Salaries of Members of Congress: Recent Actions and Historical Tables

[Excerpt] This report contains information on the pay procedure and actions and freezes since the last pay adjustment in 2009. It also contains historical information on the rate of pay for Members of Congress since 1789; the adjustments projected by the Ethics Reform Act as compared to actual adjustments in Member pay; details on past legislation enacted with language prohibiting the annual pay adjustment; and Member pay in constant and current dollars since 1992

Salaries of Members of Congress: Congressional Votes, 1990-2014

The automatic annual adjustment for Members of Congress is determined by a formula using a component of the Employment Cost Index (ECI), which measures rate of change in private sector pay. The adjustment automatically takes effect unless (1) Congress statutorily prohibits the adjustment; (2) Congress statutorily revises the adjustment; or (3) the annual base pay adjustment of General Schedule (GS) federal employees is established at a rate less than the scheduled increase for Members, in which case the percentage adjustment for Member pay is automatically lowered to match the percentage adjustment in GS base pay. In the past, Member pay has been frozen statutorily in two ways: (1) directly, through legislation that freezes salaries for Members but not other federal employees, and (2) indirectly, through broader pay freeze legislation that covers Members and other specified categories of federal employees. Under the formula, Members may not receive an annual pay adjustment greater than 5%. This adjustment formula was established by the Ethics Reform Act of 1989. Votes on the annual adjustments since the implementation of this act are contained in this report

Salaries of Members of Congress: A List of Payable Rates and Effective Dates, 1789-2008

Congress is required by Article I, Section 6, of the Constitution to determine its own pay. Prior to 1969, Congress did so by enacting stand-alone legislation. From 1789 through 1968, Congress raised its pay 22 times using this procedure. Congressional salaries initially were $1,500. By 1968, they had risen to$30,000. Stand-alone legislation may still be used to raise Member pay, as it was most recently in 1982, 1983, 1989, and 1991, but two other methods — including an automatic annual adjustment procedure and a commission process — are now also available. Under the annual adjustment procedure, Members were scheduled to receive a 2.7% increase in January 2008. The increase was revised to 2.5%, resulting in a salary in 2008 of $169,300, to match the percent increase in the base pay of General Schedule (GS) employees. By law, Members may not receive an increase greater than the increase in the base pay of GS employees. Congress voted to deny the scheduled January 2007 adjustment. Members last received a pay increase (1.9$165,200

Genus Two Partition Functions and Renyi Entropies of Large c CFTs

We compute genus two partition functions in two dimensional conformal field theories at large central charge, focusing on surfaces that give the third Renyi entropy of two intervals. We compute this for generalized free theories and for symmetric orbifolds, and compare it to the result in pure gravity. We find a new phase transition if the theory contains a light operator of dimension $\Delta\leq0.19$. This means in particular that unlike the second Renyi entropy, the third one is no longer universal.Comment: 28 pages + Appendice

Orbital Circularization of a Planet Accreting Disk Gas: Formation of Distant Jupiters in Circular Orbits based on Core Accretion Model

Recently, gas giant planets in nearly circular orbits with large semimajor axes ($a \sim$ 30--1000AU) have been detected by direct imaging. We have investigated orbital evolution in a formation scenario for such planets, based on core accretion model: i) Icy cores accrete from planetesimals at $\lesssim$ 30AU, ii) they are scattered outward by an emerging nearby gas giant to acquire highly eccentric orbits, and iii) their orbits are circularized through accretion of disk gas in outer regions, where they spend most of time. We analytically derived equations to describe the orbital circularization through the gas accretion. Numerical integrations of these equations show that the eccentricity decreases by a factor of more than 5 during the planetary mass increases by a factor of 10. Because runaway gas accretion increases planetary mass by $\sim$ 10--300, the orbits are sufficiently circularized. On the other hand, $a$ is reduced at most only by a factor of 2, leaving the planets in outer regions. If the relative velocity damping by shock is considered, the circularization is slowed down, but still efficient enough. Therefore, this scenario potentially accounts for the formation of observed distant jupiters in nearly circular orbits. If the apocenter distances of the scattered cores are larger than the disk sizes, their $a$ shrink to a quarter of the disk sizes; the $a$-distribution of distant giants could reflect outer edges of the disks in a similar way that those of hot jupiters may reflect inner edges.Comment: 28 pages, 13 figures, accepted for publication in Ap

Twist-nontwist correlators in M^N/S_N orbifold CFTs

We consider general 2D orbifold CFTs of the form M^N/S_N, with M a target space manifold and S_N the symmetric group, and generalize the Lunin-Mathur covering space technique in two ways. First, we consider excitations of twist operators by modes of fields that are not twisted by that operator, and show how to account for these excitations when computing correlation functions in the covering space. Second, we consider non-twist sector operators and show how to include the effects of these insertions in the covering space. We work two examples, one using a simple bosonic CFT, and one using the D1-D5 CFT at the orbifold point. We show that the resulting correlators have the correct form for a 2D CFT.Comment: 30 pages, 1 figure, additional reference adde

