The Effect of Right-to-Work Laws on Unionization in the United States

State right-to-work laws, the subject of considerable controversy in the industrial relations field, typically state that no person will be required to become a union member or, conversely, be required to abstain from union membership as a condition of obtaining or retaining employment. Little hard evidence exists on the effect of right-to-work laws. Meyers (1955) concludes that in Texas the law does not appear to have had a noticeable impact on union strength. Kuhlman (1955) finds that the Virginia law has caused little change in hiring practices, and he cites lack of enforcement as a major cause. Novit (1969), in examining Indiana as the only state to pass a right-to-work law and subsequently repeal it, argues that the law was ineffective because unions found ways to circumvent its restrictions. During the period 1957-65 when the law was in force in Indiana, there was a dramatic increase in the agency shop which allows nonunion workers but which requires all employees to pay union dues. A Fortune (1957) survey of employers and union leaders in states with right-to-work laws concluded that the laws had little effect on overall union strength. In many states the laws were not being enforced, and in some instances employers were unwilling or unable to avoid de facto union shops. For example, in Arizona it was reported that the attempt to hire a nonunion worker resulted in the union labor force calling in sick. Similarly, in Nevada, South Carolina, South Dakota, and Iowa, the survey found that unions were able to maintain union shop practices in spite of legislation to the contrary. One North Dakota legislator expressed his frustration by remarking, It\u27s a beneficial law to have, but there is no specific use for it right now (Fortune 1957, p. 236). In this paper we pursue the question of the effect of right-to-work laws beyond the impressionistic and fragmented evidence just cited and attempt to determine whether such laws significantly affect union membership. Since measuring the impact of right-to-work laws necessitates holding other things constant, a secondary product of this study is the assessment of the effect of other variables on union membership

Phonon Density of States of LaFeAsO1-xFx

We have studied the phonon density of states (PDOS) in LaFeAsO1-xFx with inelastic neutron scattering methods. The PDOS of the parent compound(x=0) is very similar to the PDOS of samples optimally doped with fluorine to achieve the maximum Tc (x~0.1). Good agreement is found between the experimental PDOS and first-principle calculations with the exception of a small difference in Fe mode frequencies. The PDOS reported here is not consistent with conventional electron-phonon mediated superconductivity

The pre-main sequence binary HK Ori : Spectro-astrometry and EXPORT data

In this paper we present multi-epoch observations of the pre-main sequence binary HK Ori. These data have been drawn from the EXPORT database and are complemented by high quality spectro-astrometric data of the system. The spectroscopic data appear to be very well represented by a combination of an A dwarf star spectrum superposed on a (sub-)giant G-type spectrum. The radial velocity of the system is consistent with previous determinations, and does not reveal binary motion, as expected for a wide binary. The spectral, photometric and polarimetric properties and variability of the system indicate that the active object in the system is a T Tauri star with UX Ori characteristics. The spectro-astrometry of HK Ori is sensitive down to milli-arcsecond scales and confirms the speckle interferometric results from Leinert et al. The spectro-astrometry allows with fair certainty the identification of the active star within the binary, which we suggest to be a G-type T Tauri star based on its spectral characteristics.Comment: MNRAS in press 8 pages 7 figure

The 2dF Galaxy Redshift Survey: spectral types and luminosity functions

We describe the 2dF Galaxy Redshift Survey (2dFGRS) and the current status of the observations. In this exploratory paper, we apply a principal component analysis to a preliminary sample of 5869 galaxy spectra and use the two most significant components to split the sample into five spectral classes. These classes are defined by considering visual classifications of a subset of the 2dF spectra, and also by comparison with high-quality spectra of local galaxies. We calculate a luminosity function for each of the different classes and find that later-type galaxies have a fainter characteristic magnitude, and a steeper faint-end slope. For the whole sample we find M*=−19.7 (for Ω=1, H₀=100 km s⁻¹ Mpc⁻¹), α=−1.3, φ*=0.017. For class 1 (‘early-type’) we find M*=−19.6, α=−0.7, while for class 5 (‘late-type’) we find M*=−19.0, α=−1.7. The derived 2dF luminosity functions agree well with other recent luminosity function estimates

The 2dF galaxy redshift survey: clustering properties of radio galaxies

The clustering properties of local, S1.4 GHz≥ 1 mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20 cm (FIRST) and 2dF Galaxy Redshift surveys. To this aim, we present 271 new bJ≤ 19.45 spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper. The two-point correlation function for the local radio population is found to be entirely consistent with estimates obtained for the whole sample of 2dFGRS galaxies. From measurements of the redshift-space correlation function ξ(s) we derive a redshift-space clustering length s0 = 10.7+0.8 −0.7 Mpc, while from the projected correlation function Ξ(rT) we estimate the parameters of the real-space correlation function ξ(r) = (r/r0) −γ, r0 = 6.7+0.9 −1.1 Mpc and γ= 1.6 ± 0.1, where h = 0.7 is assumed. Different results are instead obtained if we only consider sources that present signatures of active galactic nucleus (AGN) activity in their spectra. These objects are shown to be very strongly correlated, with r0 = 10.9+1.0 −1.2 Mpc and γ= 2 ± 0.1, a steeper slope than has been claimed in other recent works. No difference is found in the clustering properties of radio-AGNs of different radio luminosity. Comparisons with models for ξ(r) show that AGN-fuelled sources reside in dark matter haloes more massive than ∼1013.4 M⊙, higher than the corresponding figure for radio-quiet quasi-stellar objects. This value can be converted into a minimum black hole mass associated with radio-loud, AGN-fuelled objects of MminBH∼ 109 M⊙. The above results then suggest - at least for relatively faint radio objects - the existence of a threshold black hole mass associated with the onset of significant radio activity such as that of radio-loud AGNs; however, once the activity is triggered, there appears to be no evidence for a connection between black hole mass and level of radio outpu