Tracking Patterns of Needs During a Telephone Follow-up Program for Family Caregivers of Persons with Stroke

Purpose Programs that address stroke family caregiver needs and skill-building are recommended based on the literature and patient care guidelines for stroke rehabilitation. The purpose of this study was to explore patterns of perceived needs and skill-building during a stroke caregiver intervention program. Method Descriptive statistics were used to analyze data from 123 stroke caregivers enrolled in the intervention group of a randomized controlled clinical trial. Caregivers received 8 weekly telephone sessions, with a booster session a month later. At each session, the Caregiver Needs and Concerns Checklist (CNCC) was used to identify and prioritize current needs that were then addressed through skill-building strategies. Results Perceived needs changed over time. Information about stroke was the highest priority need during Session 1. Managing survivor emotions and behaviors was the highest priority for Sessions 2 through 4. Caregivers generally waited until Sessions 5 through 9 to address their own emotional and physical health needs. Physical and instrumental care needs were relatively low but stable across all 9 sessions. Skill-building was consistently high, though it peaked during Sessions 2 and 3. Conclusions Tracking patterns of needs and skill-building suggest appropriate timing for targeting different types of family caregiver support during stroke rehabilitation

Very Low-mass Stellar and Substellar Companions to Solar-like Stars from MARVELS II: A Short-period Companion Orbiting an F Star with Evidence of a Stellar Tertiary And Significant Mutual Inclination

We report the discovery via radial velocity of a short-period (P = 2.430420 \pm 0.000006 days) companion to the F-type main sequence star TYC 2930-00872-1. A long-term trend in the radial velocities indicates the presence of a tertiary stellar companion with $P > 2000$ days. High-resolution spectroscopy of the host star yields T_eff = 6427 +/- 33 K, log(g) = 4.52 +/- 0.14, and [Fe/H]=-0.04 +/- 0.05. These parameters, combined with the broad-band spectral energy distribution and parallax, allow us to infer a mass and radius of the host star of M_1=1.21 +/- 0.08 M_\odot and R_1=1.09_{-0.13}^{+0.15} R_\odot. We are able to exclude transits of the inner companion with high confidence. The host star's spectrum exhibits clear Ca H and K core emission indicating stellar activity, but a lack of photometric variability and small v*sin(I) suggest the primary's spin axis is oriented in a pole-on configuration. The rotational period of the primary from an activity-rotation relation matches the orbital period of the inner companion to within 1.5 \sigma, suggesting they are tidally locked. If the inner companion's orbital angular momentum vector is aligned with the stellar spin axis, as expected through tidal evolution, then it has a stellar mass of M_2 ~ 0.3-0.4 M_\odot. Direct imaging limits the existence of stellar companions to projected separations < 30 AU. No set of spectral lines and no significant flux contribution to the spectral energy distribution from either companion are detected, which places individual upper mass limits of M < 1.0 M_\odot, provided they are not stellar remnants. If the tertiary is not a stellar remnant, then it likely has a mass of ~0.5-0.6 M_\odot, and its orbit is likely significantly inclined from that of the secondary, suggesting that the Kozai-Lidov mechanism may have driven the dynamical evolution of this system.Comment: 37 pages, 7 tables, 21 figures, Accepted in A

Very low mass stellar and substellar companions to solar-like stars from MARVELS. II. A short-period companios orbiting an F star with evidence of a stellar tertiary and significant mutual inclination

