2,011 research outputs found
Individually Transferable Quotas and the Magnuson Act: Creating Economic Efficiency in Our Nation\u27s Fisheries
Implementing Cognitive Behavioral Therapy for Insomnia with Motivational Interviewing in the Mental Health Setting
Can you imagine not sleeping well for weeks or months at a time? Insomnia impacts approximately one-third of adults and is considered the most prevalent of all sleep disorders. With a lack of consistent, quality sleep, insomnia has significant negative consequences that impact a person’s overall mental well-being, like increased anxiety, depression, chronic pain, and daily coping. Cognitive Behavioral Therapy for Insomnia (CBT-I) allows patients to reduce or eliminate insomnia or related symptoms without needing medication to obtain quality and consistent sleep. CBT-I is difficult, so partnering it with Motivational Interviewing (MI) techniques provides patient engagement and compliance to strike a good balance for completion and reduce patient drop-out rates. The primary purposes of the project were to increase patients’ quality of sleep, reduce insomnia symptoms, and reduce symptoms of depression, all while keeping patients engaged. Project outcomes were measured using pre- and post-assessments and weekly sleep diaries. For the project results, 80% of patients improved their sleep quality, reduced insomnia severity, and reduced sleep aid administration. Additionally, 100% of patients improved their sleep efficiency, increased their sleep confidence, and decreased their depressive symptoms. When CBT-I is implemented independently, it typically has a drop-out rate of between 24.7-33%. This project had a 100% patient completion rate, likely attributed to the small group size, longer project implementation duration, and use of MI from project initiation
VLBI for Gravity Probe B. VII. The Evolution of the Radio Structure of IM Pegasi
We present measurements of the total radio flux density as well as
very-long-baseline interferometry (VLBI) images of the star, IM Pegasi, which
was used as the guide star for the NASA/Stanford relativity mission Gravity
Probe B. We obtained flux densities and images from 35 sessions of observations
at 8.4 GHz (wavelength = 3.6 cm) between 1997 January and 2005 July. The
observations were accurately phase-referenced to several extragalactic
reference sources, and we present the images in a star-centered frame, aligned
by the position of the star as derived from our fits to its orbital motion,
parallax, and proper motion. Both the flux density and the morphology of IM Peg
are variable. For most sessions, the emission region has a single-peaked
structure, but 25% of the time, we observed a two-peaked (and on one occasion
perhaps a three-peaked) structure. On average, the emission region is elongated
by 1.4 +- 0.4 mas (FWHM), with the average direction of elongation being close
to that of the sky projection of the orbit normal. The average length of the
emission region is approximately equal to the diameter of the primary star. No
significant correlation with the orbital phase is found for either the flux
density or the direction of elongation, and no preference for any particular
longitude on the star is shown by the emission region.Comment: Accepted for publication in the Astrophysical Journal Supplement
Serie
Discovery of an Energetic Pulsar Associated with SNR G76.9+1.0
We report the discovery of PSR J2022+3842, a 24 ms radio and X-ray pulsar in
the supernova remnant G76.9+1.0, in observations with the Chandra X-ray
telescope, the Robert C. Byrd Green Bank Radio Telescope, and the Rossi X-ray
Timing Explorer (RXTE). The pulsar's spin-down rate implies a rotation-powered
luminosity Edot = 1.2 x 10^{38} erg/s, a surface dipole magnetic field strength
B_s = 1.0 x 10^{12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is
thus the second-most energetic Galactic pulsar known, after the Crab, as well
as the most rapidly-rotating young, radio-bright pulsar known. The radio
pulsations are highly dispersed and broadened by interstellar scattering, and
we find that a large (delta-f / f ~= 1.9 x 10^{-6}) spin glitch must have
occurred between our discovery and confirmation observations. The X-ray pulses
are narrow (0.06 cycles FWHM) and visible up to 20 keV, consistent with
magnetospheric emission from a rotation-powered pulsar. The Chandra X-ray image
identifies the pulsar with a hard, unresolved source at the midpoint of the
double-lobed radio morphology of SNR G76.9+1.0 and embedded within faint,
compact X-ray nebulosity. The spatial relationship of the X-ray and radio
emissions is remarkably similar to extended structure seen around the Vela
pulsar. The combined Chandra and RXTE pulsar spectrum is well-fitted by an
absorbed power-law model with column density N_H = (1.7\pm0.3) x 10^{22}
cm^{-2} and photon index Gamma = 1.0\pm0.2; it implies that the Chandra
point-source flux is virtually 100% pulsed. For a distance of 10 kpc, the X-ray
luminosity of PSR J2022+3842 is L_X(2-10 keV) = 7.0 x 10^{33} erg s^{-1}.
Despite being extraordinarily energetic, PSR J2022+3842 lacks a bright X-ray
wind nebula and has an unusually low conversion efficiency of spin-down power
to X-ray luminosity, L_X/Edot = 5.9 x 10^{-5}.Comment: 8 pages in emulateapj format. Minor changes (including a shortened
abstract) to reflect the version accepted for publicatio
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