The Influence of Socioeconomic Factors on Fear of Falling and Mobility Outcomes after Lower Limb Loss: a Preliminary Study

Background and Purpose: Current research has revealed that as much as 52.4% of individuals with lower limb loss report falling at least once in the past year. Previous research has also indicated that rehabilitation, including physical therapy (PT), generally improves patient outcomes after definitive amputation. Socioeconomic status has been shown to be an important factor in accessing healthcare but has yet to be investigated in this population. The purpose of this study was to investigate the effects of socioeconomic status and access to PT, and how limb loss affects mobility and fear of falling perception. We hypothesized: [1] individuals with socioeconomic difficulty would have reduced access to PT after amputation, and [2] individuals with limb loss will have increased fear of falling and decreased mobility performance when compared to non-amputee, age-matched controls. Subjects: 23 participants (7 females,16 males) mean age 51.30 years old (+ 13.17 SD, range 22-70) with lower limb loss ambulating with a definitive prosthesis. Materials/Methods: Participants completed a survey that included the Fear of Falling Avoidance Behavior Questionnaire (FFABQ), questions to determine their socioeconomic status, and whether they received PT after amputation. Mobility outcomes were measured using the standardized Timed Up and Go test (TUG) and the Six Minute Walk Test (6MWT). Results: There was no statistically significant difference in access to PT after amputation between those with and without financial difficulty (p=.354). However, 75% of participants who had no socioeconomic difficulty reported receiving PT, in comparison to only 25% in those who had socioeconomic difficulty. Additionally, 34.8% of our participants reported socioeconomic difficulties. When comparing the participants with amputation to the non-amputee, age-matched controls, there was a significant difference in the TUG (p\u3c.001), 6MWT (p\u3c.001), and FFABQ (p=.008). On average, participants with limb loss were 4.4 seconds slower on the TUG, walked 136.4m less on the 6MWT, and had an increased FFABQ score of 6.6 points out of 56 points. Discussion: Access to physical therapy and socioeconomic status have been overlooked in current literature for individuals after amputation. While the effect of socioeconomic status on PT access did not reach statistical significance in this preliminary study, only 25% of those who reported socioeconomic difficulty received physical therapy after amputation, compared to 75% in those who reported no difficulty. Further research is needed to determine whether low socioeconomic status is predictive of receiving rehabilitation services post-amputation and long-term outcomes. Our findings also showed that when compared to age-matched non-amputees, amputees tend to have impaired mobility and higher degree of fear of falling. These findings agree with current literature. Conclusion: Although not statistically significant, our preliminary findings showed that socioeconomic difficulty may affect access to physical therapy after amputation. Furthermore, our data demonstrated that individuals with lower limb loss exhibit reduced mobility performance and increased fear of falling when compared to the age-matched controls

Minding the Gap: A Discourse Analysis on Corporate and Adolescent Users on Snapchat

This MRP investigates popular discourses within commercial social media. Through examining Snapchat, this MRP suggests that there are two main influences that dictate the cultural language used within the Snapchat community – the adolescent user and the corporate user. By applying Gee’s Discourse Analysis Tools (Gee, 2014), this MRP seeks to understand how both users demonstrate their co-constructed cultural language proficiencies by constructing multimodal texts and provide discussion that explains for what purposes that language is used. This MRP has found that there are clear neoliberal influences that may shape adolescent identity formation. However, adolescents also demonstrate that they are just as influential towards the larger meaning making of cultural language within their community. Understanding the adolescent perspective is important, because they are the group who have grown up with social media. (Joosten, 2012) Therefore, the insights that they have may have are valuable when attempting to understand the impact that social media has on their process of meaning making. Juxtaposing both the adolescent and corporate user, this MRP intends to show effective uses of social media and how each user uses their competency to construct and re-construct meaning based on their goals. Providing this perspective will in turn allow educators to reflect upon their practice, and hopefully gain insights to using the innate abilities of adolescents, in addition to re-appropriating techniques currently used by neoliberal influences to conversely benefit adolescent learning

CAN Bus: The Future of Additive Manufacturing (3D Printing)

