Efeitos da aplicação de retardador (CCC) e acelerador (GA) de crescimento na morfologia e produtividade do feijoeiro (Phaseolus vulgaris L. cv. Carioca)

Verificou-se os efeitos de CCC e GA quando aplicados sob a forma de pulverização das plântulas, na morfologia, florescimento e produtividade do feijoeiro cultivar Carioca, em condições de casa de vegetação. Estudou-se as concentrações de 500, 2000 e 4000 ppm de CCC juntamente com 50 pprn de GA; sendo que CCC 500 + GA 50 ppm promoveu aceleração no crescimento da haste principal e CCC 4000 + GA 50 ppm retardou esse crescimento em relação ao controle. Aplicação de CCC 500 + GA 50 ppm aumentou o número de folhas do feijoeiro. Num período de 2 semanas após o tratamento com CCC 500 + GA 50 ppm ocorreu aumento no comprimento dos meritalos, sendo que 30 dias após a aplicação de CCC 4000 + GA 50 ppm verificou-se diminuição no comprimento dos mesmos. Observou-se aumento no comprimento do limbo foliar 5 dias após os tratamentos com CCC 500 + GA 50 ppm ou CCC 2000 + GA 50 ppm. Ocorreu aumento no número médio de flores com aplicação de CCC 500 + GA 50 ppm. Não ocorreram diferenças significativas entre a produtividade das plantas tratadas com relação ao controle.In this paper the autors tested the effects of (2 - chloroethyl) trimethylammonium chloride (CCC) and gibberellic acid (GA) on the cultivar Carioca of bean, in three different concentrations (500, 2000, and 4000 ppm) of CCC and one concentration of GA (50 ppm). Treatment with CCC 500 ppm + GA 50 ppm increased the height of bean plant and CCC 4000 ppm + GA 50 ppm reduced the height of Phaseolus vulgaris. Application of CCC 500 ppm + GA 50 ppm or CCC 2000 ppm + GA 50 ppm increased the leaf number of bean plant. CCC 500 ppm + GA 50 ppm promoted a increase in the internode length and CCC 4000 ppm + GA 50 ppm reduced the length of internodcs. Application of CCC 500 ppm + GA 50 ppm or CCC 2000 ppm + GA 50 ppm increased the leaf length 5 days after the treatment. CCC 500 ppm + GA 50 ppm promoted higher flowering in relation to the check.

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO-Virgo Run O3b

We search for gravitational-wave signals associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (2019 November 1 15:00 UTC-2020 March 27 17:00 UTC). We conduct two independent searches: A generic gravitational-wave transients search to analyze 86 GRBs and an analysis to target binary mergers with at least one neutron star as short GRB progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these GRBs. A weighted binomial test of the combined results finds no evidence for subthreshold gravitational-wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each GRB. Finally, we constrain the population of low-luminosity short GRBs using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate. © 2022. The Author(s). Published by the American Astronomical Society

Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run

Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours-months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets. © 2022. The Author(s). Published by the American Astronomical Society

Search for gravitational-wave transients associated with magnetar bursts in advanced LIGO and advanced Virgo data from the third observing run

