Given the potential for perinatal distress, seizures and PVL, we questioned if this disorder has clinical overlap with hypoxic ischemic encephalopathy (HIE). We reviewed the medical records of 69 individuals with 1p36 deletion to clarify the perinatal phenotype of this disorder and determine if there is evidence of perinatal distress and/or hypoxic injury. Our data provides evidence that these babies have signs of perinatal distress. The majority (59% term; 75% preterm) needed resuscitation and approximately 18% had cardiac arrest. Most had abnormal brain imaging (84% term; 73% preterm) with abnormal white matter findings in over half of patients. PVL or suggestion of \u201chypoxic insult\u201d was present in 18% of term and 45% of preterm patients. In conclusion, individuals with 1p36 deletion have evidence of perinatal distress, white matter changes, and seizures, which can mimic HIE but are likely related to their underlying chromosome disorder

Masses, radii, and orbits of small Kepler planets: The transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). © 2014. The American Astronomical Society. All rights reserved.