Location Of Bump Research Articles

Effects of Interviewer Age on the Reminiscence Bump in Older adults’ Autobiographical Memories

ABSTRACT Introduction This study aims to investigate whether the reminiscence bump in older adults’ autobiographical memory is influenced by the interviewer’s age. Methods: I arranged four interviewer. Conditions child, university student, middle-aged adult, and older adult. The participating older adults were asked individually to describe three memories and the age at which the event occurred. I analyzed the temporal distribution of the bumps and the recall order. Results The results indicate that the interviewer’s age, especially the child interviewers were influenced the temporal location of the reminiscence bump. Conclusion: This study discusses the implications of these findings for older adults’ social communication processes.

Navigation and the efficiency of spatial coding: insights from closed-loop simulations

Spatial learning is critical for survival and its underlying neuronal mechanisms have been studied extensively. These studies have revealed a wealth of information about the neural representations of space, such as place cells and boundary cells. While many studies have focused on how these representations emerge in the brain, their functional role in driving spatial learning and navigation has received much less attention. We extended an existing computational modeling tool-chain to study the functional role of spatial representations using closed-loop simulations of spatial learning. At the heart of the model agent was a spiking neural network that formed a ring attractor. This network received inputs from place and boundary cells and the location of the activity bump in this network was the output. This output determined the movement directions of the agent. We found that the navigation performance depended on the parameters of the place cell input, such as their number, the place field sizes, and peak firing rate, as well as, unsurprisingly, the size of the goal zone. The dependence on the place cell parameters could be accounted for by just a single variable, the overlap index, but this dependence was nonmonotonic. By contrast, performance scaled monotonically with the Fisher information of the place cell population. Our results therefore demonstrate that efficiently encoding spatial information is critical for navigation performance.

Kinematical Signs of Dust Trapping and Feedback in a Local Pressure Bump in the Protoplanetary Disk around HD 142527 Revealed with ALMA

Abstract We analyzed the archival data of the continuum emission at six wavelengths from 3 to 0.4 mm and 13CO and C18O (1–0, 2–1, and 3–2) lines in the protoplanetary disk around HD 142527 obtained with the Atacama Large Millimeter/submillimeter Array. We performed fitting to the spectral energy distributions obtained at the six wavelengths with the graybody slab models to estimate the distributions of the dust surface density and spectral index of dust absorption coefficient β. We also estimated the distribution of the gas column density by fitting the C18O spectra and measured the disk rotation by fitting the Keplerian disk models to the C18O data. We found super- and sub-Keplerian rotation inside and outside the dust ring in the northwest in the HD 142527 disk, suggestive of the presence of a local pressure bump. In comparison with our estimated dust and gas distributions, the location of the pressure bump is coincident with the region showing a three times higher dust density and a three times lower gas-to-dust mass ratio than the mean values in the disk, suggesting dust trapping in the pressure bump. Nevertheless, there is no correlation between our derived β distribution and the location of the pressure bump. In addition, we found that the width of the dust ring is comparable to or larger than the width of the pressure bump, which could suggest that dust feedback is significant in the pressure bump.

Active and passive control of a galloping cylinder with heat transfer

Wind energy caused the transverse vibration of the beam, and the mechanical energy of vibration is transferred to electrical charge by piezoelectric transducer. In the current study, the active and passive control of energy release from a galloping bluff body is found. The system consists of a bluff body in front of wind which is mounted on a cantilever beam and supported by piezoelectric sheets. The nonlinear motion of the Euler–Bernoulli beam and conservation of electrical energy is modeled by lumped ordinary differential equations. The wind force on bluff body is modeled by moving mesh techniques in OpenFoam software where the fluid and solid corresponding dynamics are connected in timescales. The position of piezoelectric actuator and the location of bump are the two parameters considered for optimization analysis of galloping device. Genetic algorithms are used to find the optimal arrangements. Numerous models are offered for a clamped−clamped supported beam.

