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FEMAâs Public Assistance Grant Program: Background and Considerations for Congress
[Excerpt] The Robert T. Stafford Disaster Relief and Emergency Assistance Act (42 U.S.C. 5121 et seq., henceforth the Stafford Act) confers upon the President a broad set of authorities âto alleviate the suffering and damageâ of affected tribal, state, and local governments, as well as individual citizens, from disasters. The Federal Emergency Management Agency (FEMA) of the Department of Homeland Security (DHS) has been given the responsibility of administering almost all of the Presidentâs Stafford Act authorities through other law, a series of Executive Orders, and a DHS delegation. FEMA has established the Public Assistance (PA) Grant Program by combining the authority of multiple sections of the Stafford Act. The PA Program provides financial grant assistance to states, tribes, and local communities both in the response to and recovery from significant disasters. Between FY2000-FY2013, the PA Program has provided $52.6 billion in grant assistance to help communities pay for an array of eligible response and recovery activities, including debris removal, emergency protective measures, and the repair, replacement, or restoration of disaster-damaged, publicly owned facilities and the facilities of certain private nonprofit (PNP) organizations. The authorities of the PA Program were most recently significantly amended by the Sandy Recovery Improvement Act (Division B of P.L. 113- 2, the Disaster Relief Appropriations Act, 2013; henceforth SRIA). For a brief legislative history of PA Program authorities, see Appendix A.
This report provides background on key elements of the PA Program, such as the eligibility of applicants, the types of assistance available, and the methods FEMA uses for awarding grant assistance. Summary analysis of federal obligations for PA Program assistance is also provided along important variables, such as the distribution of federal obligations across the PA Program eligible categories of work assistance. The report concludes with discussion of several policy issues that Congress may wish to consider when evaluating the PA Program in the future, including considerations of significant prospective changes to the PA Program and the role of the PA Program in the context of other federal agency disaster assistance authorities
Polarimetric variations of binary stars. II. Numerical simulations for circular and eccentric binaries in Mie scattering envelopes
We present numerical simulations of the periodic polarimetric variations
produced by a binary star placed at the center of an empty spherical cavity
inside a circumbinary ellipsoidal and optically thin envelope made of dust
grains. Mie single-scattering is considered along with pre- and post-scattering
extinction factors which produce a time-varying optical depth and affect the
morphology of the periodic variations. We are interested in the effects that
various parameters will have on the average polarization, the amplitude of the
polarimetric variations, and the morphology of the variability. We show that
the absolute amplitudes of the variations are smaller for Mie scattering than
for Thomson scattering. Among the four grain types that we have studied, the
highest polarizations are produced by grains with sizes in the range 0.1-0.2
micron. In general, the variations are seen twice per orbit. In some cases,
because spherical dust grains have an asymmetric scattering function, the
polarimetric curves produced also show variations seen once per orbit.
Circumstellar disks produce polarimetric variations of greater amplitude than
circumbinary envelopes.
Another goal of these simulations is to see if the 1978 BME (Brown, McLean, &
Emslie, ApJ, 68, 415) formalism, which uses a Fourier analysis of the
polarimetric variations to find the orbital inclination for Thomson-scattering
envelopes, can still be used for Mie scattering. We find that this is the case,
if the amplitude of the variations is sufficient and the true inclinations is
i_true > 45 deg. For eccentric orbits, the first-order coefficients of the
Fourier fit, instead of second-order ones, can be used to find almost all
inclinations.Comment: 23 pages, 5 figures, to be published in Astronomical Journa
On the cornerstones of personhood, the creation of the self and the formation of individual identity
This thesis aims to set out some provisional theories as to the essential factors that motivate a person to give notable prominence to a particular aspect of their person and thereby orient their attitudes and behaviours to the expression of that aspect and, in some cases, the pursuit of the right to do so. This is achieved in three chapters. The first chapter concerns the nature of identity. I draw upon the work of David Hume in explaining how identity is constituted in the being of an object, and go on to explore how such definitions can be applied to human identity, highlighting some of the problems that Hume encountered. In an effort to address these issues, I draw on the work of Jean-Paul Sartre to explain how it is possible for a person to apprehend their own self, and set out to demonstrate how Sartre's theory accounts for the creation of a personal sense of self, and the consequences thereof. Where relevant, I indicate how Sartre's view complements or resembles Hume's earlier account to demonstrate the concordance between them. The second chapter consists of four short, but focused studies of significant 'cornerstones' of personhood in an attempt to demonstrate how the phenomena described in the first chapter come to bear in real world situations. These studies of race, nationhood, gender, and sexuality should serve to demonstrate that there is a consistent and relatively predictable pattern of stimulus and response that results in a person placing particular emphasis on one of these cornerstones. The third chapter expands upon the themes introduced in chapter 1, explicating their relationship to each other and to the real world, culminating in the conclusion that the way in which individuals perceive themselves in relation to the world has a specific and identifiable behavioural response with specific social consequences