Additive Manufacturing (AM) is gaining renewed popularity and attention due to low-cost fabrication systems proliferating the market. Current communication protocols used in AM limit the connection flexibility between the control board and peripherals; they are often complex in their wiring and thus restrict their avenue of expansion. Thus, the Controller Area Network (CAN) bus is an attractive pathway for inter-hardware connections due to its innate quality. However, the combination of CAN and AM is not well explored and documented in existing literature. This article aims to provide examples of CAN bus applications in AM.Comment: 6 page

Infall and Outflow around the HH 212 protostellar system

HH 212 is a highly collimated jet discovered in H2 powered by a young Class 0 source, IRAS 05413-0104, in the L1630 cloud of Orion. We have mapped around it in 1.33 mm continuum, 12CO ($J=2-1$), 13CO ($J=2-1$), C18O ($J=2-1$), and SO ($J_K = 6_5-5_4$) emission at $\sim$ \arcs{2.5} resolution with the Submillimeter Array. A dust core is seen in the continuum around the source. A flattened envelope is seen in C18O around the source in the equator perpendicular to the jet axis, with its inner part seen in 13CO. The structure and kinematics of the envelope can be roughly reproduced by a simple edge-on disk model with both infall and rotation. In this model, the density of the disk is assumed to have a power-law index of $p=-1.5$ or -2, as found in other low-mass envelopes. The envelope seems dynamically infalling toward the source with slow rotation because the kinematics is found to be roughly consistent with a free fall toward the source plus a rotation of a constant specific angular momentum. A 12CO outflow is seen surrounding the H2 jet, with a narrow waist around the source. Jetlike structures are also seen in 12CO near the source aligned with the H2 jet at high velocities. The morphological relationship between the H2 jet and the 12CO outflow, and the kinematics of the 12CO outflow along the jet axis are both consistent with those seen in a jet-driven bow shock model. SO emission is seen around the source and the H2 knotty shocks in the south, tracing shocked emission around them.Comment: 17 pages, 11 figures, Accepted by the Ap

The CO Molecular Outflows of IRAS 16293-2422 Probed by the Submillimeter Array

We have mapped the proto-binary source IRAS 16293-2422 in CO 2-1, 13CO 2-1, and CO 3-2 with the Submillimeter Array (SMA). The maps with resolution of 1".5-5" reveal a single small scale (~3000 AU) bipolar molecular outflow along the east-west direction. We found that the blueshifted emission of this small scale outflow mainly extends to the east and the redshifted emission to the west from the position of IRAS 16293A. A comparison with the morphology of the large scale outflows previously observed by single-dish telescopes at millimeter wavelengths suggests that the small scale outflow may be the inner part of the large scale (~15000 AU) E-W outflow. On the other hand, there is no clear counterpart of the large scale NE-SW outflow in our SMA maps. Comparing analytical models to the data suggests that the morphology and kinematics of the small scale outflow can be explained by a wide-angle wind with an inclination angle of ~30-40 degrees with respect to the plane of the sky. The high resolution CO maps show that there are two compact, bright spots in the blueshifted velocity range. An LVG analysis shows that the one located 1" to the east of source A is extremely dense, n(H_2)~10^7 cm^-3, and warm, T_kin >55 K. The other one located 1" southeast of source B has a higher temperature of T_kin >65 K but slightly lower density of n(H_2)~10^6 cm^-3. It is likely that these bright spots are associated with the hot core-like emission observed toward IRAS 16293. Since both two bright spots are blueshifted from the systemic velocity and are offset from the protostellar positions, they are likely formed by shocks.Comment: 27 pages, 8 figures, accepted for publication in ApJ, minor typos correcte

PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows and Hot Cores

This paper presents a large spectral line and continuum survey of 8 deeply embedded, low-mass protostellar cores using the Submillimeter Array. Each source was observed in high excitation lines of some of the most common molecular species, CO, HCO+, CS, SO, H2CO, CH3OH and SiO. Line emission from 11 species originating from warm and dense gas have been imaged at high angular resolution (1-3"; typically 200-600 AU) together with continuum emission at 230 GHz (1.3 mm) and 345 GHz (0.8 mm). Compact continuum emission is observed for all sources which likely originates in marginally optically thick circumstellar disks, with typical lower limits to their masses of 0.1 M_sun (1-10% of the masses of their envelopes) and having a dust opacity law with beta approximately 1. Prominent outflows are present in CO 2-1 observations in all sources: the most diffuse outflows are found in the sources with the lowest ratios of disk-to-envelope mass, and it is suggested that these sources are in a phase where accretion of matter from the envelope has almost finished and the remainder of the envelope material is being dispersed by the outflows. Other characteristic dynamical signatures are found with inverse P Cygni profiles indicative of infalling motions seen in the 13CO 2-1 lines toward NGC1333-IRAS4A and -IRAS4B. Outflow-induced shocks are present on all scales in the protostellar environments and are most clearly traced by the emission of CH3OH in NGC1333-IRAS4A and -IRAS4B. These observations suggest that the emission of CH3OH and H2CO from these proposed "hot corinos" are related to the shocks caused by the protostellar outflows. Only one source, NGC1333-IRAS2A, has evidence for hot, compact CH3OH emission coincident with the embedded protostar.Comment: Accepted for publication in ApJ (52 pages; 9 figures). Abstract abridge

Lunar-sourced GEO Powersats: An Integrated ISRU System

Solar power satellites (powersats) can be built almost entirely from lunar resources. When C-class asteroids are also included as ore bodies a complete powersat can be built through insitu resource utilization (ISRU) given appropriate processing and transportation technology.This article provides an in-depth overview of the technical feasibility and economic viabilityof lunar construction and operations for powersat component construction and delivery togeostationary earth orbit (GEO). Techno-economic analysis suggests a return on investmentin seven years assuming a three percent discount rate. Electrical power collected in GEO andbeamed to terrestrial receivers by the powersats can be sold as baseload power in the wholesale electricity market to generate revenue. This work presents a complete concept of operationsfrom initial rocket launches to regolith harvesting through transport to GEO. Lunarinfrastructure can be constructed of modules to optimize size and weight for launch costs.Future growth can be derived from using ISRU to build additional processing bases. A scale-up in this manner can provide 22% of the world’s energy needs by the end of a 20-year period.This work builds upon previous studies and completes the architectural description ofpredominantly lunar-sourced GEO powersats

Extreme Active Molecular Jets in L1448C

The protostellar jet driven by L1448C was observed in the SiO J=8-7 and CO J=3-2 lines and 350 GHz dust continuum at ~1" resolution with the Submillimeter Array (SMA). A narrow jet from the northern source L1448C(N) was observed in the SiO and the high-velocity CO. The jet consists of a chain of emission knots with an inter-knot spacing of ~2" (500 AU) and a semi-periodic velocity variation. The innermost pair of knots, which are significant in the SiO map but barely seen in the CO, are located at ~1" (250 AU) from the central source, L1448C(N). Since the dynamical time scale for the innermost pair is only ~10 yr, SiO may have been formed in the protostellar wind through the gas-phase reaction, or been formed on the dust grain and directly released into the gas phase by means of shocks. It is found that the jet is extremely active with a mechanical luminosity of ~7 L_sun, which is comparable to the bolometric luminosity of the central source (7.5 L_sun). The mass accretion rate onto the protostar derived from the mass-loss rate is ~10^{-5} M_sun/yr. Such a high mass accretion rate suggests that the mass and the age of the central star are 0.03-0.09 M_sun and (4-12)x10^3 yr, respectively, implying that the central star is in the very early stage of protostellar evolution. The low-velocity CO emission delineates two V-shaped shells with a common apex at L1448C(N). The kinematics of these shells are reproduced by the model of a wide opening angle wind. The co-existence of the highly-collimated jets and the wide-opening angle shells can be explained by the unified X-wind model" in which highly-collimated jet components correspond to the on-axis density enhancement of the wide-opening angle wind. The CO $J$=3--2 map also revealed the second outflow driven by the southern source L1448C(S) located at ~8.3" (2000 AU) from L1448C(N).Comment: 45 pages, 13 figures, Accepted for the publication in the Astrophysical Journa