Gravitational waves are expected to be produced from neutron star oscillations associated with magnetar giant f lares and short bursts. We present the results of a search for short-duration (milliseconds to seconds) and longduration (∼100 s) transient gravitational waves from 13 magnetar short bursts observed during Advanced LIGO, Advanced Virgo, and KAGRA’s third observation run. These 13 bursts come from two magnetars, SGR1935 +2154 and SwiftJ1818.0−1607. We also include three other electromagnetic burst events detected by FermiGBM which were identified as likely coming from one or more magnetars, but they have no association with a known magnetar. No magnetar giant flares were detected during the analysis period. We find no evidence of gravitational waves associated with any of these 16 bursts. We place upper limits on the rms of the integrated incident gravitational-wave strain that reach 3.6 × 10−²³ Hz at 100 Hz for the short-duration search and 1.1 ×10−²² Hz at 450 Hz for the long-duration search. For a ringdown signal at 1590 Hz targeted by the short-duration search the limit is set to 2.3 × 10−²² Hz. Using the estimated distance to each magnetar, we derive upper limits upper limits on the emitted gravitational-wave energy of 1.5 × 1044 erg (1.0 × 1044 erg) for SGR 1935+2154 and 9.4 × 10^43 erg (1.3 × 1044 erg) for Swift J1818.0−1607, for the short-duration (long-duration) search. Assuming isotropic emission of electromagnetic radiation of the burst fluences, we constrain the ratio of gravitational-wave energy to electromagnetic energy for bursts from SGR 1935+2154 with the available fluence information. The lowest of these ratios is 4.5 × 103

A joint Fermi-GBM and Swift-BAT analysis of gravitational-wave candidates from the third gravitational-wave observing run

We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers

Open data from the third observing run of LIGO, Virgo, KAGRA, and GEO

The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages

Constraints on the cosmic expansion history from GWTC–3

We use 47 gravitational wave sources from the Third LIGO–Virgo–Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC–3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34 M⊙, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding ${H}_{0}={68}_{-8}^{+12}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC–1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of ${H}_{0}={68}_{-6}^{+8}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC–1 result and 20% with respect to recent H0 studies using GWTC–2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814

‘Starlight’ —Great Northern Dry Bean

The release of ‘Starlight’, a Great Northern dry bean cultivar (Phaseolus vulgaris L.), fulfills a need in western Nebraska for a cultivar with a relatively large seed size and a uniformly bright-white seedcoat (Korban et al., 1981). Foreign buyers of Great Northern beans desire a larger seed than the current predominant Great Northern cultivar Beryl (J.A. McGill, Jr., personal communication). In addition, the cultivar possesses improved architectural avoidance mechanisms to white mold disease (WMD) incited by Sclerotinia sclerotiorum (Lib.) de Bary (Coyne, 1980), a serious problem in some seasons in western Nebraska. Origin ‘Starlight’ (evaluated as F10 WM1-85-43) was derived by pedigree selection from a cross of the F5 breeding lines GN-WM2-79-12 and GN-SK-80-45. These lines were derived from crosses of ‘Tacaragua’ from Venezuela (black seed, upright architecture, and resistance to rust) × GN Nebraska #1 selection 27 [resistant to common bacterial blight incited by Xanthomonas campestris pv. phaseoli (Smith) Dye] and ‘GN Emerson’ (large white seed and moderate resistance to common blight) × ‘Bulgarian White’ (unadapted line with late maturity and large white seed), respectively. GN WM2-79-12 is resistant to rust, bean common mosaic virus (BCMV), and common bacterial blight and has a moderately upright and open habit of growth, which contributed to its avoidance of WMD. However, it has small seed with a dull-colored seedcoat. GN SK-80-45 has moderately early maturity and large, uniform, bright-white, Great Northern-type seed with resistance to seedcoat cracking

Registration of Common Bacterial Blight Resistant Pinto Bean Germplasm Line ABCP-8

Pinto bean (Phaseolus vulgaris L.) germplasm line ABCP-8 (Reg. no. GP-237, PI 635118) was developed by the University of Nebraska Agricultural Research Division in cooperation with USDA-ARS and released in 2004. This line was bred specifically for enhanced resistnace to common bacterial blight [caused by Xanthomonas campestris pv. phaseoli (Smith) Dye]. Pinto and other dry bean market classes (dark red kidney, great northern, navy, etc.) grown in the U.S.A. east of the continental divide are often attacked by common bacterial blight, a seed-transmitted disease that causes up to 40% yield loss in susceptible cultivars as well as reduction of seed quality through discoloration of infected seed. Development of cultivars with genetic resistance combined from different sources is the most cost effective method to control common bacterial blight