RETROSPECTIVE LIFE HISTORY SURVEY REVEALED AUTOBIOGRAPHICAL MEMORY BUMP

The reminiscence bump is a well-documented autobiographical memory phenomenon characterized by middle-aged and older adults reporting a disproportionate number of memories from adolescence and early adulthood (Rubin, Wetzler, & Nebes, 1986). It is typically assessed through either cue word or important memory techniques. The Life History Mail Survey (LHMS) in the Health and Retirement Study affords unique data to investigate this phenomenon among a representative US sample of older adults. At the beginning of the LHMS, participants (N=3088, M age=70, range 50-107) completed a calendar noting the important things that happened to them in seven life decades, starting with ages 0-9 and ending by ages 70-79 (or their actual age). For each life period, we coded the number of events respondents reported. We observed significantly more memories reported for the age decade 20-29, compared with other life periods (80% vs 47-66%). Our results are consistent with previous findings in the autobiographical memory literature. Follow-up analyses evaluated existing theoretical accounts of the bump, such as cultural life script theory which suggests that life events occur in a specific order and are characterized by a prototypical life course. For example, we determined whether respondents’ sociodemographic characteristics, such as age cohort, gender, marital and educational histories (information available in LHMS) influenced the size and temporal location of the reminiscence bump. We also analyzed the content of reported important life events to investigate whether types of events included in each decade of life are consistent with the cultural life script account of the phenomenon.

The Influence of the Metal Mass Fraction Z, Age, and Mixing-length Parameter on the RGB Bump Magnitude for the M4 Cluster

Abstract We identify the location of the RGB bump of M4 (NGC 6121) using the available photometric data, and measure V RGBB (∼13.57 ± 0.04 mag). According to the observed [Fe/H], we compute theoretical isochrones with the scaled-solar composition in the MESA model and alpha-enhanced composition in the BaSTI model, respectively. Using a color–magnitude diagram, we compare these isochrones with the observed data to obtain the magnitude difference δV bump between the predicted and the observed bump magnitude. Based on the best fit of the MESA model with [Fe/H] = −1.05, [α/Fe] = 0, α MLT = 2.0, and t = 13.3 Gyr, the bump magnitude difference δV bump is about 0.46 mag. Based on the best fit of the BaSTI model with α MLT = 2.2 ∼ 2.4, [Fe/H] = −1.05, [α/Fe] = 0.4, and t = 12.5 Gyr, the bump magnitude difference δV bump is about 0.2 mag. To try and explain the bump magnitude differences, the metal mass fraction Z is enhanced as 0.0037, 0.00591, 0.0076, and 0.0085. Accordingly, , , and by the MESA model are 0, −0.01, and 0 mag, respectively. Increasing the assumed metallicity can decrease the discrepancy between the predicted and observed bump magnitudes. However, a metallicity increase large enough to resolve the offset, roughly ∼0.60 dex for the MESA models, is ruled out by the spectroscopic data.

Understanding the reminiscence bump: A systematic review.

One of the most consistently observed phenomena in autobiographical memory research is the reminiscence bump: a tendency for middle-aged and elderly people to access more personal memories from approximately 10–30 years of age. This systematic review (PROSPERO 2017:CRD42017076695) aimed to synthesize peer-reviewed literature pertaining to the reminiscence bump. The researchers conducted searches in nine databases for studies published between the date of inception of each database and the year 2017. Keywords used included: reminiscence, bump, peak, surge, blip, reminiscence effect, and reminiscence component. Sixty-eight quantitative studies, out of 523, met the inclusion criteria. The researchers implemented a thematic analytic technique for data extraction. Four main themes were generated: methods of memory activation/instruction for life scripts, types of memory/life scripts recalled, location of the reminiscence bump, and theoretical accounts for the bump. The two prevailing methods of memory activation implemented were the cuing method and important memories method. Three types of memories/life scripts were recalled: personal/autobiographical memory, memories for public events, and life script events. The findings illustrate differing temporal periods for the bump: approximately 10–30 years for memories for important events, approximately 5–30 years for memories that were induced by word cues, and 6–39 years for studies using life scripts. In explaining the bump, the narrative/identity account and cultural life script account received the most support.

Recent Advances in Understanding the Reminiscence Bump

The reminiscence bump is the increased proportion of autobiographical memories from youth and early adulthood observed in adults over 40. It is one of the most robust findings in autobiographical-memory research. Although described as a single period from which there are more memories, a recent meta-analysis that reported the beginning and ending ages of the bump from individual studies found that different classes of cues produce distinct bumps that vary in size and temporal location. The bump obtained in response to cue words is both smaller and located earlier in the life span than the bump obtained when important memories are requested. The bump obtained in response to odor cues is even earlier. This variation in the size and temporal location of the reminiscence bump argues for theories based primarily on retrieval rather than encoding and retention, which most current theories stress. Furthermore, it points to the need to develop theories of autobiographical memory that account for this flexibility in the memories retrieved.