We report the discovery via radial velocity (RV) measurements of a short-period (P = 2.430420±0.000006 days) companion to the F-type main-sequence star TYC 2930-00872-1. A long-term trend in the RV data also suggests the presence of a tertiary stellar companion with P > 2000 days. High-resolution spectroscopy of the host star yields Teff = 6427 ± 33 K, log g = 4.52 ± 0.14, and [Fe/H] = −0.04 ± 0.05. These parameters, combined with the broadband spectral energy distribution (SED) and a parallax, allow us to infer a mass and radius of the host star of M1 = 1.21 ± 0.08 M and R1 = 1.09+0.15 −0.13 R . The minimum mass of the inner companion is below the hydrogen-burning limit; however, the true mass is likely to be substantially higher. We are able to exclude transits of the inner companion with high confidence. Further, the host star spectrum exhibits a clear signature of Ca H and K core emission, indicating stellar activity, but a lack of photometric variability and small v sin I suggest that the primary’s spin axis is oriented in a pole-on configuration. The rotational period of the primary estimated through an activity–rotation relation matches the orbital period of the inner companion to within 1.5 σ, suggesting that the primary and inner companion are tidally locked. If the inner companion’s orbital angular momentum vector is aligned with the stellar spin axis as expected through tidal evolution, then it has a stellar mass of ∼0.3–0.4 M . Direct imaging limits the existence of stellar companions to projected separations <30 AU. No set of spectral lines and no significant flux contribution to the SED from either companion are detected, which places individual upper mass limits of M{2,3} 1.0 M , provided they are not stellar remnants. If the tertiary is not a stellar remnant, then it likely has a mass of ∼0.5–0.6M , and its orbit is likely significantly inclined from that of the secondary, suggesting that the Kozai–Lidov mechanism may have driven the dynamical evolution of this system

Morality and Work–Family Conflict in the Lives of Poor and Low-Income Women

Contemporary understandings of work and family are largely based on middle-class women\u27s experience, whereas poverty and welfare researchers focus on the economic struggles of single female-headed families. This qualitative study examines the cultural and moral forces underlying the tension between paid work and family responsibilities through the experience of poor and low-income women. Interview data reveal that as expected, the conditions of poverty and welfare shape work and family decisions. Yet, choices about work and family entail moral and emotional commitments defined through powerful gendered cultural schemas. Providing financially for children reflects a strong work ethic and moral worth corresponding to a masculine model of individual responsibility privileging self-sufficiency and independence. This is challenged by a shared moral imperative that mother\u27s primary responsibility is the care of children. This examination is important for researchers in understanding the moral and emotional salience of gender in shaping the work and family lives of poor and low-income women

Very low mass stellar and substellar companions to solar-like stars from MARVELS. II. A short-period companios orbiting an F star with evidence of a stellar tertiary and significant mutual inclination

We report the discovery via radial velocity (RV) measurements of a short-period (P = 2.430420±0.000006 days) companion to the F-type main-sequence star TYC 2930-00872-1. A long-term trend in the RV data also suggests the presence of a tertiary stellar companion with P > 2000 days. High-resolution spectroscopy of the host star yields Teff = 6427 ± 33 K, log g = 4.52 ± 0.14, and [Fe/H] = −0.04 ± 0.05. These parameters, combined with the broadband spectral energy distribution (SED) and a parallax, allow us to infer a mass and radius of the host star of M1 = 1.21 ± 0.08 M and R1 = 1.09+0.15 −0.13 R . The minimum mass of the inner companion is below the hydrogen-burning limit; however, the true mass is likely to be substantially higher. We are able to exclude transits of the inner companion with high confidence. Further, the host star spectrum exhibits a clear signature of Ca H and K core emission, indicating stellar activity, but a lack of photometric variability and small v sin I suggest that the primary’s spin axis is oriented in a pole-on configuration. The rotational period of the primary estimated through an activity–rotation relation matches the orbital period of the inner companion to within 1.5 σ, suggesting that the primary and inner companion are tidally locked. If the inner companion’s orbital angular momentum vector is aligned with the stellar spin axis as expected through tidal evolution, then it has a stellar mass of ∼0.3–0.4 M . Direct imaging limits the existence of stellar companions to projected separations <30 AU. No set of spectral lines and no significant flux contribution to the SED from either companion are detected, which places individual upper mass limits of M{2,3} 1.0 M , provided they are not stellar remnants. If the tertiary is not a stellar remnant, then it likely has a mass of ∼0.5–0.6M , and its orbit is likely significantly inclined from that of the secondary, suggesting that the Kozai–Lidov mechanism may have driven the dynamical evolution of this system