19,886 research outputs found
Environmental aspects of soil phosphorus testing
peer-reviewedSoil phosphorus testing in Ireland uses Morgan’s reagent from samples taken to 10 cm
depth for agronomic recommendations. However, its suitability as an environmental
indicator has been questioned in terms of sample depth and extraction solution. Seven
grassland sites were sampled to depths of 2, 5 and 10 cm and extracted for Morgan’s
P, the standard agronomic test, as well as iron-oxide impregnated paper strip P (FeOP),
calcium chloride extractable P (CaCl2-P) and water soluble P (WSP), all proposed
as environmental soil tests. Extractable soil P decreased with increasing sample depth,
as did variances in each test, such that, 2 cm samples had highest concentrations and
variances. The current standard sample depth (10 cm) was linearly related to corresponding
data from samples taken to 2 and 5 cm, indicating that surface soil P can be
consistently estimated from the current standard depth. When soil tests were compared
with dissolved reactive P (DRP) in overland flow collected from two field sites,
certain soil tests were better indicators of P loss than others. The relative difference in
Morgan’s P values at the standard sample depth (10 cm) was reflected in the relative
difference in P loss between the two sites. Average values of DRP collected from two
sites ranged from 0.032 to 0.067 mg/l at the low P site and 0.261 to 0.620 at the high P
site. Average DRP values from the high P site and maximum DRP values from the low
P site were simulated using water-soluble P extraction at water to soil ratios 5 to 250
l/kg. In this study, Morgan’s P to 10 cm gave a good indication of the relative difference in DRP loss between the two sites
A Nearly Model-Independent Characterization of Dark Energy Properties as a Function of Redshift
Understanding the acceleration of the universe and its cause is one of the
key problems in physics and cosmology today, and is best studied using a
variety of mutually complementary approaches. Daly and Djorgovski (2003, 2004)
proposed a model independent approach to determine the expansion and
acceleration history of the universe and a number of important physical
parameters of the dark energy as functions of redshift directly from the data.
Here, we apply the method to explicitly determine the first and second
derivatives of the coordinate distance with respect to redshift and combine
them to solve for the acceleration of the universe and the kinetic and
potential energy density of the dark energy as functions of redshift. A data
set of 228 supernova and 20 radio galaxy measurements with redshifts from zero
to 1.79 is used for this study. The values we obtain are shown to be consistent
with the values expected in a standard Lambda Cold Dark Matter model.Comment: 5 pages, 8 figure
A Decade of Dark Energy: 1998 - 2008
The years 1998 to 2008 were very exciting years for cosmology. It was a
pleasure to accept this invitation to describe my contributions to the
development of our knowledge and understanding of the universe over the course
of the past decade. Here, I begin by describing some of my work on radio
galaxies as a modified standard yardstick and go on to describe
model-independent studies of the accelerating universe and the properties of
the dark energy. During the course of these studies, I came upon interesting
ways to study the spin and other properties of supermassive black holes, some
of which are briefly mentioned.Comment: Proceedings of the 2008 UCLA Conference "Dark Matter and Dark Energy
in the Universe," submitted to AIP Conference Proceedings, 6 page
Black Hole Spin Properties of 130 AGN
Supermassive black holes may be described by their mass and spin. When
supermassive black holes are active, the activity provides a probe of the state
of the black hole system. The spin of a hole can be estimated when the black
hole mass and beam power of the source are known for sources with powerful
outflows. Seventy-five sources for which both the black hole mass and beam
power could be obtained are identified and used to obtain estimates of black
hole spins. The 75 supermassive black holes studied include 52 FRII radio
galaxies and 23 FRII radio loud quasars with redshifts ranging from about zero
to two. The new values are combined with those obtained previously for 19 FRII
radio galaxies, 7 FRII radio loud quasars, and 29 radio sources associated with
CD galaxies to form samples of 71 FRII radio galaxies, 30 FRII quasars, and a
total sample of 130 spin values; all of the sources are associated with massive
elliptical galaxies. The new values obtained are similar to those obtained
earlier at similar redshift, and range from about 0.1 to 1 for FRII sources.
The overall results are consistent with those obtained previously: the spins
tend to decrease with decreasing redshift for the FRII sources studied. There
is a hint that the range of values of black hole spin at a given redshift is
larger for FRII quasars than for FRII radio galaxies. There is no indication of
a strong correlation between supermassive black hole mass and spin for the
supermassive black holes studied here. The relation between beam power and
black hole mass is obtained and used as a diagnostic of the outflows and the
dependence of the magnetic field strength on black hole mass.Comment: 12 pages, 12 figures, 5 table
Lateral Expansion of the Bridges of Cygnus A and other Powerful Radio Sources
Measurements of the width of the radio bridge at several locations along the
bridge for each of four powerful extended radio sources are presented. Adopting
a few simple assumptions, these measurements may be used to predict the radio
surface brightness as a function of position across the radio bridge. The
predicted and observed surface brightnesses across the bridges are compared and
found to agree fairly well. The results are consistent with a simple picture in
which the radio power and size of the radio lobe at the forward edge of the
radio bridge are roughly time-independent for a given source, and the expansion
of the bridge in the lateral direction is adiabatic. There is no indication
that reacceleration or energy transport is important in the bridges of these
sources. The rate of lateral expansion of the bridge just behind the radio lobe
and hotspot in terms of the rate of forward propagation is compared with that
predicted, and found to be in good agreement with the predicted value.Comment: 7 pages, uuencoded compressed postscript. To appear in the Proceding
of the Cygnus A workshop, May 1-4, Green Bank, W
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