MULTIPLE STELLAR POPULATIONS OF GLOBULAR CLUSTERS FROM HOMOGENEOUS Ca by PHOTOMETRY. I. M22 (NGC 6656)

We investigate the multiple stellar populations in one of peculiar globular clusters (GCs) M22 using new ground-based wide-field Ca by and HST/WFC3 photometry with equivalent passbands, confirming our previous result that M22 has a distinctive red-giant branch (RGB) split mainly due to difference in metal abundances. We also make use of radial velocity measurements of the large number of cluster membership stars by other. Our main results are followings. (i) The RGB and the subgiant branch (SGB) number ratios show that the calcium-weak (Ca-w) group is the dominant population of the cluster. However, an irreconcilable difference can be seen in the rather simple two horizontal branch (HB) classification by other. (ii) Each group has its own CN-CH anti-correlation. However, the alleged CN-CH positive correlation is likely illusive. (iii) The location of the RGB bump of the calcium-strong (Ca-s) group is significantly fainter, which may pose a challenge to the helium enhancement scenario in the Ca-s group. (iv) The positions of the center are similar. (v) The Ca-w group is slightly more centrally concentrated, while the the Ca-s is more elongated at larger radii. (vi) The mean radial velocities for both groups are similar, but the Ca-s group has a larger velocity dispersion. (vii) The Ca-s group rotates faster. The plausible scenario for the formation of M22 is that it formed via a merger of two GCs in a dwarf galaxy environment and accreted later to our Galaxy.

New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies

We extend the {\sl\,PARSEC} library of stellar evolutionary tracks by computing new models of massive stars, from 14\Msun to 350\Msun. The input physics is the same used in the {\sl\,PARSEC}~V1.1 version, but for the mass-loss rate which is included by considering the most recent updates in literature. We focus on low metallicity, $Z$=0.001 and $Z$=0.004, for which the metal poor dwarf irregular star forming galaxies, Sextans A, WLM and NCG6822, provide simple but powerful workbenches. The models reproduce fairly well the observed CMDs but the stellar colour distributions indicate that the predicted blue loop is not hot enough in models with canonical extent of overshooting. In the framework of a mild extended mixing during central hydrogen burning, the only way to reconcile the discrepancy is to enhance the overshooting at the base of the convective envelope (EO) during the first dredge-UP. The mixing scales required to reproduce the observed loops, EO=2\HP or EO=4\HP, are definitely larger than those derived from, e.g., the observed location of the RGB bump in low mass stars. This effect, if confirmed, would imply a strong dependence of the mixing scale below the formal Schwarzschild border, on the stellar mass or luminosity. Reproducing the features of the observed CMDs with standard values of envelope overshooting would require a metallicity significantly lower than the values measured in these galaxies. Other quantities, such as the star formation rate and the initial mass function, are only slightly sensitive to this effect. Future investigations will consider other metallicities and different mixing schemes.

The Best Location for Speed Bump Installation Using Experimental Design Methodology

Speed bumps, as traffic calming devices, have been extensively used to reduce traffic speed on local streets. This study represents a unique application of experimental design methodology where the effects of some controllable factors in determining the best location for installing speed bumps before stop points (e.g. entry gates, road junctions) were investigated. Through Classical Design of Experiments (DOE), the optimum location of the speed bump was obtained based on the graphical plots of the significant effects. The speed at the stop point was treated as the response and minimum speed is desirable. Design-Expert® software was used to evaluate and analyze the results obtained. The suggested mathematical model effectively explains the performance indicators within the ranges of the factors. The car speed is the most significant factor that affects the distance-time in comparison with other factors, which provides secondary contributions.

Temporal distribution of autobiographical memory: Uncovering the reminiscence bump in Japanese young and middle-aged adults1

The reminiscence bump is the effect that people recall more personal events from their teenage period than from adjacent lifetime periods. The effect is generally found in studies that divide the results of participants, who were at least 40 years old, into age bins of 10 years. In this study, the temporal distribution of autobiographical memories of Japanese young and middle-aged adults was examined. Because the questionnaire was presented on the internet, many participants could take part (N = 252). By dividing the personal events into smaller age bins and applying a mathematical method that corrects for the increased recall of recent events, a reminiscence bump could be identified in the memories of young adults. The location of the reminiscence bump of young adults was similar to the location of the reminiscence bump of middle-aged adults.

DEEPHST/ACS PHOTOMETRY OF THE M81 HALO

We present a deep color–magnitude diagram (CMD) for individual stars in the halo of the nearby spiral galaxy M81, at a projected distance of 19 kpc, based on data taken with the Advanced Camera for Surveys on the Hubble Space Telescope (HST). The CMD reveals a red giant branch (RGB) that is narrow and fairly blue, and a horizontal branch that has stars that lie mostly redward of the RR Lyrae instability strip. We derive a mean metallicity of [M/H] = −1.15 ± 0.11 and age of 9 ± 2 Gyr for the dominant population in our field, from the shape of the RGB, the magnitude of the red clump, and the location of the RGB bump. We compare our metallicity and age results with those found previously for stars in different locations within M81 and in the spheroids of other nearby galaxies.