William H. Bordley (1820-1905)
Mr. William H. Bordley was born in Kent County Maryland in 1820. I was unable to find the names of his parents but there are a lot of Bordleys in Maryland. The name Bordley can also be spelled Broadly, Broadley, Brodly, or Boardly but I will spell it Bordley. William H. Bordley lived in Savannah until he died in 1905. He fathered seven children, three girls and four boys.https://digitalcommons.georgiasouthern.edu/sav-bios-lane/1017/thumbnail.jp
The coevolution of toxin and antitoxin genes drives the dynamics of bacterial addiction complexes and intragenomic conflict
Bacterial genomes commonly contain âaddictionâ gene complexes that code for both a toxin and a corresponding antitoxin. As long as both genes are expressed, cells carrying the complex can remain healthy. However, loss of the complex (including segregational loss in daughter cells) can entail death of the cell. We develop a theoretical model to explore a number of evolutionary puzzles posed by toxinâantitoxin (TA) population biology. We first extend earlier results demonstrating that TA complexes can spread on plasmids, as an adaptation to plasmid competition in spatially structured environments, and highlight the role of kin selection. We then considered the emergence of TA complexes on plasmids from previously unlinked toxin and antitoxin genes. We find that one of these traits must offer at least initially a direct advantage in some but not all environments encountered by the evolving plasmid population. Finally, our study predicts non-transitive ârock-paper-scissorsâ dynamics to be a feature of intragenomic conflict mediated by TA complexes. Intragenomic conflict could be sufficient to select deleterious genes on chromosomes and helps to explain the previously perplexing observation that many TA genes are found on bacterial chromosomes
Synergy and Group Size in Microbial Cooperation
Microbes produce many molecules that are important for their growth and development, and the consumption of these secretions by nonproducers has recently become an important paradigm in microbial social evolution. Though the production of these public goods molecules has been studied intensely, little is known of how the benefits accrued and costs incurred depend on the quantity of public good molecules produced. We focus here on the relationship between the shape of the benefit curve and cellular density with a model assuming three types of benefit functions: diminishing, accelerating, and sigmoidal (accelerating then diminishing). We classify the latter two as being synergistic and argue that sigmoidal curves are common in microbial systems. Synergistic benefit curves interact with group sizes to give very different expected evolutionary dynamics. In particular, we show that whether or not and to what extent microbes evolve to produce public goods depends strongly on group size. We show that synergy can create an âevolutionary trapâ which can stymie the establishment and maintenance of cooperation. By allowing density dependent regulation of production (quorum sensing), we show how this trap may be avoided. We discuss the implications of our results for experimental design
Exploring the Design of Pay-Per-Use Objects in the Construction Domain
Equipment used in the construction domain is often hired in order to reduce cost and maintenance overhead. The cost of hire is dependent on the time period involved and does not take into account the actual use equipment has received. This paper presents our initial investigation into how physical objects augmented with sensing and communication technologies can measure use in order to enable new pay-per-use payment models for equipment hire. We also explore user interaction with pay-per-use objects via mobile devices. The user interactions that take place within our prototype scenario range from simple information access to transactions involving multiple users. This paper presents the design, implementation and evaluation of a prototype pay-per-use system motivated by a real world equipment hire scenario. We also provide insights into the various challenges introduced by supporting a pay-per-use model, including data storage and data security in addition to user interaction issues
The return of the Andromedids meteor shower
The Andromedid meteor shower underwent spectacular outbursts in 1872 and
1885, producing thousands of visual meteors per hour and described as `stars
fell like rain' in Chinese records of the time. The shower originates from
comet 3D/Biela whose disintegration in the mid-1800's is linked to the
outbursts, but the shower has been weak or absent since the late 19th Century.
This shower returned in December 2011 with a zenithal hourly rate of
approximately 50, the strongest return in over a hundred years. Some 122
probable Andromedid orbits were detected by the Canadian Meteor Orbit Radar.
The shower outburst occurred during 2011 Dec 3-5. The radiant at RA
+ and Dec + is typical of the `classical' Andromedids of
the early 1800's, whose radiant was actually in Cassiopeia. The orbital
elements indicate that the material involved was released before 3D/Biela's
breakup prior to 1846. The observed shower in 2011 had a slow geocentric speed
(16 km s) and was comprised of small particles: the mean measured mass
from the radar is kg corresponding to radii of 0.5 mm at
a bulk density of 1000 kg/m.
Numerical simulations of the parent comet indicate that the meteoroids of the
2011 return of the Andromedids shower were primarily ejected during 3D/Biela's
1649 perihelion passage. The orbital characteristics, radiant, timing as well
as the absence of large particles in the streamlet are all consistent with
simulations. Predictions are made regarding other appearances of the shower in
the years 2000-2047 based on our numerical model. We note that the details of
the 2011 return can, in principle, be used to better constrain the orbit of
3D/Biela prior to the comets first recorded return in 1772.Comment: submitted to the Astronomical Journal Sep 22 201
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