Operator mixing for string states in the D1-D5 CFT near the orbifold point

In the context of the fuzzball programme, we investigate deforming the microscopic string description of the D1-D5 system on T^4xS^1 away from the orbifold point. Using conformal perturbation theory and a generalization of Lunin-Mathur symmetric orbifold technology for computing twist-nontwist correlators developed in a companion work, we initiate a program to compute the anomalous dimensions of low-lying string states in the D1-D5 superconformal field theory. Our method entails finding four-point functions involving a string operator O of interest and the deformation operator, taking coincidence limits to identify which other operators mix with O, subtracting the identified conformal family to isolate other contributions to the four-point function, finding the mixing coefficients, and iterating. For the lowest-lying string modes, this procedure should truncate in a finite number of steps. We check our method by showing how the operator dual to the dilaton does not participate in mixing that would change its conformal dimension, as expected. Next we complete the first stage of the iteration procedure for a low-lying string state of the form \partial X \partial X \bar\partial X \bar\partial X and find its mixing coefficient. Our main qualitative result is evidence of operator mixing at first order in the deformation parameter, which means that the string state acquires an anomalous dimension. After diagonalization this will mean that anomalous dimensions of some string states in the D1-D5 SCFT must decrease away from the orbifold point while others increase.Comment: 43 pages, added references and a commen

Bosonization, cocycles, and the D1-D5 CFT on the covering surface

We consider the D1-D5 CFT near the orbifold point, specifically the computation of correlators involving twist sector fields using covering surface techniques. As is well known, certain twists introduce spin fields on the cover. Here we consider the bosonization of fermions to facilitate computations involving the spin fields. We find a set of cocycle operators that satisfy constraints coming from various $SU(2)$ symmetries, including the $SU(2)_L\times SU(2)_R$ R-symmetry. Using these cocycles, we consider the correlator of four spin fields on the cover, and show that it is invariant under all of the $SU(2)$ symmetries of the theory. We consider the mutual locality of operators, and compute several three-point functions. These computations lead us to a notion of radial ordering on the cover that is inherited from the original computation before lifting. Further, we note that summing over orbifold images sets certain branch-cut ambiguous correlators to zero.Comment: 29 pages, 1 figur

Women in the United States Congress: Historical Overview, Tables, and Discussion

A record 102 women currently serve in the 113th Congress: 82 in the House (63 Democrats and 19 Republicans) and 20 in the Senate (16 Democrats and 4 Republicans). One hundred one women were initially sworn in to the 113th Congress—1 female Republican House Member has since resigned, and 2 Democratic House Members have been elected. This is higher than the previous record number of 95 women who were initially elected to the 111th Congress. The first woman elected to Congress was Representative Jeannette Rankin (R- MT, 1917-1919, 1941-1943). The first woman to serve in the Senate was Rebecca Latimer Felton (D-GA). She was appointed in 1922 and served for only one day. Hattie Caraway (D-AR, 1931-1945) was the first Senator to succeed her husband and the first woman elected to a six-year Senate term. A total of 298 women have served in Congress, 194 Democrats and 104 Republicans. Of these women, 254 (165 Democrats, 89 Republicans) have served only in the House of Representatives; 34 (21 Democrats, 13 Republicans) have served only in the Senate; and 10 (8 Democrats, 2 Republicans) have served in both houses. These figures include 4 non-voting Delegates, 1 each from Guam, Hawaii, the District of Columbia, and the U.S. Virgin Islands. A total of 33 African American women have served in Congress (1 in the Senate, 32 in the House), including 17 serving in the 113th Congress. Ten Hispanic women have been elected to the House; nine serve in the 113th Congress. Nine Asian Pacific American women have served in Congress (8 in the House, 1 in both the House and Senate), including seven in the 113th Congress. Nineteen women in the House, and 10 women in the Senate, have chaired committees. In the 113th Congress, 1 woman chairs a House committee, and 5 women chair Senate committees, with 1 female Senator chairing two committees. This report includes a discussion of the impact of women in Congress as well as historical information, including the number and percentage of women in Congress over time, means of entry to Congress, comparisons to international and state legislatures, records for tenure, firsts for women in Congress, women in leadership, and African American and Asian Pacific American women in Congress. The report may reflect data at the beginning or end of each Congress, or changes during a Congress. See the notes throughout the report for information on the currency of the data

3D MHD Simulations of Planet Migration in Turbulent Stratified Disks

We performed 3D MHD simulations of planet migration in stratified disks using the Godunov code PLUTO, where the disk is turbulent due to the magnetorotational instability. We study the migration for planets with different planet-star mass ratios $q=M_{p}/M_{s}$. In agreement with previous studies, for the low-mass planet cases ($q=5\times10^{-6}$ and $10^{-5}$), migration is dominated by random fluctuations in the torque. For a Jupiter-mass planet $(q=M_{p}/M_{s}=10^{-3}$ for $M_{s}=1M_{\odot})$, we find a reduction of the magnetic stress inside the orbit of the planet and around the gap region. After an initial stage where the torque on the planet is positive, it reverses and we recover migration rates similar to those found in disks where the turbulent viscosity is modelled by an $\alpha$ viscosity. For the intermediate-mass planets ($q=5\times10^{-5}, 10^{-4}$ and $2\times10^{-4}$) we find a new and so far unexpected behavior. In some cases they experience sustained and systematic outwards migration for the entire duration of the simulation. For this case, the horseshoe region is resolved and torques coming from the corotation region can remain unsaturated due to the stresses in the disk. These stresses are generated directly by the magnetic field. The magnitude of the horseshoe drag can overcome the negative Lindblad contribution when the local surface density profile is flat or increasing outwards, which we see in certain locations in our simulations due to the presence of a zonal flow. The intermediate-mass planet is migrating radially outwards in locations where there is a positive gradient of a pressure bump (zonal flow).Comment: Accepted for publication in Ap