Wide-field multi-color photometry of the Galactic globular cluster NGC 1261

<i>Aims. <i/>This work studies in more detail the stellar population, including its photometric properties and characteristics, in the rarely studied southern Galactic globular cluster NGC 1261. We focus on the brighter sequences of the cluster's color–magnitude diagram (CMD). Like in our previous works, we rely upon photometry in several passbands to achieve more reliable results and conclusions.<i>Methods. <i/>We carried out and analyzed new multi-color photometry of NGC 1261 in <i>UBVI<i/> reaching below the turnoff point in all passbands in a fairly extended cluster field, about 14' × 14'.<i>Results. <i/>We found several signs of the inhomogeneity (“multiplicity”) in the stellar population. The most prominent of them are: (1) the dependence of the radial distribution of sub-giant branch (SGB) stars in the cluster on their <i>U<i/> magnitude, with brighter stars less centrally concentrated at the 99.9% level than their fainter counterparts; (2) the dependence of the location of red giant branch (RGB) stars in the <i>U<i/>-(<i>U<i/>-<i>B<i/>) CMD on their radial distance from the cluster center, with the portion of stars bluer in the (<i>U<i/>-<i>B<i/>) color increasing towards the cluster outskirts. Additionally, the radial variation of the RGB luminosity function in the bump region is suspected. We assume that both the SGB stars brighter in the <i>U<i/> and the RGB stars bluer in the (<i>U<i/>-<i>B<i/>) color are probably associated with blue horizontal branch stars, because of a similarity in their radial distribution in the cluster. We estimated the metalicity of NGC 1261 from the slope of the RGB in <i>U<i/>-based CMDs and the location of the RGB bump on the branch. These metallicity indicators give [Fe/H]<sub>ZW<sub/> = -1.34 <i>±<i/> 0.16 dex and [Fe/H]<sub>ZW<sub/> = -1.41 <i>±<i/> 0.10 dex, respectively. We isolated 18 probable blue straggler candidates. They are more centrally concentrated than the lower red giants of comparable brightness at the 97.9% level. Their photometric characteristics imply that their majority is not consistent with the collisional origin. We also reliably isolated the asymptotic giant branch (AGB) clump and estimated the parameter = 1.01 <i>±<i/> 0.06, that is the difference between the <i>V<i/>-levels of the zero age HB and the clump.

Multi-color photometry in wide field of the Galactic globular cluster NGC 3201

Aims. This paper aims at further studying one of the nearby Galactic globular clusters (GCs), NGC 3201. It is known to experience notable irregular variability of reddening across its face. By relying on our previous studies and findings and by developing them, we focus on the brighter sequences of the color-magnitude diagram (CMD) and on the cluster's characteristics. Methods. We carried out and analyzed new multi-color photometry of NGC 3201 in UBVI reaching below the turnoff point in all passbands in a fairly large cluster field, about $14\arcmin \times 14 \arcmin$. To achieve more reliable results and conclusions, we reduced the negative impact of the irregularly varying reddening and contamination by field stars. Results. With this aim we first estimated mean reddening in different zones of the studied cluster field and then took its variations into account, by reducing them to the same level. We estimated metallicity of NGC 3201 using a new metallicity indicator related to U -based CMDs, recently proposed by us. We find [Fe/H]$_{ZW} = -1.54 \pm 0.12$ dex, which falls between extreme estimates of the cluster's metallicity obtained using different methods or indicators. Also, the location of the RGB bump on the branch corresponds to [Fe/H]$_{ZW} = -1.46 \pm 0.15$ dex. We isolate 73 probable blue straggler (BS) candidates, the largest population found in NGC 3201 so far. They are more centrally concentrated than the lower red giants at the 99.2% level. Their position in the two-color diagram assumes that presumably none of them belongs to BSa of collisional origin. The luminosity function (LF) of the RGB and its features in the low part of the branch are examined and discussed. We also resolve some of the contradictory results of previous publications.

What is the best way to measure baryonic acoustic oscillations?

Oscillations in the baryon-photon fluid prior to recombination imprint different signatures on the power spectrum and correlation function of matter fluctuations. The measurement of these features using galaxy surveys has been proposed as means to determine the equation of state of the dark energy. The accuracy required to achieve competitive constraints demands an extremely good understanding of systematic effects which change the baryonic acoustic oscillation (BAO) imprint. We use 50 very large volume N-body simulations to investigate the BAO signature in the two-point correlation function. The location of the BAO bump does not correspond to the sound horizon scale at the level of accuracy required by future measurements, even before any dynamical or statistical effects are considered. Careful modelling of the correlation function is therefore required to extract the cosmological information encoded on large scales. We find that the correlation function is less affected by scale dependent effects than the power spectrum. We show that a model for the correlation function proposed by Crocce & Scoccimarro (2008), based on renormalised perturbation theory, gives an essentially unbiased measurement of the dark energy equation of state. This means that information from the large scale shape of the correlation function, in addition to the form of the BAO peak, can be used to provide robust constraints on cosmological parameters. The correlation function therefore provides a better constraint on the distance scale (~50% smaller errors with no systematic bias) than the more conservative approach required when using the power spectrum (i.e. which requires amplitude and long wavelength shape information to be discarded).

The interplay between ionized gas and massive stars in the HII galaxy IIZw70: integral field spectroscopy with PMAS

We performed an integral field spectroscopic study for the HII galaxy IIZw70 in order to investigate the interplay between its ionized interstellar medium (ISM) and the massive star formation (SF). Observations were taken in the optical spectral range (3700-6800 A) with the Potsdam Multi-Aperture Spectrophotometer (PMAS) attached to the 3.5 m telescope at CAHA. We created and analysed maps of spatially distributed emission-lines, continuum emission and properties of the ionized ISM (e.g. physical-chemical conditions, dust extinction, kinematics). We investigated the relation of these properties to the spatial distribution and evolutionary stage of the massive stars. For the first time we have detected the presence of Wolf-Rayet (WR) stars in this galaxy. The peak of the ionized gas emission coincides with the location of the WR bump. The region of the galaxy with lower dust extinction corresponds to the region that shows the lowest values of velocity dispersion and radial velocity. The overall picture suggests that the ISM of this region is being disrupted via photoionization and stellar winds, leading to a spatial decoupling between gas+stars and dust clouds. The bulk of dust appears to be located at the boundaries of the region occupied by the probable ionizing cluster. We also found that this region is associated to the nebular emission in HeII4686 and to the intensity maximum of most emission lines. This indicates that the hard ionizing radiation responsible for the HeII4686 nebular emission can be related to the youngest stars. Within $\sim$ 0.4 x 0.3 kpc^2 in the central burst, we derived O/H using direct determinations of Te[OIII]. We found abundances in the range 12+log(O/H)=7.65-8.05, yielding an error-weighted mean of 12+log(O/H)=7.86 $\pm$0.05.

Influence of the Ion Mobility on the Exact Location of the Regime Bump in NLCDs

In this article, we propose an improvement of the ion transport model in NLCDs, taking into consideration the possible dependence of the ion mobility on the ion density. The presence of ion channels in the LC bulk, initiated by a Carr-Helfrich-like mechanism, would lead to a higher mobility at the start of the regime pulse. A better explanation of the exact location of the current bump during the regime pulse can then be reached.

Disruption of vma-1, the Gene Encoding the Catalytic Subunit of the Vacuolar H+-ATPase, Causes Severe Morphological Changes in Neurospora crassa

By using the process of Repeat-induced Point mutation (Selker, E. U., and Garrett, P. W. (1988) Proc. Natl. Acad. Sci. U. S. A. 85, 6870-6874), we inactivated vma-1, the gene encoding subunit A of the V-ATPase of Neurospora crassa. Two vma-1 mutant strains were characterized. One was mutated at multiple sites, did not make a protein product, and produced spores that only rarely germinated. The other had four point mutations, made a protein product, and produced viable spores. Neither strain had detectable V-ATPase activity. The vma-1 mutant strains did not grow in medium buffered to pH 7.0 or above or in medium supplemented with the cation Zn(2+). They were completely resistant to inhibition by concanamycin C, supporting our hypothesis that the V-ATPase is the in vivo target of this antibiotic. Inactivation of the vma-1 gene had a pronounced effect on morphology and development of the organism. In the mutants tip growth was inhibited, and multiple branching was induced. The vma-1 mutant strains could not differentiate conidia or perithecia. They could grow slowly as mycelia and could donate nuclei in a sexual cross. A mutation in the plasma membrane ATPase, which suppressed the sensitivity of wild type N. crassa to concanamycin, also proved effective in suppressing the sensitivity of a vma-1 null mutant to basic pH but did not correct the morphological defects.